Editing Ganymede (moon)

{{Short description|Largest moon of Jupiter and in the Solar System}}
{{distinguish|Ganymed (asteroid)}}
{{Featured article}}
{{Use mdy dates|date=August 2024}}
{{Infobox planet
| name = Ganymede
| alt_names = Jupiter {{rn|III}}
| pronounced = {{IPAc-en|ˈ|ɡ|æ|n|ᵻ|m|iː|d}}<br />{{respell|GAN|im|eed}}<ref>{{cite OED|Ganymede}}<br />{{cite Merriam-Webster|Ganymede}}</ref>
| adjectives = Ganymedian,<ref>Quinn Passey & E. M. Shoemaker (1982) "Craters on Ganymede and Callisto", in David Morrison, ed., ''Satellites of Jupiter'', vol. 3, International Astronomical Union, pp. 385–386, 411.</ref><br />Ganymedean<ref>''Journal of Geophysical Research'', v. 95 (1990).</ref><ref>E. M. Shoemaker et al. (1982) "Geology of Ganymede", in David Morrison, ed., ''Satellites of Jupiter'', vol. 3, International Astronomical Union, pp. 464, 482, 496.</ref> ({{IPAc-en|ˌ|ɡ|æ|n|ə|ˈ|m|iː|d|i|.|ən}})
| named_after = {{lang|grc|[[Ganymede (mythology)|Γανυμήδης]]}}, {{transliteration|grc|Ganymēdēs}}
| image = Ganymede - Perijove 34 Composite.png
| image_alt = Surface with swatches of light and dark brown. The bright crater on the lower left is the Tros crater.
| caption = Ganymede in true color as imaged by the ''[[Juno (spacecraft)|Juno]]'' spacecraft June 2021<ref>{{cite web | url=https://www.missionjuno.swri.edu/junocam/processing?id=10742 | title='Tros Crater, Ganymede – PJ34-1 Detail' &#124; }}</ref>
| background = Wheat
| discovery_ref = <ref name="SidereusNuncius">{{cite web|last=Galilei |first=Galileo |url=http://hsci.cas.ou.edu/images/barker/5990/Sidereus-Nuncius-whole.pdf |date=March 1610 |title=Sidereus Nuncius |author2=translated by Edward Carlos |editor-first=Peter |editor-last=Barker |publisher=University of Oklahoma History of Science |access-date=January 13, 2010 |url-status=dead |archive-url=https://web.archive.org/web/20051220010647/http://hsci.cas.ou.edu/images/barker/5990/Sidereus-Nuncius-whole.pdf |archive-date=December 20, 2005 }}</ref><ref name="NASA">{{cite web |url=https://solarsystem.nasa.gov/moons/jupiter-moons/ganymede/in-depth/ |title=In Depth {{!}} Ganymede |website=NASA Solar System Exploration |access-date=June 16, 2021 |archive-date=July 28, 2018 |archive-url=https://web.archive.org/web/20180728113750/https://solarsystem.nasa.gov/moons/jupiter-moons/ganymede/in-depth/ |url-status=live }}</ref>
| discoverer = [[Galileo Galilei]]<br />[[Simon Marius]]
| discovered = January 7, 1610
| semimajor = {{val|1070400|u=km}}<ref name="orbit">{{cite web |title=Planetary Satellite Mean Orbital Parameters |publisher=Jet Propulsion Laboratory, California Institute of Technology |url=http://ssd.jpl.nasa.gov/?sat_elem |access-date=February 9, 2008 |archive-date=November 3, 2013 |archive-url=https://web.archive.org/web/20131103134221/http://ssd.jpl.nasa.gov/?sat_elem |url-status=live }}</ref>
| eccentricity = {{val|0.0013}}<ref name="orbit" />
| periapsis = {{val|1069200|u=km}}<ref name="periapsiscomment" group=lower-alpha />
| apoapsis = {{val|1071600|u=km}}<ref name="apoapsiscomment" group=lower-alpha />
| period = {{val|7.15455296|ul=d}}<ref name="orbit" />
| avg_speed = {{val|10.880|u=km/s}}
| inclination = 2.214° (to the [[ecliptic]])<br />0.20° (to Jupiter's equator)<ref name="orbit" />
| satellite_of = [[Jupiter]]
| group = [[Galilean moon]]
| mean_radius = {{val|2634.1|0.3|u=km}} (0.413 Earths)<ref name="Showman1999">{{cite journal |last1=Showman |first1=Adam P. |last2=Malhotra |first2=Renu |title=The Galilean Satellites |date=October 1, 1999 |journal=Science |volume=286 |pages=77–84 |doi=10.1126/science.286.5437.77 |url=http://www.lpl.arizona.edu/~showman/publications/showman-malhotra-1999.pdf |pmid=10506564 |issue=5437 |access-date=January 17, 2008 |archive-date=May 14, 2011 |archive-url=https://web.archive.org/web/20110514231040/http://www.lpl.arizona.edu/~showman/publications/showman-malhotra-1999.pdf |url-status=live }}</ref>
| surface_area = {{val|8.72|e=7|u=km2}} (0.171 Earths)<ref name="surfaceareacomment" group=lower-alpha />
| volume = {{val|7.66|e=10|u=km3}} (0.0704 Earths)<ref name="volumecomment" group=lower-alpha />
| mass = {{val|1.4819|e=23|u=kg}} 
(0.025 Earths)<ref name="Showman1999" />
| density = {{val|1.936|ul=g/cm3}} (0.351 Earths)<ref name="Showman1999" />
| surface_grav = {{val|1.428|ul=m/s2}} (0.146 ''[[g-force|g]]'')<ref name="surfacegravitycomment" group=lower-alpha />
| moment_of_inertia_factor = {{val|0.3115|0.0028}}<ref name="Schubert2004">{{cite book |last1=Schubert |first1=G. |last2=Anderson |first2=J. D. |last3=Spohn |first3=T. |last4=McKinnon |first4=W. B. |editor1-last=Bagenal |editor1-first=F. |editor2-last=Dowling |editor2-first=T. E. |editor3-last=McKinnon |editor3-first=W. B. |title=Jupiter: the planet, satellites, and magnetosphere |chapter=Interior composition, structure and dynamics of the Galilean satellites |date=2004 |publisher=Cambridge University Press |location=New York |url=https://books.google.com/books?id=aMERHqj9ivcC |chapter-url=https://books.google.com/books?id=aMERHqj9ivcC&pg=PA281 |isbn=978-0521035453 |pages=281–306 |oclc=54081598 |access-date=July 23, 2019 |archive-date=April 16, 2023 |archive-url=https://web.archive.org/web/20230416151559/https://books.google.com/books?id=aMERHqj9ivcC |url-status=live }}</ref>
| escape_velocity = {{val|2.741|u=km/s}}<ref name="escapevelocitycomment" group=lower-alpha />
| rotation = [[synchronous rotation|synchronous]]
| axial_tilt = 0–0.33°<ref name="Bills2005">{{cite journal |last=Bills |first=Bruce G. |title=Free and forced obliquities of the Galilean satellites of Jupiter |date=2005 |volume=175 |issue=1 |pages=233–247 |doi=10.1016/j.icarus.2004.10.028 |bibcode=2005Icar..175..233B |journal=Icarus |url=https://zenodo.org/record/1259023 |access-date=July 13, 2019 |archive-date=July 27, 2020 |archive-url=https://web.archive.org/web/20200727063125/https://zenodo.org/record/1259023 |url-status=live }}</ref> (to Jupiter's equator)
| right_asc_north_pole = 268.20°<ref name="iau2015">{{Cite journal |last1=Archinal |first1=B. A. |last2=Acton |first2=C. H. |last3=A'Hearn |first3=M. F. |last4=Conrad |first4=A. |last5=Consolmagno |first5=G. J. |last6=Duxbury |first6=T. |last7=Hestroffer |first7=D. |last8=Hilton |first8=J. L. |last9=Kirk |first9=R. L. |last10=Klioner |first10=S. A. |last11=McCarthy |first11=D. |last12=Meech |first12=K. |last13=Oberst |first13=J. |last14=Ping |first14=J. |last15=Seidelmann |first15=P. K. |date=2018 |title=Report of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2015 |url=http://link.springer.com/10.1007/s10569-017-9805-5 |journal=Celestial Mechanics and Dynamical Astronomy |language=en |volume=130 |issue=3 |page=22 |doi=10.1007/s10569-017-9805-5 |bibcode=2018CeMDA.130...22A |issn=0923-2958}}</ref>
| declination = 64.57°<ref name="iau2015" />
| angular_size = {{nowrap |1.2 to 1.8 [[minute and second of arc|arcseconds]]}}
| albedo = {{val|0.43|0.02}}<ref name="jplfact">{{cite web |last=Yeomans |first=Donald K. |date=July 13, 2006 |title=Planetary Satellite Physical Parameters |publisher=JPL Solar System Dynamics |url=http://ssd.jpl.nasa.gov/?sat_phys_par |access-date=November 5, 2007 |archive-date=November 1, 2013 |archive-url=https://web.archive.org/web/20131101144111/http://ssd.jpl.nasa.gov/?sat_phys_par |url-status=live }}</ref>
| magnitude = 4.61 ([[opposition (astronomy)|opposition]])<ref name="jplfact" /><br />4.38 (in 1951)<ref name="horizons">{{cite web |title=Horizon Online Ephemeris System for Ganymede (Major Body 503) |publisher=California Institute of Technology, Jet Propulsion Laboratory |last1=Yeomans |last2=Chamberlin |url=http://ssd.jpl.nasa.gov/horizons.cgi?find_body=1&body_group=mb&sstr=503 |access-date=April 14, 2010 |archive-date=February 2, 2014 |archive-url=https://web.archive.org/web/20140202122141/http://ssd.jpl.nasa.gov/horizons.cgi?find_body=1&body_group=mb&sstr=503 |url-status=live }} (4.38 on 1951-Oct-03).</ref>
| temp_name1 = K
| max_temp_1 = 152<ref name="Orton1996">{{cite journal |last1=Orton |first1=G. S. |last2=Spencer |first2=G. R. |last3=Travis |first3=L. D. |last4=Martin |first4=T. Z. |last5=Tamppari |first5=L. K. |display-authors=2 |title=Galileo Photopolarimeter-radiometer observations of Jupiter and the Galilean Satellites |journal=Science |date=1996 |volume=274 |issue=5286 |pages=389–391 |bibcode=1996Sci...274..389O |doi=10.1126/science.274.5286.389 |s2cid=128624870 }}</ref>
| mean_temp_1 = 110<ref name="Delitsky1998">{{cite journal|last1=Delitsky |first1=Mona L. |last2=Lane |first2=Arthur L. |title=Ice chemistry of Galilean satellites |journal=J. Geophys. Res. |date=1998 |volume=103 |issue=E13 |pages=31,391–31,403 |doi=10.1029/1998JE900020 |url=https://trs.jpl.nasa.gov/bitstream/handle/2014/20675/98-1725.pdf |bibcode=1998JGR...10331391D |archive-url=https://web.archive.org/web/20061003013845/http://trs-new.jpl.nasa.gov/dspace/bitstream/2014/20675/1/98-1725.pdf |archive-date=October 3, 2006 |doi-access=free }}</ref>
| min_temp_1 = 70<ref name="Delitsky1998" />
| atmosphere = yes
| surface_pressure = {{convert|0.2-1.2|μPa|atm|sigfig=3|abbr=on}}<ref name="Hall1998">{{cite journal |last1=Hall |first1=D. T. |last2=Feldman |first2=P. D. |last3=McGrath |first3=M. A. |last4=Strobel |first4=D. F. |display-authors=2 |title=The Far-Ultraviolet Oxygen Airglow of Europa and Ganymede |journal=The Astrophysical Journal |date=1998 |volume=499 |issue=1 |pages=475–481 |doi=10.1086/305604 |bibcode=1998ApJ...499..475H |doi-access=free }}</ref>
| atmosphere_composition = mostly [[oxygen]]<ref name="Hall1998" />
| temp_name2 = °C
| min_temp_2 = −203
| max_temp_2 = −121
| mean_temp_2 = −163
}}

'''Ganymede''', or '''Jupiter III''', is the [[List of Solar System objects by size|largest and most massive]] [[natural satellite]] of [[Jupiter]], and in the [[Solar System]]. Despite being the only moon in the Solar System with a substantial [[magnetic field]], it is the largest Solar System object without a substantial atmosphere. Like [[Saturn]]'s largest moon [[Titan (moon)|Titan]], it is larger than the planet [[Mercury (planet)|Mercury]], but has somewhat less [[surface gravity]] than Mercury, [[Io (moon)|Io]], or the [[Moon]] due to its lower density compared to the three.<ref name="nasa.gany">{{cite web |publisher=www2.jpl.nasa.gov |title=Ganymede Fact Sheet |url=http://www2.jpl.nasa.gov/galileo/ganymede/ |archive-url=https://web.archive.org/web/19970105182318/http://www.jpl.nasa.gov/galileo/ganymede/ |url-status=dead |archive-date=January 5, 1997 |access-date=January 14, 2010 }}</ref> Ganymede [[orbit]]s Jupiter in roughly seven days and is in a 1:2:4 [[orbital resonance]] with the moons [[Europa (moon)|Europa]] and [[Io (moon)|Io]], respectively.

Ganymede is composed of [[silicate|silicate rock]] and [[water substance|water]] in approximately equal proportions. It is a fully [[Planetary differentiation|differentiated]] body with an iron-rich, [[Planetary core|liquid metallic core]], giving it the lowest [[moment of inertia factor]] of any solid body in the Solar System. Its [[Planetary oceanography|internal ocean]] potentially contains more water than all of Earth's oceans combined.<ref name="Ocean Hubble">{{cite news |last=Staff |url=http://www.nasa.gov/press/2015/march/nasa-s-hubble-observations-suggest-underground-ocean-on-jupiters-largest-moon/#.VQJhMM26t0s |title=NASA's Hubble Observations Suggest Underground Ocean on Jupiter's Largest Moon |work=NASA News |date=March 12, 2015 |access-date=March 15, 2015 |archive-date=November 5, 2019 |archive-url=https://web.archive.org/web/20191105035942/https://www.nasa.gov/press/2015/march/nasa-s-hubble-observations-suggest-underground-ocean-on-jupiters-largest-moon/#.VQJhMM26t0s |url-status=live }}</ref><ref name="clubsandwich 2014">{{cite news |last=Clavin |first=Whitney |url=http://www.jpl.nasa.gov/news/news.php?release=2014-138 |title=Ganymede May Harbor 'Club Sandwich' of Oceans and Ice |work=NASA |publisher=Jet Propulsion Laboratory |date=May 1, 2014 |access-date=May 1, 2014 |archive-date=January 31, 2020 |archive-url=https://web.archive.org/web/20200131231329/https://www.jpl.nasa.gov/news/news.php?release=2014-138 |url-status=live }}</ref><ref name="Vance">{{cite journal |title=Ganymede's internal structure including thermodynamics of magnesium sulfate oceans in contact with ice |journal=Planetary and Space Science |date=April 12, 2014 |last1=Vance |first1=Steve |last2=Bouffard |first2=Mathieu |last3=Choukroun |first3=Mathieu |last4=Sotina |first4=Christophe |doi=10.1016/j.pss.2014.03.011 |bibcode = 2014P&SS...96...62V |volume=96 |pages=62–70}}</ref><ref name="NASA-20140501c">{{cite web |author=Staff |title=Video (00:51) – Jupiter's 'Club Sandwich' Moon |url=https://www.youtube.com/watch?v=oBbWjlkuw5U | archive-url=https://ghostarchive.org/varchive/youtube/20211114/oBbWjlkuw5U| archive-date=November 14, 2021 | url-status=live|date=May 1, 2014 |work=[[NASA]] |access-date=May 2, 2014 }}{{cbignore}}</ref> 

