Editing Cygnus (constellation) (section)

=== Stars ===
{{See also|List of stars in Cygnus}}
[[File:CygnusCC.jpg|thumb|left|upright|The constellation Cygnus as it can be seen by the naked eye, with the [[Northern Cross (asterism)|Northern Cross]] in the middle.]]
Bayer catalogued many stars in the constellation, giving them the [[Bayer designation]]s from Alpha to Omega and then using lowercase Roman letters to g. [[John Flamsteed]] added the Roman letters h, i, k, l and m (these stars were considered ''informes'' by Bayer as they lay outside the asterism of Cygnus), but were dropped by [[Francis Baily]].<ref name=wagman /><!-- cites previous two sentences -->

[[File:A young star takes centre stage.jpg|thumb|[[V1331 Cygni]] is located in the dark cloud LDN 981.<ref>{{cite news |title=A young star takes centre stage |url=http://www.spacetelescope.org/images/potw1509a/ |access-date=3 March 2015 |work=ESA/Hubble Picture of the Week |agency=ESA/Hubble}}</ref>]]

There are several bright stars in Cygnus. α Cygni, called [[Deneb]], is the brightest star in Cygnus. It is a white [[supergiant]] star of spectral type A2Iae that varies between magnitudes 1.21 and 1.29,<ref name=AAVSOalf>{{cite web |url=http://www.aavso.org/vsx/index.php?view=detail.top&oid=13281 |title=Alpha Cygni |last=BSJ |date=4 January 2010 |website=AAVSO Website |publisher=American Association of Variable Star Observers |access-date=22 December 2013}}</ref> one of the largest and most luminous A-class stars known.<ref name="illinois-deneb">{{cite web |url=http://stars.astro.illinois.edu/sow/deneb.html |title=Deneb |author=Jim Kaler |date=26 June 2009 |website=Stars |access-date=15 January 2013}}</ref> It is located about 2600 light-years away.<ref name="earthsky">{{cite web |url=http://earthsky.org/brightest-stars/deneb-among-the-farthest-stars-to-be-seen |title=Deneb: A distant and very luminous star |author=Larry Sessions |date=2018-05-23 |website=Earth Sky |access-date=2020-01-31}}</ref> Its traditional name means "tail" and refers to its position in the constellation. [[Albireo]], designated β Cygni, is a celebrated [[binary star]] among amateur astronomers for its contrasting hues. The primary is an orange-hued giant star of magnitude 3.1 and the secondary is a blue-green hued star of magnitude 5.1.<ref name=drimmel2021>{{cite journal |bibcode=2021MNRAS.502..328D |title=A celestial matryoshka: Dynamical and spectroscopic analysis of the Albireo system |last1=Drimmel |first1=Ronald |last2=Sozzetti |first2=Alessandro |last3=Schröder |first3=Klaus-Peter |last4=Bastian |first4=Ulrich |last5=Pinamonti |first5=Matteo |last6=Jack |first6=Dennis |last7=Hernández Huerta |first7=Missael A. |journal=Monthly Notices of the Royal Astronomical Society |year=2021 |volume=502 |issue=1 |page=328 |doi=10.1093/mnras/staa4038 |doi-access=free |arxiv=2012.01277 }}</ref> The system is 430 light-years away and is visible in large binoculars and all amateur telescopes.<ref name="illinois-albireo">{{cite web |url=http://stars.astro.illinois.edu/sow/albireo.html |title=Albireo |author=Jim Kaler |website=Stars |access-date=15 January 2013}}</ref> [[Gamma Cygni|γ Cygni]], traditionally named Sadr, is a yellow-tinged supergiant star of magnitude 2.2, 1800 light-years away. Its traditional name means "breast" and refers to its position in the constellation.<ref name="illinois-sadr">{{cite web |url=http://stars.astro.illinois.edu/sow/sadr.html |title=Sadr |author=Jim Kaler |date=30 November 2012 |website=Stars |access-date=15 January 2013}}</ref> [[Delta Cygni|δ Cygni]] (the proper name is Fawaris<ref name="IAU-LSN">{{cite web |url=https://www.iau.org/public/themes/naming_stars/ |title=Naming Stars |publisher=[[International Astronomical Union|IAU]] |access-date=30 July 2018}}</ref>) is another bright binary star in Cygnus, 166 light-years with a period of 800 years. The primary is a blue-white hued giant star of magnitude 2.9, and the secondary is a star of magnitude 6.6. The two components are visible in a medium-sized amateur telescope.<ref name="illinois-deltacygni">{{cite web |url=http://stars.astro.illinois.edu/sow/deltacyg.html |title=DELTA CYG |author=Jim Kaler |website=Stars |access-date=15 January 2013}}</ref> The fifth star in Cygnus above magnitude 3 is Aljanah,<ref name="IAU-LSN"/> designated [[Epsilon Cygni|ε Cygni]]. It is an orange-hued giant star of magnitude 2.5, 72 light-years from Earth.<ref name="illinois-gienah">{{cite web |url=http://stars.astro.illinois.edu/sow/gienahcyg.html |title=Gienah Cygni |author=Jim Kaler |website=Stars |access-date=15 January 2013}}</ref>{{sfn|Ridpath|Tirion|2001|pp=134–37}}

There are several other dimmer double and binary stars in Cygnus. [[Mu Cygni|μ Cygni]] is a binary star with an optical tertiary component. The binary system has a period of 790 years and is 73 light-years from Earth. The primary and secondary, both white stars, are of magnitude 4.8 and 6.2, respectively. The unrelated tertiary component is of magnitude 6.9. Though the tertiary component is visible in binoculars, the primary and secondary currently require a medium-sized amateur telescope to split, as they will through the year 2020. The two stars will be closest between 2043 and 2050, when they will require a telescope with larger aperture to split. The stars [[30 Cygni|30]] and [[31 Cygni]] form a contrasting double star similar to the brighter Albireo. The two are visible in binoculars. The primary, 31 Cygni, is an orange-hued star of magnitude 3.8, 1400 light-years from Earth. The secondary, 30 Cygni, appears blue-green. It is of spectral type A5IIIn and magnitude 4.83, and is around 610 light-years from