Ganymede's [[magnetic field]] is probably created by [[convection]] within its core, and influenced by tidal forces from Jupiter's far greater magnetic field.<ref name="Kivelson2002">{{cite journal |last1=Kivelson |first1=M.G. |last2=Khurana |first2=K.K. |last3=Coroniti |first3=F.V. |display-authors=2 |title=The Permanent and Inductive Magnetic Moments of Ganymede |journal=Icarus |date=2002 |volume=157 |issue=2 |pages=507–522 |doi=10.1006/icar.2002.6834 |url=http://www.igpp.ucla.edu/people/mkivelson/Publications/ICRUS1572507.pdf |bibcode=2002Icar..157..507K |hdl=2060/20020044825 |s2cid=7482644 |hdl-access=free |access-date=January 15, 2008 |archive-date=March 27, 2009 |archive-url=https://web.archive.org/web/20090327050816/http://www.igpp.ucla.edu/people/mkivelson/Publications/ICRUS1572507.pdf |url-status=live }}</ref> Ganymede has a thin [[oxygen]] [[atmosphere]] that includes O, O<sub>2</sub>, and possibly O<sub>3</sub> ([[ozone]]).<ref name="Hall1998" /> [[Atomic hydrogen]] is a minor atmospheric constituent. Whether Ganymede has an [[ionosphere]] associated with its atmosphere is unresolved.<ref name="Eviatar2001">{{cite journal |last1=Eviatar |first1=Aharon |last2=Vasyliunas |first2=Vytenis M. |last3=Gurnett |first3=Donald A. |display-authors=2 |title=The ionosphere of Ganymede |journal=Planet. Space Sci. |date=2001 |volume=49 |issue=3–4 |pages=327–336 |doi=10.1016/S0032-0633(00)00154-9 |url=http://www.tau.ac.il/~arkee/ganymop.ps |format=ps |bibcode=2001P&SS...49..327E |access-date=January 16, 2008 |archive-date=May 14, 2011 |archive-url=https://web.archive.org/web/20110514044301/http://www.tau.ac.il/~arkee/ganymop.ps |url-status=live }}</ref>

Ganymede's surface is composed of two main types of terrain, the first of which are lighter regions, generally crosscut by extensive grooves and ridges, dating from slightly less than 4 billion years ago, covering two-thirds of Ganymede. The cause of the light terrain's disrupted geology is not fully known, but may be the result of [[tectonics|tectonic]] activity due to [[tidal heating]].  The second terrain type are darker regions saturated with [[impact crater]]s, which are dated to four billion years ago.<ref name="Showman1999" />

Ganymede's discovery is credited to [[Simon Marius]] and [[Galileo Galilei]], who both observed it in 1610,<ref name="SidereusNuncius" />{{efn|name=Marius|It is probable that the German astronomer [[Simon Marius]] discovered it independently the same year.<ref>{{cite encyclopedia |url=https://www.britannica.com/place/Ganymede-satellite-of-Jupiter |title=Ganymede (satellite of Jupiter) |encyclopedia=[[Encyclopædia Britannica]] |access-date=November 19, 2019 |archive-date=June 18, 2019 |archive-url=https://web.archive.org/web/20190618122936/https://www.britannica.com/place/Ganymede-satellite-of-Jupiter |url-status=live }}</ref>}} as the third of the [[Galilean moon]]s, the first group of objects discovered orbiting another planet.<ref name="Planetary Society">{{cite web |url=http://www.planetary.org/explore/topics/our_solar_system/jupiter/moons.html |title=Jupiter's Moons |work=The Planetary Society |url-status=dead |archive-url=https://web.archive.org/web/20071231082201/http://www.planetary.org/explore/topics/our_solar_system/jupiter/moons.html |archive-date=December 31, 2007 }}</ref> Its name was soon suggested by astronomer Simon Marius, after the [[Greek mythology|mythological]] [[Ganymede (mythology)|Ganymede]], a [[Troy|Trojan]] prince desired by [[Zeus]] (the Greek counterpart of [[Jupiter (mythology)|Jupiter]]), who carried him off to be the cupbearer of the gods.<ref name="Naming">{{cite web |url=http://galileo.rice.edu/sci/observations/jupiter_satellites.html |title=Satellites of Jupiter |work=The Galileo Project |access-date=November 24, 2007 |archive-date=November 1, 2019 |archive-url=https://web.archive.org/web/20191101192948/http://galileo.rice.edu/sci/observations/jupiter_satellites.html |url-status=live }}</ref>

Beginning with ''[[Pioneer 10]]'', several spacecraft have explored Ganymede.<ref name="Pioneer 11" /> The [[Voyager program|Voyager]] probes, ''[[Voyager 1]]'' and ''[[Voyager 2]]'', refined measurements of its size, while ''[[Galileo (spacecraft)|Galileo]]'' discovered its underground ocean and magnetic field. The next planned mission to the [[Moons of Jupiter|Jovian system]] is the [[European Space Agency]]'s [[Jupiter Icy Moons Explorer]] (JUICE), which was launched in 2023.<ref name="esa-juice">{{cite web |url=https://sci.esa.int/web/juice |title=ESA Science & Technology – JUICE |publisher=[[ESA]] |date=November 8, 2021 |access-date=November 10, 2021 |archive-date=September 21, 2019 |archive-url=https://web.archive.org/web/20190921101151/https://sci.esa.int/web/juice |url-status=live }}</ref> After flybys of all three icy Galilean moons, it is planned to enter orbit around Ganymede.<ref name="selection">{{cite news |url=https://www.bbc.co.uk/news/science-environment-17917102 |title=Esa selects 1bn-euro Juice probe to Jupiter |first=Jonathan |last=Amos |date=May 2, 2012 |work=[[BBC News]] |access-date=May 2, 2012 |archive-date=May 11, 2020 |archive-url=https://web.archive.org/web/20200511181342/https://www.bbc.co.uk/news/science-environment-17917102 |url-status=live }}</ref>

[[File:Ganymede, Earth & Moon size comparison.jpg|thumb|250x250px|Size comparison of Earth, the [[Moon]] (top left), and Ganymede (bottom left)]]

==History==
Chinese astronomical records report that in 365 BC, [[Gan De]] detected what might have been a moon of Jupiter, probably Ganymede, with the naked eye.<ref name="ads.793b">{{cite journal |bibcode=1981BAAS...13..793B |title=Ancient Astronomy in Modern China |journal=Bulletin of the Astronomical Society |volume=13 |page=793 |last=Brecher |first=K. |date=1981 }}</ref> However, Gan De reported the color of the companion as reddish, which is puzzling since moons are too faint for their color to be perceived with the naked eye.<ref name=encyc>{{cite encyclopedia
 | first=Huang | last=Yi-Long | editor=Helaine Selin |editor-link=Helaine Selin | title=Gan De | encyclopedia=Encyclopaedia of the history of science, technology, and medicine in non-western cultures
 | page=342 | publisher=Springer | date=1997 | url=https://books.google.com/books?id=GzjpCAAAQBAJ&pg=PA342 | isbn=978-0-7923-4066-9 }}</ref> [[Shi Shen]] and Gan De together made fairly accurate observations of the five major planets.<ref name="Deng2011">{{cite book|author=Yinke Deng|title=Ancient Chinese Inventions|url=https://books.google.com/books?id=EeVPT6UAk3EC&pg=PA68|date=March 3, 2011|publisher=Cambridge University Press|isbn=978-0-521-18692-6|page= 68}}</ref><ref>{{cite journal | last = Xi | first = Ze-zong | title = The Discovery of Jupiter's Satellite Made by Gan De 2000 Years Before Galileo | journal = [[Acta Astrophysica Sinica]] | volume = 1 | issue = 2 | pages = 87 | date = 1981 | bibcode = 1981AcApS...1...85X | url = http://en.cnki.com.cn/Article_en/CJFDTOTAL-TTWL198102000.htm | access-date = March 22, 2017 | archive-date = November 4, 2020 | archive-url = https://web.archive.org/web/20201104160900/http://en.cnki.com.cn/Article_en/CJFDTOTAL-TTWL198102000.htm | url-status = dead }}</ref>

On January 7, 1610, [[Galileo Galilei]] used a telescope to observe what he thought were three [[star]]s near Jupiter, including what turned out to be Ganymede, [[Callisto (moon)|Callisto]], and one body that turned out to be the combined light from [[Io (moon)|Io]] and [[Europa (moon)|Europa]]; the next night he noticed that they had moved. On January 13, he saw all four at once for the first time, but had seen each of the moons before this date at least once. By January 15, Galileo concluded that the stars were actually bodies orbiting [[Jupiter]].<ref name="SidereusNuncius" /><ref name="NASA" />{{efn|name=Marius}}

==Name==
Galileo claimed the right to name the moons he had discovered. He considered "Cosmian Stars" and settled on "[[Galilean Satellites#Dedication to the Medicis|Medicean Stars]]", in honor of [[Cosimo II de' Medici]].<ref name="Naming" />

The French astronomer [[Nicolas-Claude Fabri de Peiresc]] suggested individual names from the [[Medici]] family for the moons, but his proposal was not taken up.<ref name="Naming" /> [[Simon Marius]], who had originally claimed to have found the Galilean satellites,<ref name="College">{{cite web |url=http://www.cascadia.ctc.edu/facultyweb/instructors/jvanleer/astro%20sum01/astro101/discovery.htm |archive-url=https://web.archive.org/web/20060920121740/http://www.cascadia.ctc.edu/facultyweb/instructors/jvanleer/astro%20sum01/astro101/discovery.htm |archive-date=September 20, 2006 |title=Discovery |work=Cascadia Community College |access-date=November 24, 2007 }}</ref> tried to name the moons the "Saturn of Jupiter", the "Jupiter of Jupiter" (this was Ganymede), the "Venus of Jupiter", and the "Mercury of Jupiter", another nomenclature that never caught on. Later on, after finding out about a suggestion from [[Johannes Kepler]], Marius agreed with Kepler's proposal and so he then proposed a naming system based on [[Greek mythology]] instead.  This final Kepler/Marius proposal was ultimately successful.<ref name="Naming" />

{{blockquote|Jupiter is much blamed by the poets on account of his irregular loves. Three maidens are especially mentioned as having been clandestinely courted by Jupiter with success. Io, daughter of the River Inachus, Callisto of Lycaon, Europa of Agenor. Then there was Ganymede, the handsome son of King Tros, whom Jupiter, having taken the form of an eagle, transported to heaven on his back, as poets fabulously tell... I think, therefore, that I shall not have done amiss if the First is called by me Io, the Second Europa, the Third, on account of its majesty of light, Ganymede, the Fourth Callisto...<ref name=Helden>{{cite journal |last1=Van Helden |first1=Albert |title=Naming the Satellites of Jupiter and Saturn |journal=The Newsletter of the Historical Astronomy Division of the American Astronomical Society |date=August 1994 |issue=32 |url=https://had.aas.org/sites/had.aas.org/files/HADN32.pdf |access-date=10 March 2023 |archive-date=December 7, 2022 |archive-url=https://web.archive.org/web/20221207151902/https://had.aas.org/sites/had.aas.org/files/HADN32.pdf |url-status=live }}</ref><ref>{{cite book |last1=Marius |first1=Simon |title=Mundus Iovialis: anno MDCIX detectus ope perspicilli Belgici, hoc est, quatuor Jovialium planetarum, cum theoria, tum tabulæ |date=1614 |publisher=Sumptibus & Typis Iohannis Lauri |location=Nuremberg |page=B2, recto and verso (images 35 and 36), with erratum on last page (image 78) |url=https://repository.ou.edu/uuid/748b6fe7-62da-5877-ae84-885372b3030c |access-date=June 30, 2020 |archive-date=July 2, 2020 |archive-url=https://web.archive.org/web/20200702154450/https://repository.ou.edu/uuid/748b6fe7-62da-5877-ae84-885372b3030c |url-status=live }}</ref>}}

This name and those of the other Galilean satellites fell into disfavor for a considerable time, and were not in common use until the mid-20th century. In much of the earlier astronomical literature, Ganymede is referred to instead by its Roman numeral designation, {{nowrap|Jupiter III}} (a system introduced by Galileo), in other words "the third satellite of Jupiter". Following the discovery of moons of Saturn, a naming system based on that of Kepler and Marius was used for Jupiter's moons.<ref name="Naming" /> Ganymede is the only Galilean moon of Jupiter named after a male figure—like Io, Europa, and Callisto, he was a lover of Zeus.

In English, the Galilean satellites Io, Europa and Callisto have the Latin spellings of their names, but the Latin form of Ganymede is ''Ganymēdēs'', which would be pronounced {{IPAc-en|,|g|ae|n|I|'|m|i:|d|i:|z}}.<ref>''Merriam-Webster's Encyclopedia of Literature'', 1995.</ref> However, the final syllable is dropped in English, perhaps under the influence of French ''Ganymède'' ({{IPA|fr|ɡanimɛd|}}).

Planetary moons other than Earth's were never given symbols in the astronomical literature. Denis Moskowitz, a software engineer who designed most of the [[dwarf planet]] symbols, proposed a Greek [[gamma]] (the initial of Ganymede) combined with the cross-bar of the Jupiter symbol as the symbol of Ganymede ([[File:Ganymede symbol (fixed width).svg|16px]]). This symbol is not widely used.<ref name=moons>{{cite web |url=https://www.unicode.org/L2/L2025/25079-phobos-and-deimos.pdf |title=Phobos and Deimos symbols |last1=Bala |first1=Gavin Jared |last2=Miller |first2=Kirk |date=7 March 2025 |website=unicode.org |publisher=The Unicode Consortium |access-date=14 March 2025 |quote=}}</ref>

==Orbit and rotation==
[[File:Galilean moon Laplace resonance animation 2.gif|thumb|right|[[Laplace resonance]] of Ganymede, [[Europa (moon)|Europa]], and [[Io (moon)|Io]] (conjunctions are highlighted by color changes)]]

Ganymede [[orbit]]s Jupiter at a distance of {{convert|1070400|km|mi}}, third among the Galilean satellites,<ref name="Planetary Society" /> and completes a revolution every seven days and three hours (7.155 days<ref>{{Cite web |title=Ganymede: Facts – NASA Science |url=https://science.nasa.gov/jupiter/moons/ganymede/facts/ |access-date=November 18, 2023 |website=science.nasa.gov |language=en}}</ref>). Like most known moons, Ganymede is [[tidal locking|tidally locked]], with one side always facing toward the planet, hence its day is also seven days and three hours.<ref name="The Grand Tour">{{cite book |title=The Grand Tour: A Traveler's Guide to the Solar System |last1=Miller |first1=Ron |author-link=Ron Miller (artist and author) |first2=William K. |last2=Hartmann |date=May 2005 |pages=108–114 |publisher=Workman Publishing |location=Thailand |edition=3rd |isbn=978-0-7611-3547-0 }}</ref> Its orbit is very slightly eccentric and inclined to the Jovian [[equator]], with the [[orbital eccentricity|eccentricity]] and [[inclination]] changing [[almost periodic function|quasi-periodically]] due to solar and planetary gravitational [[perturbation (astronomy)|perturbations]] on a timescale of centuries. The ranges of change are 0.0009–0.0022 and 0.05–0.32°, respectively.<ref name="Musotto2002">{{cite journal |last1=Musotto |first1=Susanna |last2=Varadi |first2=Ferenc |last3=Moore |first3=William |last4=Schubert |first4=Gerald |title=Numerical Simulations of the Orbits of the Galilean Satellites |date=2002 |volume=159 |issue=2 |pages=500–504 |doi=10.1006/icar.2002.6939 |bibcode=2002Icar..159..500M |journal=Icarus }}</ref> These orbital variations cause the [[axial tilt]] (the angle between the rotational and orbital axes) to vary between 0 and 0.33°.<ref name="Bills2005" />

Ganymede participates in [[orbital resonance]]s with Europa and Io: for every orbit of Ganymede, Europa orbits twice and Io orbits four times.<ref name="Musotto2002" /><ref name="SPACE.com">{{cite web |url=http://www.space.com/searchforlife/seti_tidal_europa_021003.html |title=High Tide on Europa |first=Cynthia |last=Phillips|author-link=Cynthia B. Phillips |work=SPACE.com |date=October 3, 2002 |url-status=dead |archive-date=October 17, 2002 |archive-url=https://web.archive.org/web/20021017211633/http://space.com/searchforlife/seti_tidal_europa_021003.html }}</ref> [[Astronomical conjunction|Conjunctions]] (alignment on the same side of Jupiter) between Io and Europa occur when Io is at [[periapsis]] and Europa at [[apoapsis]]. Conjunctions between Europa and Ganymede occur when Europa is at periapsis.<ref name="Musotto2002" /> The longitudes of the Io–Europa and Europa–Ganymede conjunctions change at the same rate, making triple conjunctions impossible. Such a complicated resonance is called the [[Laplace resonance]].<ref name="Showman1997a">{{cite journal |last1=Showman |first1=Adam P. |last2=Malhotra |first2=Renu |title=Tidal Evolution into the Laplace Resonance and the Resurfacing of Ganymede |journal=Icarus |date=1997 |volume=127 |issue=1 |pages=93–111 |doi=10.1006/icar.1996.5669 |url=http://www.lpl.arizona.edu/~showman/publications/showman-malhotra-1997.pdf |bibcode=1997Icar..127...93S |access-date=January 22, 2008 |archive-date=May 14, 2011 |archive-url=https://web.archive.org/web/20110514231007/http://www.lpl.arizona.edu/~showman/publications/showman-malhotra-1997.pdf |url-status=live }}</ref>
The current Laplace resonance is unable to pump the orbital eccentricity of Ganymede to a higher value.<ref name="Showman1997a" /> The value of about 0.0013 is probably a remnant from a previous epoch, when such pumping was possible.<ref name="SPACE.com" /> The Ganymedian orbital eccentricity is somewhat puzzling; if it is not pumped now it should have decayed long ago due to the tidal [[dissipation]] in the interior of Ganymede.<ref name="Showman1997a" /> This means that the last episode of the eccentricity excitation happened only several hundred million years ago.<ref name="Showman1997a" /> Because Ganymede's orbital eccentricity is relatively low—on average 0.0015<ref name="SPACE.com" />—tidal heating is negligible now.<ref name="Showman1997a" /> However, in the past Ganymede may have passed through one or more Laplace-like resonances<ref name="laplaceres" group=lower-alpha /> that were able to pump the orbital eccentricity to a value as high as 0.01–0.02.<ref name="Showman1999" /><ref name="Showman1997a" /> This probably caused a significant tidal heating of the interior of Ganymede; the formation of the grooved terrain may be a result of one or more heating episodes.<ref name="Showman1999" /><ref name="Showman1997a" />

There are two hypotheses for the origin of the Laplace resonance among Io, Europa, and Ganymede: that it is primordial and has existed from the beginning of the Solar System;<ref name="Peale2002">{{cite journal |last1=Peale |first1=S.J. |last2=Lee |first2=Man Hoi |title=A Primordial Origin of the Laplace Relation Among the Galilean Satellites |journal=Science |date=2002 |volume=298 |pages=593–597 |doi=10.1126/science.1076557 |bibcode=2002Sci...298..593P |pmid=12386333 |issue=5593 |arxiv=astro-ph/0210589 |s2cid=18590436 }}</ref> or that it developed after the [[Formation and evolution of the Solar System|formation of the Solar System]]. A possible sequence of events for the latter scenario is as follows: Io raised tides on Jupiter, causing Io's orbit to expand (due to conservation of momentum) until it encountered the 2:1 resonance with Europa; after that, the expansion continued, but some of the angular [[moment (physics)|moment]] was transferred to Europa as the resonance caused its orbit to expand as well; the process continued until Europa encountered the 2:1 resonance with Ganymede.<ref name="Showman1997a" /> Eventually the drift rates of conjunctions between all three moons were synchronized and locked in the Laplace resonance.<ref name="Showman1997a" />

==Physical characteristics==
[[Image:Noaa ganymede.jpg|thumb|Depiction of Ganymede centered over 45° W. longitude; dark areas are Perrine (upper) and Nicholson (lower) regions; prominent craters are Tros (upper right) and Cisti (lower left).]]
[[File:Ganymede - Voyager 2 (26670869304).png|thumb|Three high-resolution views of Ganymede taken by [[Voyager 1]] near closest approach on July 9, 1979]]

===Size===
{{See also|List of Solar System objects by size}}
With a diameter of about {{convert|5270|km|mi}} and a mass of {{convert|1.48E20|tonne|kg lbs}}, Ganymede is the largest and most massive [[Satellite system (astronomy)|moon]] in the [[Solar System]].<ref>{{Cite web|title=Ganymede|url=https://solarsystem.nasa.gov/moons/jupiter-moons/ganymede/in-depth|access-date=June 15, 2021|website=NASA Solar System Exploration|archive-date=November 12, 2018|archive-url=https://web.archive.org/web/20181112163337/https://solarsystem.nasa.gov/moons/jupiter-moons/ganymede/in-depth/|url-status=live}}</ref> It is slightly more massive than the second most massive moon, Saturn's satellite [[Titan (moon)|Titan]], and is more than twice as massive as the Earth's Moon. It is larger than the planet [[Mercury (planet)|Mercury]], which has a diameter of {{convert|4880|km|mi}} but is only 45 percent of Mercury's mass. Ganymede is the ninth-largest object in the solar system, but the tenth-most massive.

===Composition===
The average [[density]] of Ganymede, 1.936 g/cm<sup>3</sup> (a bit greater than Callisto's), suggests a composition of about equal parts rocky material and mostly water [[Ice (planetary science)|ices]].<ref name="Showman1999" /> Some of the water is liquid, forming an underground ocean.<ref name="NYT-20150315" /> The [[mass fraction (chemistry)|mass fraction]] of ices is between 46 and 50 percent, which is slightly lower than that in Callisto.<ref name="Kuskov2005">{{cite journal |last1=Kuskov |first1=O.L. |last2=Kronrod |first2=V.A. |title=Internal structure of Europa and Callisto |date=2005 |volume=177 |issue=2 |pages=550–569|doi=10.1016/j.icarus.2005.04.014 |bibcode=2005Icar..177..550K |journal=Icarus }}</ref> Some additional volatile ices such as [[ammonia]] may also be present.<ref name="Kuskov2005" /><ref name="Spohn2003" /> The exact composition of Ganymede's [[rock (geology)|rock]] is not known, but is probably close to the composition of [[L chondrite|L]]/[[LL chondrite|LL type]] [[ordinary chondrite]]s,<ref name="Kuskov2005" /> which are characterized by less total iron, less metallic iron and more [[iron oxide]] than [[H chondrite]]s. The weight ratio of iron to [[silicon]] ranges between 1.05 and 1.27 in Ganymede, whereas the [[Sun|solar ratio]] is around 1.8.<ref name="Kuskov2005" />

===Surface features===
{{See also|List of geological features on Ganymede}}
{{multiple image
 | align = right
 | total_width = 220
 | image1 = Ganymede 1.png
 | image2 = Ganymede 2.png
}}
{{Multiple image|align=left|direction=vertical|width=180px
|image1=PIA24681-1041-Ganymede-JupiterMoon-Juno-20210607.jpg
|image2=PIA24682-Ganymede-DarkSide-JupiterMoon-20210607.jpg
|footer=<div align="center">Ganymede (''Juno''; June 7, 2021)</div>}}
[[File:Tros Crater, Ganymede - PJ34-1 - Detail - Map Projected.png|thumb|left|[[Tros (crater)|Tros]] crater (''Juno''; June 7, 2021)]]
[[Image:Ganymede-moon.jpg|thumb|Enhanced-color ''Galileo'' spacecraft image of Ganymede's trailing hemisphere.<ref name="Spaceflight Now">{{cite web |url=http://spaceflightnow.com/news/n0012/29ganyflyby/ |title=Galileo has successful flyby of Ganymede during eclipse |work=Spaceflight Now |access-date=January 19, 2008 |archive-date=November 19, 2018 |archive-url=https://web.archive.org/web/20181119064953/https://spaceflightnow.com/news/n0012/29ganyflyby/ |url-status=live }}</ref> The crater Tashmetum's prominent rays are at lower right, and the large ejecta field of Hershef at upper right. Part of dark Nicholson Regio is at lower left, bounded on its upper right by Harpagia Sulcus.]]
[[File:PIA26075-JupiterMoon-GanymedeTerrain-20231030.jpg|thumb|left|Ganymede grooved terrain<br />(''Juno''; June 7, 2021)]]

Ganymede's surface has an [[albedo]] of about 43 percent.<ref name="Calvin1995">{{cite journal |last1=Calvin |first1=Wendy M. |last2=Clark |first2=Roger N. |last3=Brown |first3=Robert H. |last4=Spencer |first4=John R. |title=Spectra of the ice Galilean satellites from 0.2 to 5 μm: A compilation, new observations, and a recent summary |journal=J. Geophys. Res. |date=1995 |volume=100 |issue=E9 |pages=19,041–19,048 |bibcode=1995JGR...10019041C |doi=10.1029/94JE03349 }}</ref> Water ice seems to be ubiquitous on its surface, with a mass fraction of 50–90 percent,<ref name="Showman1999" /> significantly more than in Ganymede as a whole. Near-infrared [[spectroscopy]] has revealed the presence of strong water ice [[absorption band]]s at wavelengths of 1.04, 1.25, 1.5, 2.0 and 3.0 [[micrometre|μm]].<ref name="Calvin1995" /> The grooved terrain is brighter and has a more icy composition than the dark terrain.<ref name="RESA">{{cite web |url=http://www.resa.net/nasa/ganymede.htm |archive-url=https://web.archive.org/web/20071202132022/http://www.resa.net/nasa/ganymede.htm |archive-date=December 2, 2007 |title=Ganymede: the Giant Moon |work=Wayne RESA |access-date=December 31, 2007 }}</ref> The analysis of high-resolution, [[near-infrared]] and [[Ultraviolet|UV]] [[spectrum|spectra]] obtained by the [[Galileo (spacecraft)|''Galileo'']] spacecraft and from Earth observations has revealed various non-water materials: [[carbon dioxide]], [[sulfur dioxide]] and, possibly, [[cyanogen]], [[hydrogen sulfate]] and various [[organic compound]]s.<ref name="Showman1999" /><ref name="McCord1998">{{cite journal |last1=McCord |first1=T.B. |last2=Hansen |first2=G.V. |last3=Clark |first3=R.N. |last4=Martin |first4=P. D. |last5=Hibbitts |first5=C. A. |last6=Fanale |first6=F. P. |last7=Granahan |first7=J. C. |last8=Segura |first8=M. |last9=Matson |first9=D. L. |display-authors=2 |title=Non-water-ice constituents in the surface material of the icy Galilelean satellites from Galileo near-infrared mapping spectrometer investigation |journal=J. Geophys. Res.|date=1998 |volume=103 |issue=E4 |pages=8,603–8,626 |bibcode=1998JGR...103.8603M |doi=10.1029/98JE00788 |doi-access=free }}</ref> ''Galileo'' results have also shown [[magnesium sulfate]] (MgSO<sub>4</sub>) and, possibly, [[sodium sulfate]] (Na<sub>2</sub>SO<sub>4</sub>) on Ganymede's surface.<ref name="The Grand Tour" /><ref name="McCord2001">{{cite journal |last1=McCord |first1=Thomas B. |last2=Hansen |first2=Gary B. |last3=Hibbitts |first3=Charles A. |title=Hydrated Salt Minerals on Ganymede's Surface: Evidence of an Ocean Below |journal=Science |date=2001 |volume=292 |pages=1523–1525 |doi=10.1126/science.1059916 |bibcode=2001Sci...292.1523M |pmid=11375486 |issue=5521 |s2cid=40346198 }}</ref> These salts may originate from the subsurface ocean.<ref name="McCord2001" />

[[Image:Craters on Ganymede.jpg|thumb|The craters [[Gula (crater)|Gula]] and [[Achelous (crater)|Achelous]] (bottom), in the grooved terrain of Ganymede, with [[ejecta blanket|ejecta]] "[[pedestal crater|pedestals]]" and [[rampart crater|ramparts]]]]
The Ganymedian surface albedo is very asymmetric; the leading hemisphere<ref name="hemispherecomment" group=lower-alpha /> is brighter than the trailing one.<ref name="Calvin1995" /> This is similar to Europa, but the reverse for Callisto.<ref name="Calvin1995" /> The trailing hemisphere of Ganymede appears to be enriched in sulfur dioxide.<ref name="Domingue1996">{{cite journal |last1=Domingue |first1=Deborah |last2=Lane |first2=Arthur |last3=Moth |first3=Pimol |title=Evidence from IUE for Spatial and Temporal Variations in the Surface Composition of the Icy Galilean Satellites |journal=Bulletin of the American Astronomical Society |date=1996 |volume=28 |page=1070 |bibcode=1996DPS....28.0404D }}</ref><ref name="Domingue1998">{{cite journal |last1=Domingue |first1=Deborah L. |last2=Lane |first2=Arthur L. |last3=Beyer |first3=Ross A. |title=IEU's detection of tenuous SO2 frost on Ganymede and its rapid time variability |journal=Geophys. Res. Lett. |date=1998 |volume=25 |issue=16 |pages=3,117–3,120 |doi=10.1029/98GL02386 |bibcode=1998GeoRL..25.3117D |s2cid=128823420 |doi-access=free }}</ref> The distribution of carbon dioxide does not demonstrate any hemispheric asymmetry, but little or no carbon dioxide is observed near the poles.<ref name="McCord1998" /><ref name="Hibbitts2003">{{cite journal |last1=Hibbitts |first1=C.A. |last2=Pappalardo |first2=R. |last3=Hansen |first3=G.V. |last4=McCord |first4=T.B. |title=Carbon dioxide on Ganymede |journal=J. Geophys. Res. |date=2003 |volume=108 |issue=E5 |pages=5,036 |doi=10.1029/2002JE001956 |bibcode=2003JGRE..108.5036H |doi-access=free }}</ref> [[Impact crater]]s on Ganymede (except one) do not show any enrichment in carbon dioxide, which also distinguishes it from Callisto. Ganymede's carbon dioxide gas was probably depleted in the past.<ref name="Hibbitts2003" />
Ganymede's surface is a mix of two types of terrain: very old, highly cratered, dark regions and somewhat younger (but still ancient), lighter regions marked with an extensive array of grooves and ridges. The dark terrain, which comprises about one-third of the surface,<ref name="Patterson2007">{{cite journal |last1=Patterson |first1=Wesley |last2=Head |first2=James W. |last3=Collins |first3=Geoffrey C. |display-authors=2 |title=A Global Geologic Map of Ganymede |journal=Lunar and Planetary Science |date=2007 |volume=XXXVIII |page=1098 |url=http://www.lpi.usra.edu/meetings/lpsc2007/pdf/1098.pdf |access-date=January 30, 2008 |archive-date=March 27, 2009 |archive-url=https://web.archive.org/web/20090327050809/http://www.lpi.usra.edu/meetings/lpsc2007/pdf/1098.pdf |url-status=live }}</ref> contains clays and organic materials that could indicate the composition of the impactors from which Jovian satellites accreted.<ref name="Pappalardo2001">{{cite journal |last1=Pappalardo |first1=R.T. |last2=Khurana |first2=K.K. |last3=Moore |first3=W.B. |title=The Grandeur of Ganymede: Suggested Goals for an Orbiter Mission |journal=Lunar and Planetary Science |date=2001 |volume=XXXII |page=4062 |url=http://www.lpi.usra.edu/meetings/outerplanets2001/pdf/4065.pdf |bibcode=2001iaop.work...62P |access-date=October 21, 2007 |archive-date=March 27, 2009 |archive-url=https://web.archive.org/web/20090327050808/http://www.lpi.usra.edu/meetings/outerplanets2001/pdf/4065.pdf |url-status=live }}</ref>

The heating mechanism required for the formation of the grooved terrain on Ganymede is an unsolved problem in the [[planetary sciences]]. The modern view is that the grooved terrain is mainly [[tectonic]] in nature.<ref name="Showman1999" /> [[Cryovolcano|Cryovolcanism]] is thought to have played only a minor role, if any.<ref name="Showman1999" /> The forces that caused the strong stresses in the Ganymedian ice [[lithosphere]] necessary to initiate the tectonic activity may be connected to the [[tidal heating]] events in the past, possibly caused when the satellite passed through unstable orbital resonances.<ref name="Showman1999" /><ref name="Showman1997b">{{cite journal |last1=Showman |first1=Adam P. |last2=Stevenson |first2=David J. |last3=Malhotra |first3=Renu |title=Coupled Orbital and Thermal Evolution of Ganymede |journal=Icarus |date=1997 |volume=129 |issue=2 |pages=367–383 |doi=10.1006/icar.1997.5778 |url=http://www.lpl.arizona.edu/~showman/publications/showman-etal-1997.pdf |bibcode=1997Icar..129..367S |access-date=January 30, 2008 |archive-date=June 3, 2019 |archive-url=https://web.archive.org/web/20190603184639/http://www.lpl.arizona.edu/~showman/publications/showman-etal-1997.pdf |url-status=live }}</ref> The tidal flexing of the ice may have heated the interior and strained the lithosphere, leading to the development of cracks and [[horst and graben]] faulting, which erased the old, dark terrain on 70 percent of the surface.<ref name="Showman1999" /><ref name="Bland2007">{{cite journal |last1=Bland |last2=Showman |first2=A.P. |last3=Tobie |first3=G. |title=Ganymede's orbital and thermal evolution and its effect on magnetic field generation |journal=Lunar and Planetary Society Conference |date=March 2007 |volume=38 |issue=1338 |page=2020 |url=http://www.lpi.usra.edu/meetings/lpsc2007/pdf/2020.pdf |bibcode=2007LPI....38.2020B |access-date=January 16, 2008 |archive-date=March 27, 2009 |archive-url=https://web.archive.org/web/20090327050813/http://www.lpi.usra.edu/meetings/lpsc2007/pdf/2020.pdf |url-status=live }}</ref>  The formation of the grooved terrain may also be connected with the early core formation and subsequent tidal heating of Ganymede's interior, which may have caused a slight expansion of Ganymede by one to six percent due to [[phase transition]]s in ice and [[thermal expansion]].<ref name="Showman1999" /> During subsequent evolution deep, hot water [[plume (hydrodynamics)|plumes]] may have risen from the core to the surface, leading to the tectonic deformation of the lithosphere.<ref name="Barr">{{cite journal |last1=Barr |first1=A.C. |last2=Pappalardo |first2=R. T. |last3=Pappalardo |first3=Stevenson |date=2001 |title=Rise of Deep Melt into Ganymede's Ocean and Implications for Astrobiology |journal=Lunar and Planetary Science Conference |volume=32 |url=http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1781.pdf |page=1781 |bibcode=2001LPI....32.1781B |access-date=January 10, 2008 |archive-date=March 27, 2009 |archive-url=https://web.archive.org/web/20090327050810/http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1781.pdf |url-status=live }}</ref> [[Radiogenic heat]]ing within the satellite is the most relevant current heat source, contributing, for instance, to ocean depth. Research models have found that if the orbital eccentricity were an order of magnitude greater than currently (as it may have been in the past), tidal heating would be a more substantial heat source than radiogenic heating.<ref name="gra.6">{{cite journal |last1=Huffmann |first1=H. |last2=Sohl |first2=F. |date=2004 |title=Internal Structure and Tidal Heating of Ganymede |journal=Geophysical Research Abstracts |volume=6 |url=http://www.cosis.net/abstracts/EGU04/05114/EGU04-J-05114.pdf |display-authors=1 |access-date=January 21, 2008 |archive-date=March 27, 2009 |archive-url=https://web.archive.org/web/20090327050805/http://www.cosis.net/abstracts/EGU04/05114/EGU04-J-05114.pdf |url-status=live }}</ref>

Cratering is seen on both types of terrain, but is especially extensive on the dark terrain: it appears to be saturated with impact craters and has evolved largely through impact events.<ref name="Showman1999" /> The brighter, grooved terrain contains many fewer impact features, which have been only of minor importance to its tectonic evolution.<ref name="Showman1999" /> The density of cratering indicates an age of 4&nbsp;billion years for the dark terrain, similar to the highlands of the Moon, and a somewhat younger age for the grooved terrain (but how much younger is uncertain).<ref name="Zahnle1998">{{cite journal|last1=Zahnle |first1=K. |last2=Dones |first2=L. |title=Cratering Rates on the Galilean Satellites |journal=Icarus |date=1998 |volume=136 |issue=2 |pages=202–222 |doi=10.1006/icar.1998.6015 |url=http://lasp.colorado.edu/icymoons/europaclass/Zahnle_etal_1998.pdf |pmid=11878353 |bibcode=1998Icar..136..202Z |url-status=dead |archive-url=https://web.archive.org/web/20080227015923/http://lasp.colorado.edu/icymoons/europaclass/Zahnle_etal_1998.pdf |archive-date=February 27, 2008 }}</ref> Ganymede may have experienced a period of heavy cratering 3.5 to 4&nbsp;billion years ago similar to that of the Moon.<ref name="Zahnle1998" /> If true, the vast majority of impacts happened in that epoch, whereas the cratering rate has been much smaller since.<ref name="nineplanets.org-Ganymede">{{cite web |publisher=nineplanets.org |title=Ganymede |date=October 31, 1997 |url=http://www.nineplanets.org/ganymede.html |access-date=February 27, 2008 |archive-date=August 27, 2019 |archive-url=https://web.archive.org/web/20190827231253/https://nineplanets.org/ganymede.html |url-status=live }}</ref> Craters both overlay and are crosscut by the groove systems, indicating that some of the grooves are quite ancient. Relatively young craters with rays of ejecta are also visible.<ref name="nineplanets.org-Ganymede" /><ref name="Ganymede">{{cite web |work=Lunar and Planetary Institute |title=Ganymede |date=1997 |url=http://www.lpi.usra.edu/resources/outerp/gany.html |access-date=February 7, 2007 |archive-date=February 11, 2017 |archive-url=https://web.archive.org/web/20170211103518/http://www.lpi.usra.edu/resources/outerp/gany.html |url-status=live }}</ref> Ganymedian craters are flatter than those on the Moon and Mercury. This is probably due to the relatively weak nature of Ganymede's icy crust, which can (or could) flow and thereby soften the relief. Ancient craters whose relief has disappeared leave only a "ghost" of a crater known as a [[Palimpsest (planetary astronomy)|palimpsest]].<ref name="nineplanets.org-Ganymede" />

One significant feature on Ganymede is a dark plain named [[Galileo Regio]], which contains a series of concentric grooves, or furrows, likely created during a period of geologic activity.<ref name="Casacchia">{{cite journal |last1=Casacchia |first1=R. |last2=Strom |first2=R.G. |date=1984 |title=Geologic evolution of Galileo Regio |journal=Journal of Geophysical Research |volume=89 |issue=S02 |pages=B419–B428 |bibcode=1984LPSC...14..419C |doi=10.1029/JB089iS02p0B419 }}</ref>

Ganymede also has polar caps, likely composed of water frost. The frost extends to 40° latitude.<ref name="The Grand Tour" /> These polar caps were first seen by the [[Voyager program|''Voyager'']] spacecraft. Theories on the formation of the caps include the migration of water to higher latitudes and the bombardment of the ice by plasma. Data from ''Galileo'' suggests the latter is correct.<ref name="Polar caps" /> The presence of a magnetic field on Ganymede results in more intense charged particle bombardment of its surface in the unprotected polar regions; sputtering then leads to redistribution of water molecules, with frost migrating to locally colder areas within the polar terrain.<ref name="Polar caps">{{cite journal |last1=Khurana |first1=Krishan K. |last2=Pappalardo |first2=Robert T. |last3=Murphy |first3=Nate |last4=Denk |first4=Tilmann |date=2007 |title=The origin of Ganymede's polar caps |journal=Icarus |volume=191 |issue=1 |pages=193–202 |doi=10.1016/j.icarus.2007.04.022 |bibcode=2007Icar..191..193K }}</ref>

A crater named [[Anat (crater)|Anat]] provides the reference point for measuring longitude on Ganymede. By definition, Anat is at 128° longitude.<ref name="iau.table2">{{cite web |url=https://astrogeology.usgs.gov/Projects/WGCCRE/constants/iau2000_table2.html |title=USGS Astrogeology: Rotation and pole position for planetary satellites (IAU WGCCRE) |access-date=August 28, 2017 |archive-url=https://web.archive.org/web/20111024101848/http://astrogeology.usgs.gov/Projects/WGCCRE/constants/iau2000_table2.html |archive-date=October 24, 2011 |url-status=dead }}</ref> The 0° longitude directly faces Jupiter, and unless stated otherwise longitude increases toward the west.<ref name="targetcoordsys">{{cite web|title=Planetary Names: Target Coordinate Systems|url=http://planetarynames.wr.usgs.gov/TargetCoordinates|website=planetarynames.wr.usgs.gov|publisher=International Astronomical Union|access-date=May 21, 2016|archive-url=https://web.archive.org/web/20160527032231/http://planetarynames.wr.usgs.gov/TargetCoordinates|archive-date=May 27, 2016|url-status=dead}}</ref>

===Internal structure===
Ganymede appears to be fully [[Planetary differentiation|differentiated]], with an internal structure consisting of an [[iron(II) sulfide|iron-sulfide]]–iron [[core (geology)|core]], a [[silicate]] [[mantle (geology)|mantle]], and outer layers of water ice and liquid water.<ref name="Showman1999" /><ref name="Sohl2002">{{cite journal |last1=Sohl |first1=F. |last2=Spohn |first2=T |last3=Breuer |first3=D. |last4=Nagel |first4=K. |title=Implications from Galileo Observations on the Interior Structure and Chemistry of the Galilean Satellites |journal=Icarus |date=2002 |volume=157 |issue=1 |pages=104–119 |doi=10.1006/icar.2002.6828 |bibcode=2002Icar..157..104S }}</ref>
<ref name="Bhatia2017">{{cite journal|last1=Bhatia|first1= G.K.|last2=Sahijpal|first2= S.|title=Thermal evolution of trans-Neptunian objects, icy satellites, and minor icy planets in the early solar system |journal=Meteoritics & Planetary Science |doi=10.1111/maps.12952|volume=52|issue= 12|year=2017|pages=2470–2490|bibcode=2017M&PS...52.2470B|s2cid= 133957919|doi-access=free}}</ref> The precise thicknesses of the different layers in the interior of Ganymede depend on the assumed composition of silicates (fraction of [[olivine]] and [[pyroxene]]) and amount of [[sulfur]] in the core.<ref name="Kuskov2005" /><ref name="Sohl2002" /><ref name="Kuskov2005b">{{cite journal |last1=Kuskov |first1=O.L. |last2=Kronrod |first2=V.A. |last3=Zhidikova |first3=A.P. |title=Internal Structure of Icy Satellites of Jupiter |journal=Geophysical Research Abstracts |date=2005 |volume=7 |page=01892 |url=http://www.cosis.net/abstracts/EGU05/01892/EGU05-J-01892.pdf |access-date=January 21, 2008 |archive-date=March 27, 2009 |archive-url=https://web.archive.org/web/20090327050809/http://www.cosis.net/abstracts/EGU05/01892/EGU05-J-01892.pdf |url-status=live }}</ref><ref name="Kuskov2005c">{{Cite journal |last1=Kuskov |first1=O. L. |last2=Kronrod |first2=V. A. |last3=Zhidikova |first3=A. P. |date=May 2010 |title=Internal Structure of Icy Satellites of Jupiter |journal=Advances in Geosciences |language=en |publisher=World Scientific |volume=19 |pages=365–376 |bibcode=2010aogs...19..365K |doi=10.1142/9789812838162_0028 |doi-broken-date=November 1, 2024 |isbn=9789812838162 |editor-first1=Anil |editor-last1=Bhardwaj}}</ref> Ganymede has the lowest [[moment of inertia factor]], 0.31,<ref name="Showman1999" /> among the solid Solar System bodies. This is a consequence of its substantial water content and fully differentiated interior.

====Subsurface oceans====
[[File:Ganymede diagram.svg|thumb|upright=2|Artist's cut-away representation of the internal structure of Ganymede. Layers drawn to scale.]]
In the 1970s, NASA scientists first suspected that Ganymede had a thick ocean between two layers of ice, one on the surface and one beneath a liquid ocean and atop the rocky mantle.<ref name="Showman1999" /><ref name="clubsandwich 2014" /><ref name="Sohl2002" /><ref name="Freeman2006">{{cite journal |last=Freeman |first=J. |title=Non-Newtonian stagnant lid convection and the thermal evolution of Ganymede and Callisto |journal=Planetary and Space Science |date=2006 |volume=54 |issue=1 |pages=2–14 |doi=10.1016/j.pss.2005.10.003 |url=http://bowfell.geol.ucl.ac.uk/~lidunka/EPSS-papers/pete2.pdf |archive-url=https://web.archive.org/web/20070824155106/http://bowfell.geol.ucl.ac.uk/~lidunka/EPSS-papers/pete2.pdf |archive-date=August 24, 2007 |bibcode=2006P&SS...54....2F }}</ref><ref name="amount of water in ocean">{{cite web | url=http://earthsky.org/space/underground-ocean-on-jupiters-largest-moon | title=Underground ocean on Jupiter's largest moon | publisher=EarthSky | date=March 15, 2015 | access-date=August 14, 2015 | archive-date=October 11, 2019 | archive-url=https://web.archive.org/web/20191011045129/https://earthsky.org/space/underground-ocean-on-jupiters-largest-moon | url-status=live }}</ref> In the 1990s, NASA's ''Galileo'' mission flew by Ganymede, and found indications of such a subsurface ocean.<ref name="NYT-20150315">{{cite news |last=Chang |first=Kenneth |title=Suddenly, It Seems, Water Is Everywhere in Solar System |url=https://www.nytimes.com/2015/03/13/science/space/suddenly-it-seems-water-is-everywhere-in-solar-system.html |date=March 12, 2015 |work=[[New York Times]] |access-date=March 12, 2015 |archive-date=May 9, 2020 |archive-url=https://web.archive.org/web/20200509080640/https://www.nytimes.com/2015/03/13/science/space/suddenly-it-seems-water-is-everywhere-in-solar-system.html |url-status=live }}</ref> An analysis published in 2014, taking into account the realistic thermodynamics for water and effects of salt, suggests that Ganymede might have a stack of several ocean layers separated by different [[phases of ice]], with the lowest liquid layer adjacent to the rocky [[Mantle (geology)|mantle]].<ref name="clubsandwich 2014" /><ref name="Vance" /><ref name="NASA-20140501c" /><ref name="Hubble 2015">{{cite news |url=http://phys.org/news/2015-03-hubble-underground-ocean-jupiter-largest.html |title=Hubble observations suggest underground ocean on Jupiter's largest moon Ganymede |work=NASA |publisher=PhysOrg |date=March 12, 2015 |access-date=March 13, 2015 |archive-date=March 28, 2022 |archive-url=https://web.archive.org/web/20220328173030/https://phys.org/news/2015-03-hubble-underground-ocean-jupiter-largest.html |url-status=live }}</ref> Water–rock contact may be an important factor in the [[Abiogenesis|origin of life]].<ref name="clubsandwich 2014" /> The analysis also notes that the extreme depths involved (~800&nbsp;km to the rocky "seafloor") mean that temperatures at the bottom of a convective (adiabatic) ocean can be up to 40 K higher than those at the ice–water interface.

In March 2015, scientists reported that measurements with the Hubble Space Telescope of how the [[aurora]]e moved confirmed that Ganymede has a subsurface ocean.<ref name="NYT-20150315"/> A large saltwater ocean affects Ganymede's magnetic field, and consequently, its aurorae.<ref name="Ocean Hubble"/><ref name="Hubble 2015"/><ref name="sciencedaily1503">{{Cite web | url=https://www.sciencedaily.com/releases/2015/03/150312112112.htm | title=Underground ocean on Jupiter's largest moon, Ganymede | access-date=March 9, 2018 | archive-date=November 16, 2018 | archive-url=https://web.archive.org/web/20181116100344/https://www.sciencedaily.com/releases/2015/03/150312112112.htm | url-status=live }}</ref><ref name="sswater1">{{cite journal | last1 = Saur | first1 = Joachim | last2 = Duling | first2 = Stefan | last3 = Roth | first3 = Lorenz | last4 = Jia | first4 = Xianzhe | last5 = Strobel | first5 = Darrell F. | last6 = Feldman | first6 = Paul D. | last7 = Christensen | first7 = Ulrich R. | last8 = Retherford | first8 = Kurt D. | last9 = McGrath | first9 = Melissa A. | last10 = Musacchio | first10 = Fabrizio | last11 = Wennmacher | first11 = Alexandre | last12 = Neubauer | first12 = Fritz M. | last13 = Simon | first13 = Sven | last14 = Hartkorn | first14 = Oliver | year = 2015 | title = The Search for a Subsurface Ocean in Ganymede with Hubble Space Telescope Observations of its Auroral Ovals | url = http://kth.diva-portal.org/smash/get/diva2:814598/FULLTEXT01 | journal = Journal of Geophysical Research: Space Physics | volume = 120 | issue = 3 | pages = 1715–1737 | doi = 10.1002/2014JA020778 | bibcode = 2015JGRA..120.1715S | hdl = 2027.42/111157 | doi-access = free | access-date = August 25, 2019 | archive-date = July 20, 2018 | archive-url = https://web.archive.org/web/20180720185410/http://kth.diva-portal.org/smash/get/diva2:814598/FULLTEXT01 | url-status = live | hdl-access = free }}</ref> The evidence suggests that Ganymede's oceans might be the largest in the entire Solar System.<ref name='Sci Am 2017'>{{Cite news |url=https://www.scientificamerican.com/article/overlooked-ocean-worlds-fill-the-outer-solar-system/ |title=Overlooked Ocean Worlds Fill the Outer Solar System |first=John |last=Wenz |work=Scientific American |date=October 4, 2017 |access-date=January 6, 2018 |archive-date=December 26, 2018 |archive-url=https://web.archive.org/web/20181226133924/https://www.scientificamerican.com/article/overlooked-ocean-worlds-fill-the-outer-solar-system/ |url-status=live }}</ref> These observations were later supported by ''[[Juno (spacecraft)|Juno]]'', which detected various salts and other compounds on Ganymede's surface, including [[hydrohalite|hydrated sodium chloride]], [[ammonium chloride]], [[sodium bicarbonate]], and possibly [[aldehyde|aliphatic aldehydes]]. These compounds were potentially deposited from Ganymede's ocean in past resurfacing events and were discovered to be most abundant in Ganymede's lower latitudes, shielded by its small magnetosphere.<ref>{{Cite web |title=Ganymede moon has a huge internal ocean and salty surface |url=https://www.earth.com/news/jupiters-moon-ganymede-has-huge-internal-ocean-and-salty-surface/ |access-date=November 18, 2023 |website=Earth.com |language=en}}</ref> As a result of these findings, there is increasing speculation on the potential [[planetary habitability|habitability]] of Ganymede's ocean.<ref name="amount of water in ocean"/><ref name="subsurface ocean found">{{cite news | url=https://www.independent.co.uk/news/science/ganymede-oceans-on-jupiters-moon-could-have-been-home-to-alien-life-10106286.html | archive-url= https://web.archive.org/web/20150313232038/https://www.independent.co.uk/news/science/ganymede-oceans-on-jupiters-moon-could-have-been-home-to-alien-life-10106286.html| archive-date= March 13, 2015| url-status= dead| title=Ganymede: oceans on Jupiter's moon could have been home to alien life | newspaper=The Independent | date=March 13, 2015 | access-date= February 19, 2018 | author=Griffin, Andrew}}</ref>

====Core====
The existence of a liquid, [[iron–nickel alloy|iron–nickel]]-rich core<ref name="Bhatia2017" /> provides a natural explanation for the intrinsic [[magnetosphere|magnetic field]] of Ganymede detected by ''Galileo'' spacecraft.<ref name="Hauk2006">{{cite journal |last1=Hauck |first1=Steven A. |last2=Aurnou |first2=Jonathan M. |last3=Dombard |first3=Andrew J. |title=Sulfur's impact on core evolution and magnetic field generation on Ganymede |journal=J. Geophys. Res.|date=2006 |volume=111 |issue=E9 |pages=E09008 |doi=10.1029/2005JE002557 |bibcode=2006JGRE..111.9008H |doi-access=free }}</ref> The [[convection]] in the liquid iron, which has high [[electrical conductivity]], is the most reasonable model of magnetic field generation.<ref name="Kivelson2002" /> The density of the core is 5.5–6 g/cm<sup>3</sup> and the silicate mantle is 3.4–3.6 g/cm<sup>3</sup>.<ref name="Kuskov2005" /><ref name="Sohl2002" /><ref name="Kuskov2005b" /><ref name="Hauk2006" /> The radius of this core may be up to 500&nbsp;km.<ref name="Hauk2006" /> The temperature in the core of Ganymede is probably 1500–1700 K and pressure up to {{convert|10|GPa|atm|abbr=on}}.<ref name="Sohl2002" /><ref name="Hauk2006" />

===Atmosphere and ionosphere===
In 1972, a team of Indian, British and American astronomers working in [[Java]], [[Indonesia]] and [[Kavalur]], India claimed that they had detected a thin atmosphere during an [[occultation]], when it and Jupiter passed in front of a [[star]].<ref name="Carlson1973">{{cite journal |last1=Carlson |first1=R.W. |last2=Bhattacharyya |first2=J. C. |author-link2=J. C. Bhattacharyya |last3=Smith |first3=B.A. |last4=Johnson |first4=T. V. |last5=Hidayat |first5=B. |last6=Smith |first6=S. A. |last7=Taylor |first7=G. E. |last8=O'Leary |first8=B. |last9=Brinkmann |first9=R. T. |display-authors=2 |title=Atmosphere of Ganymede from its occultation of SAO 186800 on 7 June 1972 |journal=Science |date=1973 |volume=182 |bibcode=1973Sci...182...53C |doi=10.1126/science.182.4107.53 |issue=4107 |pmid=17829812 |pages=53–5 |s2cid=33370778 |url=http://authors.library.caltech.edu/61963/1/1736235.pdf |access-date=April 20, 2018 |archive-date=December 2, 2017 |archive-url=https://web.archive.org/web/20171202104832/https://authors.library.caltech.edu/61963/1/1736235.pdf |url-status=live }}</ref> They estimated that the surface pressure was around 0.1 [[Pascal (unit)|Pa]] (1 microbar).<ref name="Carlson1973" /> However, in 1979, ''[[Voyager 1]]'' observed an occultation of the star [[Kappa Centauri|κ Centauri]] during its flyby of Jupiter, with differing results.<ref name="Broadfoot1981">{{cite journal |last1=Broadfoot |first1=A.L. |last2=Sandel |first2=B.R. |last3=Shemansky |first3=D.E. |last4=McConnell |first4=J. C. |last5=Smith |first5=G. R. |last6=Holberg |first6=J. B. |last7=Atreya |first7=S. K. |last8=Donahue |first8=T. M. |last9=Strobel |first9=D. F. |display-authors=2 |title=Overview of the Voyager Ultraviolet Spectrometry Results through Jupiter Encounter |journal=Journal of Geophysical Research |date=1981 |volume=86 |issue=A10 |pages=8259–8284 |url=http://www-personal.umich.edu/~atreya/Articles/1981_Overview_Voyager.pdf |bibcode=1981JGR....86.8259B |doi=10.1029/JA086iA10p08259 |access-date=January 16, 2008 |archive-date=March 27, 2009 |archive-url=https://web.archive.org/web/20090327050807/http://www-personal.umich.edu/~atreya/Articles/1981_Overview_Voyager.pdf |url-status=live }}</ref> The occultation measurements were conducted in the [[far-ultraviolet]] spectrum at [[wavelength]]s shorter than 200 [[nanometre|nm]], which were much more sensitive to the presence of gases than the 1972 measurements made in the [[visible spectrum]]. No atmosphere was revealed by the ''Voyager'' data. The upper limit on the surface particle [[number density]] was found to be {{nowrap|1.5{{E|9}} cm<sup>−3</sup>}}, which corresponds to a surface pressure of less than 2.5 μPa (25 picobar).<ref name="Broadfoot1981" /> The latter value is almost five orders of magnitude less than the 1972 estimate.<ref name="Broadfoot1981" />
[[Image:Map of temparatureof ganymede.jpg|thumb|left|False-color temperature map of Ganymede]]
Despite the ''Voyager'' data, evidence for a tenuous oxygen atmosphere ([[exosphere]]) on Ganymede, very similar to the one found on Europa, was found by the [[Hubble Space Telescope]] (HST) in 1995.<ref name="Hall1998" /><ref name="JPLAtmosphere">{{cite web |archive-url= https://web.archive.org/web/20090504072525/http://www2.jpl.nasa.gov/galileo/hst7.html |url= http://www2.jpl.nasa.gov/galileo/hst7.html|title=Hubble Finds Thin Oxygen Atmosphere on Ganymede |work=Jet Propulsion Laboratory |publisher=NASA |date=October 23, 1996 |access-date= February 17, 2017|url-status= dead |archive-date= May 4, 2009}}</ref> HST actually observed [[airglow]] of atomic oxygen in the far-ultraviolet at the wavelengths 130.4&nbsp;nm and 135.6&nbsp;nm. Such an airglow is excited when [[molecular oxygen]] is [[dissociation (chemistry)|dissociated]] by electron impacts,<ref name="Hall1998" /> which is evidence of a significant neutral atmosphere composed predominantly of O<sub>2</sub> molecules. The surface number density probably lies in the {{nowrap |(1.2–7){{E|8}} cm<sup>−3</sup>}} range, corresponding to the surface pressure of {{nowrap |0.2–1.2 μPa}}.<ref name="Hall1998" /><ref name="surfacedensitynumber" group=lower-alpha /> These values are in agreement with ''Voyager''<nowiki>'</nowiki>s upper limit set in 1981. The oxygen is not evidence of life; it is thought to be produced when water ice on Ganymede's surface is split into [[hydrogen]] and oxygen by radiation, with the hydrogen then being more rapidly lost due to its low atomic mass.<ref name="JPLAtmosphere" /> The airglow observed over Ganymede is not spatially homogeneous like that observed over Europa. HST observed two bright spots located in the northern and southern hemispheres, near ± 50° latitude, which is exactly the boundary between the open and closed field lines of the Ganymedian magnetosphere (see below).<ref name="Feldman2000">{{cite journal |last1=Feldman |first1=Paul D. |last2=McGrath |first2=Melissa A. |last3=Strobell |first3=Darrell F. |last4=Moos |first4=H. Warren |last5=Retherford |first5=Kurt D. |last6=Wolven |first6=Brian C. |display-authors=2 |title=HST/STIS Ultraviolet Imaging of Polar Aurora on Ganymede |journal=The Astrophysical Journal |date=2000 |volume=535 |issue=2 |pages=1085–1090 |doi=10.1086/308889 |bibcode=2000ApJ...535.1085F |arxiv=astro-ph/0003486 |s2cid=15558538 }}</ref> The bright spots are probably polar [[aurora (astronomy)|auroras]], caused by plasma precipitation along the open field lines.<ref name="Johnson1997">{{cite journal |last=Johnson |first=R.E. |date=1997 |title=Polar "Caps" on Ganymede and Io Revisited |journal=Icarus |volume=128 |issue=2 |pages=469–471 |bibcode=1997Icar..128..469J |doi=10.1006/icar.1997.5746 }}</ref>

The existence of a neutral atmosphere implies that an [[ionosphere]] should exist, because oxygen molecules are ionized by the impacts of the energetic [[electron]]s coming from the magnetosphere<ref name="Paranicas1999">{{cite journal |last1=Paranicas |first1=C. |last2=Paterson |first2=W. R. |last3=Cheng |first3=A. F. |last4=Mauk |first4=B. H. |last5=McEntire |first5=R. W. |last6=Frank |first6=L. A. |last7=Williams |first7=D. J. |display-authors=2 |title=Energetic particles observations near Ganymede |journal=J. Geophys. Res. |date=1999 |volume=104 |issue=A8 |pages=17,459–17,469 |doi=10.1029/1999JA900199 |bibcode=1999JGR...10417459P }}</ref> and by solar [[Extreme ultraviolet|EUV]] radiation.<ref name="Eviatar2001" /> However, the nature of the Ganymedian ionosphere is as controversial as the nature of the atmosphere. Some ''Galileo'' measurements found an elevated electron density near Ganymede, suggesting an ionosphere, whereas others failed to detect anything.<ref name="Eviatar2001" /> The electron density near the surface is estimated by different sources to lie in the range 400–2,500&nbsp;cm<sup>−3</sup>.<ref name="Eviatar2001" /> As of 2008, the parameters of the ionosphere of Ganymede were not well constrained.

Additional evidence of the oxygen atmosphere comes from spectral detection of gases trapped in the ice at the surface of Ganymede. The detection of [[ozone]] (O<sub>3</sub>) bands was announced in 1996.<ref name="Noll1996">{{cite journal |last1=Noll |first1=Keith S. |last2=Johnson |first2=Robert E. |last3=Domingue |first3=D. L. |last4=Weaver |first4=H. A. |display-authors=2 |date=July 1996 |title=Detection of Ozone on Ganymede |journal=Science |volume=273 |issue=5273 |pages=341–343 |doi=10.1126/science.273.5273.341 |pmid=8662517 |bibcode=1996Sci...273..341N |s2cid=32074586 }}</ref> In 1997 spectroscopic analysis revealed the [[Dimer (chemistry)|dimer]] (or [[diatomic]]) absorption features of molecular oxygen. Such an absorption can arise only if the oxygen is in a dense phase. The best candidate is molecular oxygen trapped in ice. The depth of the dimer absorption bands depends on [[latitude]] and [[longitude]], rather than on surface albedo—they tend to decrease with increasing latitude on Ganymede, whereas O<sub>3</sub> shows an opposite trend.<ref name="Oxygen97">{{cite journal |last1=Calvin |first1=Wendy M. |last2=Spencer |first2=John R. |date=December 1997 |title=Latitudinal Distribution of O<sub>2</sub> on Ganymede: Observations with the Hubble Space Telescope |journal=Icarus |volume=130 |issue=2 |pages=505–516 |doi=10.1006/icar.1997.5842 |bibcode=1997Icar..130..505C |url=https://zenodo.org/record/1229830 |access-date=July 13, 2019 |archive-date=December 2, 2020 |archive-url=https://web.archive.org/web/20201202001450/https://zenodo.org/record/1229830 |url-status=live }}</ref> Laboratory work has found that O<sub>2</sub> would not cluster or bubble but would dissolve in ice at Ganymede's relatively warm surface temperature of 100 K (−173.15&nbsp;°C).<ref name="sci.5320">{{cite journal |last1=Vidal |first1=R. A. |last2=Bahr |first2=D. |s2cid=27378519 |date=1997 |title=Oxygen on Ganymede: Laboratory Studies |journal=Science |volume=276 |issue=5320 |pages=1839–1842 |bibcode=1997Sci...276.1839V |doi=10.1126/science.276.5320.1839 |pmid=9188525 |display-authors=1 }}</ref>

A search for [[sodium]] in the atmosphere, just after such a finding on Europa, turned up nothing in 1997. Sodium is at least 13 times less abundant around Ganymede than around Europa, possibly because of a relative deficiency at the surface or because the magnetosphere fends off energetic particles.<ref name="ic.126.1">{{cite journal |last=Brown |first=Michael E. |date=1997 |title=A Search for a Sodium Atmosphere around Ganymede |journal=Icarus |volume=126 |issue=1 |pages=236–238  |bibcode=1997Icar..126..236B |doi=10.1006/icar.1996.5675 |citeseerx=10.1.1.24.7010 }}</ref> Another minor constituent of the Ganymedian atmosphere is [[atomic hydrogen]]. Hydrogen atoms were observed as far as 3,000&nbsp;km from Ganymede's surface. Their density on the surface is about {{nowrap |1.5{{E|4}} cm<sup>−3</sup>}}.<ref name="Barth1997">{{cite journal |last1=Barth |first1=C.A. |last2=Hord |first2=C.W. |last3=Stewart |first3=A.I. |last4=Pryor |first4=W. R. |last5=Simmons |first5=K. E. |last6=McClintock |first6=W. E. |last7=Ajello |first7=J. M. |last8=Naviaux |first8=K. L. |last9=Aiello |first9=J. J. |s2cid=123038216 |display-authors=2 |title=Galileo ultraviolet spectrometer observations of atomic hydrogen in the atmosphere of Ganymede |journal=Geophys. Res. Lett. |date=1997 |volume=24 |issue=17 |pages=2147–2150 |bibcode=1997GeoRL..24.2147B |doi=10.1029/97GL01927 |doi-access=free }}</ref>

In 2021, water vapour was detected in the atmosphere of Ganymede.<ref>[https://www.space.com/jupiter-moon-ganymede-water-vapor-discovery Water vapor detected on huge Jupiter moon Ganymede for 1st time] {{Webarchive|url=https://web.archive.org/web/20210806162110/https://www.space.com/jupiter-moon-ganymede-water-vapor-discovery |date=August 6, 2021 }}, Space.com</ref>

===Magnetosphere===
[[Image:Ganymede magnetic field.svg#Summary|thumb|Magnetic field of the Jovian satellite Ganymede, which is embedded into the magnetosphere of Jupiter. Closed field lines are marked with green color.]]
The ''Galileo'' craft made six close flybys of Ganymede from 1995 to 2000 (G1, G2, G7, G8, G28 and G29)<ref name="Kivelson2002" /> and discovered that Ganymede has a permanent (intrinsic) [[magnetic moment]] independent of the Jovian magnetic field.<ref name="Kivelson1997">{{cite journal |last1=Kivelson |first1=M.G. |last2=Khurana |first2=K.K. |last3=Coroniti |first3=F.V. |last4=Joy |first4=S. |last5=Russell |first5=C. T. |last6=Walker |first6=R. J. |last7=Warnecke |first7=J. |last8=Bennett |first8=L. |last9=Polanskey |first9=C. |display-authors=2 |title=The magnetic field and magnetosphere of Ganymede |journal=Geophys. Res. Lett. |date=1997 |volume=24 |issue=17 |pages=2155–2158 |doi=10.1029/97GL02201 |url=http://www.igpp.ucla.edu/people/mkivelson/Publications/97GL02201.pdf |bibcode=1997GeoRL..24.2155K |doi-access=free |access-date=January 15, 2008 |archive-date=March 27, 2009 |archive-url=https://web.archive.org/web/20090327050805/http://www.igpp.ucla.edu/people/mkivelson/Publications/97GL02201.pdf |url-status=live }}</ref> The value of the moment is about {{nowrap |1.3{{E-sp |13}} T·m<sup>3</sup>}},<ref name="Kivelson2002" /> which is three times larger than the [[Mercury's magnetic field|magnetic moment of Mercury]]. The magnetic dipole is tilted with respect to the rotational axis of Ganymede by 176°, which means that it is directed against the Jovian magnetic moment.<ref name="Kivelson2002" /> Its north pole lies below the [[orbital plane (astronomy)|orbital plane]]. The [[dipole|dipole magnetic field]] created by this permanent moment has a strength of 719 ± 2 [[Tesla (unit)|nT]] at Ganymede's equator,<ref name="Kivelson2002" /> which should be compared with the Jovian magnetic field at the distance of Ganymede—about 120 nT.<ref name="Kivelson1997" /> The equatorial field of Ganymede is directed against the Jovian field, meaning [[Magnetic reconnection|reconnection]] is possible. The intrinsic field strength at the poles is two times that at the equator—1440 nT.<ref name="Kivelson2002" />
[[Image:15-33i2-JupiterMoon-Ganymede-Aurora-20150312.png|thumb|right|Aurorae on Ganymede—auroral belt shifting may indicate a subsurface saline ocean.]]
The permanent magnetic moment carves a part of space around Ganymede, creating a tiny [[magnetosphere]] embedded inside [[Jupiter's magnetosphere|that of Jupiter]]; it is the only moon in the Solar System known to possess the feature.<ref name="Kivelson1997" /> Its diameter is 4–5 Ganymede radii.<ref name="Kivelson1998">{{cite journal |last1=Kivelson |first1=M.G. |last2=Warnecke |first2=J. |last3=Bennett |first3=L. |last4=Joy |first4=S. |last5=Khurana |first5=K. K. |last6=Linker |first6=J. A. |last7=Russell |first7=C. T. |last8=Walker |first8=R. J. |last9=Polanskey |first9=C. |display-authors=2 |title=Ganymede's magnetosphere: magnetometer overview |journal=J. Geophys. Res. |date=1998 |volume=103 |issue=E9 |pages=19,963–19,972 |doi=10.1029/98JE00227 |url=http://www.igpp.ucla.edu/people/mkivelson/Publications/98JE00227.pdf |bibcode=1998JGR...10319963K |doi-access=free |access-date=January 15, 2008 |archive-date=March 27, 2009 |archive-url=https://web.archive.org/web/20090327050819/http://www.igpp.ucla.edu/people/mkivelson/Publications/98JE00227.pdf |url-status=live }}</ref> The Ganymedian magnetosphere has a region of closed [[field line]]s located below 30° latitude, where [[charged particle]]s ([[electron]]s and [[ion]]s) are trapped, creating a kind of [[radiation belt]].<ref name="Kivelson1998" /> The main ion species in the magnetosphere is single ionized oxygen<ref name="Eviatar2001" /> (O<sup>+</sup>) which fits well with Ganymede's tenuous oxygen [[atmosphere]]. In the polar cap regions, at latitudes higher than 30°, magnetic field lines are open, connecting Ganymede with Jupiter's ionosphere.<ref name="Kivelson1998" /> In these areas, the energetic (tens and hundreds of [[kiloelectronvolt]]) electrons and ions have been detected,<ref name="Paranicas1999" /> which may cause the auroras observed around the Ganymedian poles.<ref name="Feldman2000" /> In addition, heavy ions precipitate continuously on Ganymede's polar surface, [[sputtering]] and darkening the ice.<ref name="Paranicas1999" />

The interaction between the Ganymedian magnetosphere and Jovian [[plasma (physics)|plasma]] is in many respects similar to that of the [[solar wind]] and Earth's magnetosphere.<ref name="Kivelson1998" /><ref name="Volwerk1999">{{cite journal |last1=Volwerk |first1=M. |last2=Kivelson |first2=M.G. |last3=Khurana |first3=K.K. |last4=McPherron |first4=R.L. |title=Probing Ganymede's magnetosphere with field line resonances |journal=J. Geophys. Res. |date=1999 |volume=104 |issue=A7 |pages=14,729–14,738 |doi=10.1029/1999JA900161 |url=http://www.igpp.ucla.edu/people/mkivelson/Publications/1999JA900161.pdf |bibcode=1999JGR...10414729V |doi-access=free |access-date=January 15, 2008 |archive-date=March 27, 2009 |archive-url=https://web.archive.org/web/20090327050807/http://www.igpp.ucla.edu/people/mkivelson/Publications/1999JA900161.pdf |url-status=live }}</ref> The plasma co-rotating with Jupiter impinges on the trailing side of the Ganymedian magnetosphere much like the solar wind impinges on the Earth's magnetosphere. The main difference is the speed of plasma flow—[[supersonic]] in the case of Earth and [[Speed of sound|subsonic]] in the case of Ganymede. Because of the subsonic flow, there is no [[bow shock]] off the trailing hemisphere of Ganymede.<ref name="Volwerk1999" />

In addition to the intrinsic magnetic moment, Ganymede has an induced dipole magnetic field.<ref name="Kivelson2002" /> Its existence is connected with the variation of the Jovian magnetic field near Ganymede. The induced moment is directed radially to or from Jupiter following the direction of the varying part of the planetary magnetic field. The induced magnetic moment is an order of magnitude weaker than the intrinsic one. The [[field strength]] of the induced field at the magnetic equator is about 60 nT—half of that of the ambient Jovian field.<ref name="Kivelson2002" /> The induced magnetic field of Ganymede is similar to those of Callisto and Europa, indicating that Ganymede also has a subsurface water ocean with a high electrical conductivity.<ref name="Kivelson2002" />

Given that Ganymede is completely differentiated and has a metallic core,<ref name="Showman1999" /><ref name="Hauk2006" /> its intrinsic magnetic field is probably generated in a similar fashion to the Earth's: as a result of conducting material moving in the interior.<ref name="Kivelson2002" /><ref name="Hauk2006" /> The magnetic field detected around Ganymede is likely to be caused by compositional convection in the core,<ref name="Hauk2006" /> if the magnetic field is the product of dynamo action, or magnetoconvection.<ref name="Kivelson2002" /><ref name="Hauck2002">{{cite journal |last1=Hauck |first1=Steven A. |last2=Dombard |first2=A. J. |last3=Solomon |first3=S. C. |last4=Aurnou |first4=J. M. |title=Internal structure and mechanism of core convection on Ganymede |journal=Lunar and Planetary Science |volume=XXXIII |date=2002 |page=1380 |url=http://www.lpi.usra.edu/meetings/lpsc2002/pdf/1380.pdf |bibcode=2002LPI....33.1380H |access-date=October 21, 2007 |archive-date=March 27, 2009 |archive-url=https://web.archive.org/web/20090327050805/http://www.lpi.usra.edu/meetings/lpsc2002/pdf/1380.pdf |url-status=live }}</ref>

Despite the presence of an iron core, Ganymede's magnetosphere remains enigmatic, particularly given that similar bodies lack the feature.<ref name="Showman1999" /> Some research has suggested that, given its relatively small size, the core ought to have sufficiently cooled to the point where fluid motions, hence a magnetic field would not be sustained. One explanation is that the same orbital resonances proposed to have disrupted the surface also allowed the magnetic field to persist: with Ganymede's eccentricity pumped and tidal heating of the mantle increased during such resonances, reducing heat flow from the core, leaving it fluid and convective.<ref name="Bland2007" /> Another explanation is a remnant magnetization of silicate rocks in the mantle, which is possible if the satellite had a more significant dynamo-generated field in the past.<ref name="Showman1999" />

===Radiation environment===
The radiation level at the surface of Ganymede is considerably lower than on Europa, being 50–80 mSv (5–8 rem) per day, an amount that would cause severe illness or death in human beings exposed for two months.<ref name= "Podzolko">{{cite conference | last1= Podzolko | first1= M.V. | last2= Getselev | first2= I.V. | title= Radiation Conditions of a Mission to Jupiterʼs Moon Ganymede | book-title= International Colloquium and Workshop "Ganymede Lander: Scientific Goals and Experiments | publisher= Moscow State University | date= March 8, 2013 | location= IKI, Moscow, Russia | url= https://forum.nasaspaceflight.com/index.php?action=dlattach;topic=32688.0;attach=541277 | access-date= January 6, 2020 | archive-date= March 9, 2021 | archive-url= https://web.archive.org/web/20210309003045/https://forum.nasaspaceflight.com/index.php?action=dlattach;topic=32688.0;attach=541277 | url-status= live }}</ref>

==Origin and evolution==
[[Image:Ganymede terrain.jpg|thumb|upright=1.15|A sharp boundary divides the ancient dark terrain of Nicholson Regio from the younger, finely striated bright terrain of Harpagia Sulcus.]]
Ganymede probably formed by an [[accretion (astrophysics)|accretion]] in Jupiter's [[solar nebula|subnebula]], a disk of gas and dust surrounding Jupiter after its formation.<ref name="Canup2002">{{cite journal |last1=Canup |first1=Robin M. |author1-link=Robin Canup |last2=Ward |first2=William R. |title=Formation of the Galilean Satellites: Conditions of Accretion |date=2002 |volume=124 |issue=6 |pages=3404–3423 |doi=10.1086/344684 |url=http://www.boulder.swri.edu/~robin/cw02final.pdf |journal=The Astronomical Journal |bibcode=2002AJ....124.3404C |s2cid=47631608 |access-date=January 2, 2008 |archive-date=October 9, 2022 |archive-url=https://ghostarchive.org/archive/20221009/http://www.boulder.swri.edu/~robin/cw02final.pdf |url-status=live }}</ref> The accretion of Ganymede probably took about 10,000 years,<ref name="Mosqueira2003">{{cite journal |last1=Mosqueira |first1=Ignacio |last2=Estrada |first2=Paul R |title=Formation of the regular satellites of giant planets in an extended gaseous nebula I: subnebula model and accretion of satellites |date=2003 |volume=163 |issue=1 |pages=198–231 |doi=10.1016/S0019-1035(03)00076-9 |bibcode=2003Icar..163..198M |journal=Icarus |url=https://zenodo.org/record/1259597 |access-date=August 25, 2019 |archive-date=December 1, 2020 |archive-url=https://web.archive.org/web/20201201233143/https://zenodo.org/record/1259597 |url-status=live }}</ref> much shorter than the 100,000 years estimated for Callisto. The Jovian subnebula may have been relatively "gas-starved" when the Galilean satellites formed; this would have allowed for the lengthy accretion times required for Callisto.<ref name="Canup2002" /> In contrast, Ganymede formed closer to Jupiter, where the subnebula was denser, which explains its shorter formation timescale.<ref name="Mosqueira2003" /> This relatively fast formation prevented the escape of accretional heat, which may have led to ice melt and [[Planetary differentiation|differentiation]]: the separation of the rocks and ice. The rocks settled to the center, forming the core.<ref name="Bhatia2017"/> In this respect, Ganymede is different from Callisto, which apparently failed to melt and differentiate early due to loss of the accretional heat during its slower formation.<ref name="McKinnon2006">{{cite journal |last=McKinnon |first=William B. |title=On convection in ice I shells of outer Solar System bodies, with detailed application to Callisto |date=2006 |volume=183 |issue=2 |pages=435–450 |doi=10.1016/j.icarus.2006.03.004 |bibcode=2006Icar..183..435M |journal=Icarus }}</ref> This hypothesis explains why the two Jovian moons look so dissimilar, despite their similar mass and composition.<ref name="Freeman2006" /><ref name="McKinnon2006" /> Alternative theories explain Ganymede's greater internal heating on the basis of tidal flexing<ref name="Showman2">{{cite journal |last1=Showman |first1=A. P. |last2=Malhotra |first2=R. |s2cid=55790129 |title=Tidal evolution into the Laplace resonance and the resurfacing of Ganymede |journal=[[Icarus (journal)|Icarus]] |volume=127 |issue=1 |pages=93–111 |date=March 1997 |doi=10.1006/icar.1996.5669 |bibcode=1997Icar..127...93S }}</ref> or more intense pummeling by impactors during the [[Late Heavy Bombardment]].<ref name="Baldwin">{{cite web |last=Baldwin |first=E. |title=Comet impacts explain Ganymede-Callisto dichotomy |work=[[Astronomy Now]] |date=January 25, 2010 |url=http://www.astronomynow.com/news/n1001/25galilean/ |access-date=March 1, 2010 |archive-date=January 30, 2010 |archive-url=https://web.archive.org/web/20100130231918/http://www.astronomynow.com/news/n1001/25galilean/ |url-status=dead }}</ref><ref name = "Phys.Org2010">{{cite web | url = https://phys.org/news/2010-01-explanation-differences-ganymede-callisto-moons.html | title = Researchers offer explanation for the differences between Ganymede and Callisto moons | date = January 24, 2010 | website = Phys.Org | access-date = February 3, 2017 | archive-date = February 3, 2017 | archive-url = https://web.archive.org/web/20170203163742/https://phys.org/news/2010-01-explanation-differences-ganymede-callisto-moons.html | url-status = live }}</ref><ref name="LPI1158">{{cite conference |first1=A. C. |last1=Barr |last2=Canup |first2=R. M. |title=Origin of the Ganymede/Callisto dichotomy by impacts during an outer solar system late heavy bombardment |work=41st Lunar and Planetary Science Conference (2010) |date=March 2010 |location=Houston |url=http://www.lpi.usra.edu/meetings/lpsc2010/pdf/1158.pdf |access-date=March 1, 2010 |archive-date=June 5, 2011 |archive-url=https://web.archive.org/web/20110605044843/http://www.lpi.usra.edu/meetings/lpsc2010/pdf/1158.pdf |url-status=live }}</ref><ref name="Barr3">{{cite journal |last1=Barr |first1=A. C. |last2=Canup |first2=R. M. |title=Origin of the Ganymede–Callisto dichotomy by impacts during the late heavy bombardment |journal=[[Nature Geoscience]] |volume=3 |issue=March 2010 |pages=164–167 |date=January 24, 2010 |doi=10.1038/NGEO746 |bibcode=2010NatGe...3..164B |url=http://www.planetary.brown.edu/pdfs/ab19.pdf |citeseerx=10.1.1.827.982 |access-date=April 12, 2020 |archive-date=March 1, 2021 |archive-url=https://web.archive.org/web/20210301065853/http://www.planetary.brown.edu/pdfs/ab19.pdf |url-status=dead }}</ref> In the latter case, modeling suggests that differentiation would become a [[thermal runaway|runaway process]] at Ganymede but not Callisto.<ref name="LPI1158" /><ref name="Barr3" />

After formation, Ganymede's core largely retained the heat accumulated during accretion and differentiation, only slowly releasing it to the ice mantle.<ref name="McKinnon2006" /> The mantle, in turn, transported it to the surface by convection.<ref name="Freeman2006" /> The decay of [[radioactivity|radioactive elements]] within rocks further heated the core, causing increased differentiation: an inner, iron–iron-sulfide core and a silicate mantle formed.<ref name="Hauk2006" /><ref name="McKinnon2006" /> With this, Ganymede became a fully differentiated body.<ref name="Bhatia2017" /> By comparison, the radioactive heating of undifferentiated Callisto caused convection in its icy interior, which effectively cooled it and prevented large-scale melting of ice and rapid differentiation.<ref name="Nagel2004">{{cite journal |last1=Nagel |first1=K.A |last2=Breuer |first2=D. |last3=Spohn |first3=T. |title=A model for the interior structure, evolution, and differentiation of Callisto |date=2004 |volume=169 |issue=2 |pages=402–412 |doi=10.1016/j.icarus.2003.12.019 |bibcode=2004Icar..169..402N |journal=Icarus }}</ref> The convective motions in Callisto have caused only a partial separation of rock and ice.<ref name="Nagel2004" /> Today, Ganymede continues to cool slowly.<ref name="Hauk2006" /> The heat being released from its core and silicate mantle enables the subsurface ocean to exist,<ref name="Spohn2003">{{cite journal|last1=Spohn |first1=T. |last2=Schubert |first2=G. |title=Oceans in the icy Galilean satellites of Jupiter? |journal=Icarus |date=2003 |volume=161 |issue=2 |pages=456–467 |doi=10.1016/S0019-1035(02)00048-9 |url=http://lasp.colorado.edu/icymoons/europaclass/Spohn_Schubert_oceans.pdf |bibcode=2003Icar..161..456S |url-status=dead |archive-url=https://web.archive.org/web/20080227015925/http://lasp.colorado.edu/icymoons/europaclass/Spohn_Schubert_oceans.pdf |archive-date=February 27, 2008 }}</ref>  whereas the slow cooling of the liquid Fe–FeS core causes convection and supports magnetic field generation.<ref name="Hauk2006" /> The current [[heat flux]] out of Ganymede is probably higher than that out of Callisto.<ref name="McKinnon2006" />

A study from 2020 by Hirata, Suetsugu and Ohtsuki suggests that Ganymede probably was hit by a massive asteroid 4 billion years ago; an impact so violent that may have shifted the moon's axis. The study came to this conclusion analyzing images of the furrows system in the satellite's surface.<ref>{{cite journal | url=https://www.sciencedirect.com/science/article/abs/pii/S0019103520303158 | title='Naoyuki Hirata, Ryo Suetsugu, Keiji Ohtsuki, A global system of furrows on Ganymede indicative of their creation in a single impact event, Icarus, Volume 352, 2020, 113941,ISSN 0019-1035' | journal=Icarus | date=December 2020 | volume=352 | doi=10.1016/j.icarus.2020.113941 | last1=Hirata | first1=Naoyuki | last2=Suetsugu | first2=Ryo | last3=Ohtsuki | first3=Keiji | hdl=20.500.14094/90007458 | arxiv=2205.05221 }}</ref>

==Exploration==
<!-- summary of this section -->
Several spacecraft have performed close [[flyby (spaceflight)|flyby]]s of Ganymede: two ''Pioneer'' and two ''Voyager'' spacecraft made a single flyby each between 1973 and 1979; the ''Galileo'' spacecraft made six passes between 1996 and 2000; and the [[Juno (spacecraft)|''Juno'']] spacecraft performed two flybys in 2019 and 2021.<ref name="NYT-20210608">{{cite news |last=Chang |first=Kenneth |title=NASA Just Visited the Solar System's Biggest Moon – The Juno spacecraft completed a close flyby of Ganymede, Jupiter's biggest moon, as it transitions into a new phase of its mission. |url=https://www.nytimes.com/2021/06/08/science/nasa-juno-jupiter-ganymede.html |archive-url=https://ghostarchive.org/archive/20211228/https://www.nytimes.com/2021/06/08/science/nasa-juno-jupiter-ganymede.html |archive-date=December 28, 2021 |url-access=limited |date=June 8, 2021 |work=[[The New York Times]] |access-date=June 10, 2021 }}{{cbignore}}</ref> No spacecraft has yet orbited Ganymede, but the [[Jupiter Icy Moons Explorer|JUICE]] mission, which launched in April 2023, intends to do so.

===Completed flybys===
[[File:Ganymede from Pioneer 10 19.jpg|thumb|Ganymede from ''[[Pioneer 10]]'' (1973)]]
The first spacecraft to approach close to Ganymede was ''[[Pioneer 10]]'', which performed a flyby in 1973 as it passed through the Jupiter system at high speed. ''[[Pioneer 11]]'' made a similar flyby in 1974.<ref name="Pioneer 11">{{cite web|url=http://sse.jpl.nasa.gov/missions/profile.cfm?Sort=Advanced&MCode=Pioneer_11 |title=Pioneer 11 |work=Solar System Exploration |access-date=January 6, 2008 |url-status=dead |archive-url=https://web.archive.org/web/20110902202131/http://sse.jpl.nasa.gov/missions/profile.cfm?Sort=Advanced&MCode=Pioneer_11 |archive-date=September 2, 2011 }}</ref> Data sent back by the two spacecraft was used to determine the moon's physical characteristics<ref name="Terraformers">{{cite web |url=http://society.terraformers.ca/content/view/63/112/ |archive-url=https://web.archive.org/web/20070319083334/http://society.terraformers.ca/content/view/63/112/ |archive-date=March 19, 2007 |title=Exploration of Ganymede |work=Terraformers Society of Canada |access-date=January 6, 2008 }}</ref> and provided images of the surface with up to {{convert|400|km|mi|abbr=on}} resolution.<ref name="chap6">{{cite web |url=https://history.nasa.gov/SP-349/ch6.htm |work=SP-349/396 Pioneer Odyssey |title=Chapter 6: Results at the New Frontiers |publisher=NASA |date=August 1974 |access-date=July 12, 2017 |archive-date=July 14, 2019 |archive-url=https://web.archive.org/web/20190714121940/https://history.nasa.gov/SP-349/ch6.htm |url-status=live }}</ref> Pioneer 10's closest approach was 446,250&nbsp;km, about 85 times Ganymede's diameter.<ref name="dmu.p10">{{cite web |url=http://www.dmuller.net/spaceflight/mission.php?mission=pioneer10&appear=black&showimg=yes |title=Pioneer 10 Full Mission Timeline |publisher=D Muller |access-date=May 25, 2011 |archive-url=https://web.archive.org/web/20110723095322/http://www.dmuller.net/spaceflight/mission.php?mission=pioneer10&appear=black&showimg=yes |archive-date=July 23, 2011 |url-status=dead }}</ref>

''[[Voyager 1]]'' and ''[[Voyager 2]]'' both studied Ganymede when passing through the Jupiter system in 1979. Data from those flybys were used to refine the size of Ganymede, revealing it was larger than [[Saturn]]'s moon Titan, which was previously thought to have been bigger.<ref name="Voyager">{{cite web|url=http://library.thinkquest.org/J0112188/voyager_1_and_2.htm |title=Voyager 1 and 2 |work=ThinkQuest |access-date=January 6, 2008 |url-status=dead |archive-url=https://web.archive.org/web/20071226052127/http://library.thinkquest.org/J0112188/voyager_1_and_2.htm |archive-date=December 26, 2007 }}</ref> Images from the ''Voyagers'' provided the first views of the moon's grooved surface terrain.<ref name="Voyager Mission">{{cite web |url=http://www.solarviews.com/eng/vgrfs.htm |title=The Voyager Planetary Mission |work=Views of the Solar System |access-date=January 6, 2008 |archive-url=https://web.archive.org/web/20080203032714/http://www.solarviews.com/eng/vgrfs.htm |archive-date=February 3, 2008 |url-status=dead }}</ref>

The ''Pioneer'' and ''Voyager'' flybys were all at large distances and high speeds, as they flew on [[hyperbolic orbit|unbound trajectories]] through the Jupiter system. Better data can be obtained from a spacecraft which is orbiting Jupiter, as it can encounter Ganymede at a lower speed and adjust the orbit for a closer approach. In 1995, the ''[[Galileo (spacecraft)|Galileo]]'' spacecraft entered orbit around Jupiter and between 1996 and 2000 made six close flybys of Ganymede.<ref name="The Grand Tour" /> These flybys were denoted G1, G2, G7, G8, G28 and G29.<ref name="Kivelson2002" /> During the closest flyby (G2), ''Galileo'' passed just 264&nbsp;km from the surface of Ganymede (five percent of the moon's diameter),<ref name="Kivelson2002" /> which remains the closest approach by any spacecraft. During the G1 flyby in 1996, ''Galileo'' instruments detected Ganymede's magnetic field.<ref name="Magnetic Field Discovery">{{cite web |url=http://www2.jpl.nasa.gov/galileo/status961212.html |archive-url=https://web.archive.org/web/19970105134408/http://www.jpl.nasa.gov/galileo/status961212.html |url-status=dead |archive-date=January 5, 1997 |title=New Discoveries From Galileo |work=Jet Propulsion Laboratory |access-date=January 6, 2008 }}</ref> Data from the ''Galileo'' flybys was used to discover the sub-surface ocean, which was announced in 2001.<ref name="Kivelson2002" /><ref name="The Grand Tour" /> High spatial resolution spectra of Ganymede taken by ''Galileo'' were used to identify several non-ice compounds on the surface.<ref name="McCord1998" />

The ''[[New Horizons]]'' spacecraft also observed Ganymede, but from a much larger distance as it passed through the Jupiter system in 2007 (en route to [[Pluto]]). The data were used to perform topographic and compositional mapping of Ganymede.<ref name="New Horizons">{{cite web |url=http://www.spacedaily.com/reports/Pluto_Bound_New_Horizons_Spacecraft_Gets_A_Boost_From_Jupiter_999.html |title=Pluto-Bound New Horizons Spacecraft Gets A Boost From Jupiter |work=Space Daily |access-date=January 6, 2008 |archive-date=March 23, 2019 |archive-url=https://web.archive.org/web/20190323054132/http://www.spacedaily.com/reports/Pluto_Bound_New_Horizons_Spacecraft_Gets_A_Boost_From_Jupiter_999.html |url-status=live }}</ref><ref name="Grundy2007">{{cite journal |last1=Grundy |first1=W.M. |last2=Buratti |first2=B.J. |last3=Cheng |first3=A.F. |last4=Emery |first4=J. P. |last5=Lunsford |first5=A. |last6=McKinnon |first6=W. B. |last7=Moore |first7=J. M. |last8=Newman |first8=S. F. |last9=Olkin |first9=C. B. |display-authors=2 |title=New Horizons Mapping of Europa and Ganymede |journal=Science |date=2007 |volume=318 |pages=234–237 |doi=10.1126/science.1147623 |bibcode=2007Sci...318..234G |pmid=17932288 |issue=5848 |s2cid=21071030 }}</ref>

Like ''Galileo'', the ''[[Juno (spacecraft)|Juno]]'' spacecraft orbited Jupiter. On 2019 December 25, ''Juno'' performed a distant flyby of Ganymede during its 24th orbit of Jupiter, at a range of {{convert|97680|to|109439|km|mi|sp=us}}. This flyby provided images of the moon's polar regions.<ref name="Juno">{{cite web |url=https://www.missionjuno.swri.edu/news/Ganymede |publisher=Southwest Research Institute |title=Ganymede |date=January 9, 2020 |access-date=January 10, 2020 |archive-date=February 15, 2020 |archive-url=https://web.archive.org/web/20200215020827/https://www.missionjuno.swri.edu/news/Ganymede |url-status=live }}</ref><ref name="Inaf">{{Cite web|last=Inaf|first=Ufficio stampa|date=August 6, 2021|title=Gli occhi di Jiram sull'equatore di Ganimede|url=https://www.media.inaf.it/2021/08/06/jiram-equatore-ganimede/|access-date=December 8, 2021|website=MEDIA INAF|language=it-IT|archive-date=December 8, 2021|archive-url=https://web.archive.org/web/20211208140147/https://www.media.inaf.it/2021/08/06/jiram-equatore-ganimede/|url-status=live}}</ref> In June 2021, ''Juno'' performed a second flyby, at a closer distance of {{convert|1038|km|mi|sp=us}}.<ref name="NYT-20210608" /><ref>{{cite news |title=Nasa spacecraft captures first closeups of Jupiter's largest moon in decades |url=https://www.theguardian.com/science/2021/jun/08/juno-nasa-jupiter-moon-ganymede |access-date=June 9, 2021 |work=The Guardian |agency=Associated Press |date=June 8, 2021 |language=en |archive-date=June 9, 2021 |archive-url=https://archive.today/20210609043534/https://www.theguardian.com/science/2021/jun/08/juno-nasa-jupiter-moon-ganymede |url-status=live }}</ref> This encounter was designed to provide a [[gravity assist]] to reduce ''Juno'''s orbital period from 53 days to 43 days. Additional images of the surface were collected.<ref name="NYT-20210608" />

===Future missions===
The [[Jupiter Icy Moons Explorer]] (JUICE) will be the first to enter orbit around Ganymede itself. JUICE was launched on April 14, 2023.<ref name="esa-20221202">{{cite web |url=https://www.esa.int/Newsroom/Press_Releases/ESA_highlights_in_2023 |title=ESA highlights in 2023 |work=[[ESA]] |date=December 2, 2022 |access-date=January 22, 2023 |archive-date=December 4, 2022 |archive-url=https://web.archive.org/web/20221204060807/https://www.esa.int/Newsroom/Press_Releases/ESA_highlights_in_2023 |url-status=live }}</ref> It is intended to perform its first flyby of Ganymede in 2031, then enter orbit of the moon in 2032. When the spacecraft consumes its propellant, JUICE is planned to be deorbited and impact Ganymede in February 2034.<ref>{{Cite web|author1=Elizabeth Howell|date=February 14, 2017|title=JUICE: Exploring Jupiter's Moons|url=https://www.space.com/35692-esa-juice-facts.html|access-date=February 3, 2022|website=Space.com|language=en|archive-date=May 26, 2020|archive-url=https://web.archive.org/web/20200526081142/https://www.space.com/35692-esa-juice-facts.html|url-status=live}}</ref>

In addition to JUICE, NASA's [[Europa Clipper]], which was launched in October 2024, will conduct 4 close flybys of Ganymede beginning in 2030.<ref>[https://arc.aiaa.org/doi/10.2514/1.G004309 Tour Design Techniques for the Europa Clipper Mission] – Campagnola et al. (2019)</ref> It may also crash into Ganymede at the end of its mission to aid JUICE in studying the surface's geochemistry.<ref name="LPI OPAG 2022">{{cite web | title=14 OPAG June 2022 Day 2 Bob Pappalardo Jordan Evans (unlisted) | website=YouTube | date=July 19, 2022 | url=https://www.youtube.com/watch?v=eKD6fuWUIlw&t=624 | access-date=April 15, 2024}}</ref><ref name="Waldek 2022">{{cite web | last=Waldek | first=Stefanie | title=NASA's Europa Clipper may crash into Ganymede, the largest moon in the solar system, at mission's end | website=Space.com | date=June 29, 2022 | url=https://www.space.com/europa-clipper-might-crash-into-ganymede | access-date=April 15, 2024}}</ref>

===Cancelled proposals===
Several other missions have been proposed to flyby or orbit Ganymede, but were either not selected for funding or cancelled before launch.

The [[Jupiter Icy Moons Orbiter]] would have studied Ganymede in greater detail.<ref name="JIMO">{{cite encyclopedia |url=http://www.daviddarling.info/encyclopedia/J/JIMO.html |title=Jupiter Icy Moons Orbiter (JIMO) |encyclopedia=The Internet Encyclopedia of Science |access-date=January 6, 2008 |archive-date=February 11, 2008 |archive-url=https://web.archive.org/web/20080211223140/http://www.daviddarling.info/encyclopedia/J/JIMO.html |url-status=live }}</ref> However, the mission was canceled in 2005.<ref name="n.050207">{{cite journal |last=Peplow |first=M. |url=http://www.nature.com/news/2005/050208/full/news050207-4.html |title=NASA budget kills Hubble telescope |journal=Nature |date=February 8, 2005 |doi=10.1038/news050207-4 |access-date=December 24, 2011 |doi-access=free |archive-date=July 2, 2010 |archive-url=https://web.archive.org/web/20100702062759/http://www.nature.com/news/2005/050208/full/news050207-4.html |url-status=live }}</ref> Another old proposal was called The Grandeur of Ganymede.<ref name="Pappalardo2001" />

A Ganymede orbiter based on the ''Juno'' probe was proposed in 2010 for the [[Planetary Science Decadal Survey]].<ref name="ssb">{{cite web |url=http://sites.nationalacademies.org/ssb/SSB_059331.htm |publisher=Space Studies Board |title=Planetary Science Decadal Survey Mission & Technology Studies |access-date=November 12, 2012 |archive-date=April 28, 2014 |archive-url=https://web.archive.org/web/20140428233143/http://sites.nationalacademies.org/ssb/SSB_059331.htm |url-status=dead }} {{cite web |url=http://sites.nationalacademies.org/cs/groups/ssbsite/documents/webpage/ssb_059315.pdf |title=Ganymede Orbiter |access-date=September 19, 2015 |archive-date=September 29, 2015 |archive-url=https://web.archive.org/web/20150929144405/http://sites.nationalacademies.org/cs/groups/ssbsite/documents/webpage/ssb_059315.pdf |url-status=live }}</ref> The mission was not supported, with the Decadal Survey preferring the [[Europa Clipper]] mission instead.<ref>{{cite book |author1=National Research Council |title=Vision and Voyages for Planetary Science in the Decade 2013–2022 |date=March 7, 2011 |publisher=The National Academies Press |location=Washington DC, US |isbn=978-0-309-22464-2 |url=https://www.nap.edu/catalog/13117/vision-and-voyages-for-planetary-science-in-the-decade-2013-2022 |doi=10.17226/13117 |url-access=registration |quote=The committee identified a number of additional large missions that are of high scientific value but are not recommended for the decade 2013-2022 for a variety of reasons. In alphabetical order, these missions are as follows: Ganymede Orbiter [...] |access-date=June 18, 2021 |archive-date=February 11, 2021 |archive-url=https://web.archive.org/web/20210211083518/https://www.nap.edu/catalog/13117/vision-and-voyages-for-planetary-science-in-the-decade-2013-2022 |url-status=live }}</ref>

The [[Europa Jupiter System Mission]] had a proposed launch date of 2020, and was a joint NASA and ESA proposal for exploration of many of Jupiter's moons including Ganymede. In February 2009 it was announced that ESA and NASA had given this mission priority ahead of the [[Titan Saturn System Mission]].<ref name="bbc.7897585">{{cite news |url=http://news.bbc.co.uk/1/hi/sci/tech/7897585.stm |title=Jupiter in space agencies' sights |first=Paul |last=Rincon |work=BBC News |date=February 20, 2009 |access-date=February 20, 2009 |archive-date=February 21, 2009 |archive-url=https://web.archive.org/web/20090221185643/http://news.bbc.co.uk/1/hi/sci/tech/7897585.stm |url-status=live }}</ref> The mission was to consist of the NASA-led [[Jupiter Europa Orbiter]], the ESA-led [[Jupiter Ganymede Orbiter]], and possibly a [[JAXA]]-led [[Jupiter Magnetospheric Orbiter]]. The NASA and JAXA components were later cancelled, and ESA's appeared likely to be cancelled too,<ref name="esa.41177">{{cite web |url=http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=41177 |title=Cosmic Vision 2015–2025 Proposals |date=July 21, 2007 |publisher=ESA |access-date=February 20, 2009 |archive-date=September 2, 2011 |archive-url=https://web.archive.org/web/20110902033453/http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=41177 |url-status=live }}</ref> but in 2012 ESA announced it would go ahead alone. The European part of the mission became the Jupiter Icy Moon Explorer (JUICE).<ref name="juiceL1">{{cite web |url=http://planetary.s3.amazonaws.com/assets/resources/ESA/ESA-SPC_20120417_selection-L1-mission.pdf |title=ESA – Selection of the L1 mission |date=April 17, 2012 |publisher=[[ESA]] |access-date=April 15, 2014 |archive-date=October 16, 2015 |archive-url=https://web.archive.org/web/20151016065456/http://planetary.s3.amazonaws.com/assets/resources/ESA/ESA-SPC_20120417_selection-L1-mission.pdf |url-status=live }}</ref>

The [[Russian Space Research Institute]] proposed a Ganymede lander [[astrobiology]] mission called [[Laplace-P]],<ref name="Lander workshop">{{cite web |url=http://glcw2013.cosmos.ru/ |title=International Colloquium and Workshop – "Ganymede Lander: scientific goals and experiments" |date=November 2012 |work=Russia Space Research Institute (IKI) |publisher=Roscosmos |access-date=November 20, 2012 |archive-date=November 23, 2018 |archive-url=https://web.archive.org/web/20181123154309/http://glcw2013.cosmos.ru/ |url-status=live }}</ref> possibly in partnership with JUICE.<ref name="Lander workshop" /><ref name="bbc.20407902">{{cite news |url=https://www.bbc.co.uk/news/science-environment-20407902 |title=Russia and Europe joint Mars bid agreement approved |first=Jonathan |last=Amos |work=BBC News |date=November 20, 2012 |access-date=June 20, 2018 |archive-date=December 2, 2018 |archive-url=https://web.archive.org/web/20181202232039/https://www.bbc.co.uk/news/science-environment-20407902 |url-status=live }}</ref> If selected, it would have been launched in 2023. The mission was cancelled due to a lack of funding in 2017.<ref name=":1">{{Cite news |last=Струговец |first=Дмитрий |date=July 15, 2017 |title=Вице-президент РАН: сроки реализации лунной программы сдвинулись ради проекта "ЭкзоМарс" |work=TASS |url=https://tass.ru/opinions/interviews/4411146 |url-status=dead |archive-url=https://web.archive.org/web/20180705091658/https://tass.ru/opinions/interviews/4411146 |archive-date=July 5, 2018}}</ref>

== See also ==
{{div col|colwidth=20em}}
* [[Cold trap (astronomy)]]
* [[Moons of Jupiter]]
* [[Galilean moons]] (the four biggest moons of Jupiter)
* [[Jupiter's moons in fiction]]
* [[List of craters on Ganymede]]
* [[List of geological features on Ganymede]]
* [[List of natural satellites]]
* [[Lunar and Planetary Institute]]
{{div col end}}

== Notes ==
{{Reflist|group=lower-alpha|refs=<ref name="surfacedensitynumber">The surface number density and pressure were calculated from the column densities reported in Hall, et al. 1998, assuming a [[scale height]] of 20&nbsp;km and temperature 120 K.</ref><ref name="periapsiscomment">Periapsis is derived from the semimajor axis (''a'') and eccentricity (''e''): <math>a\cdot(1-e)</math>.</ref><ref name="apoapsiscomment">Apoapsis is derived from the semimajor axis (''a'') and eccentricity (''e''): <math>a\cdot(1+e)</math>.</ref><ref name="surfaceareacomment">Surface area derived from the radius (''r''): <math>4\pi r^2</math>.</ref><ref name="volumecomment">Volume derived from the radius (''r''): <math>4\pi r^3/3</math>.</ref><ref name="surfacegravitycomment">Surface gravity derived from the mass (''m''), the [[gravitational constant]] (''G'') and the radius (''r''): <math>Gm/r^2</math>.</ref><ref name="escapevelocitycomment">Escape velocity derived from the mass (''m''), the [[gravitational constant]] (''G'') and the radius (''r''): <math>\textstyle\sqrt{2Gm/r}</math>.</ref><ref name="hemispherecomment">The leading hemisphere is the hemisphere facing the direction of orbital motion; the trailing hemisphere faces the reverse direction.</ref><ref name="laplaceres">A Laplace-like resonance is similar to the current Laplace resonance among the Galilean moons with the only difference being that longitudes of the Io–Europa and Europa–Ganymede conjunctions change with rates whose ratio is a non-unity rational number. If the ratio is unity, then the resonance is the Laplace resonance.</ref>
}}

==References==
{{Reflist}}

== Further reading ==
* {{cite conference |url=http://www.lpi.usra.edu/opag/Oct2011/presentations/Dougherty.pdf |last1=Dougherty |last2=Grasset |title=Jupiter Icy Moon Explorer |date=2011 }}
* {{cite web|title=Jupiter's Great Red Spot and Ganymede's shadow|url=http://www.spacetelescope.org/images/opo1431a/|website=www.spacetelescope.org|publisher=ESA/Hubble|access-date=October 31, 2014|archive-date=August 24, 2019|archive-url=https://web.archive.org/web/20190824191023/https://www.spacetelescope.org/images/opo1431a/|url-status=dead}}

==External links==
{{Commons category|Ganymede (moon)}}
* [https://web.archive.org/web/20180728113750/https://solarsystem.nasa.gov/moons/jupiter-moons/ganymede/in-depth/ Ganymede page] at [http://solarsystem.nasa.gov/ NASA's Solar System Exploration site]
* [http://www.nineplanets.org/ganymede.html Ganymede page] at ''The Nine Planets''
* [http://www.solarviews.com/eng/ganymede.htm Ganymede page] at ''Views of the Solar System''
* [http://www.lpi.usra.edu/resources/gc/gchome.shtml Ganymede Crater Database] from the Lunar and Planetary Institute
* [http://photojournal.jpl.nasa.gov/target/Ganymede Images of Ganymede at JPL's Planetary Photojournal]
* Movie of [https://www.youtube.com/watch?v=r8LlKoRMgaY Ganymede's rotation] from the National Oceanic and Atmospheric Administration
* [http://www.scientificamerican.com/media/inline/blog/Image/ganymede_map.jpg Ganymede map] from [http://www.scientificamerican.com/article.cfm?id=ganymede-new-map ''Scientific American'' article]
* [http://photojournal.jpl.nasa.gov/catalog/?IDNumber=PIA03781 Ganymede map with feature names] from [http://photojournal.jpl.nasa.gov/ Planetary Photojournal]
* [http://planetarynames.wr.usgs.gov/Page/GANYMEDE/target Ganymede nomenclature] and [http://planetarynames.wr.usgs.gov/images/gany_15ppi.pdf Ganymede map with feature names] from the [http://planetarynames.wr.usgs.gov USGS planetary nomenclature page]
* [http://stereomoons.blogspot.com/2009/10/galileo-4-moons-at-400-years.html Paul Schenk's 3D images and flyover videos of Ganymede and other outer solar system satellites]
* [http://sites.nationalacademies.org/SSB/xpedio/groups/ssbsite/documents/webpage/SSB_059315.pdf Ganymede Orbiter Concept]
* [http://pubs.usgs.gov/sim/3237/ Global Geologic Map of Ganymede] (USGS)
* [https://www.google.com/maps/space/ganymede/@-1.551038,-164.6549184,6869088m/data=!3m1!1e3 Google Ganymede 3D], interactive map of the moon
* [https://www.youtube.com/watch?v=Dv8UwzSOxmA Video (animation; 4:00): Flyby of Ganymede and Jupiter] ([[NASA]]; July 15, 2021).

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{{Moons of Jupiter}}
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[[Category:Astronomical objects discovered in 1610|16100107]]
[[Category:Discoveries by Galileo Galilei]]
[[Category:Ganymede (moon)| ]]
[[Category:Moons of Jupiter]]
[[Category:Moons with a prograde orbit]]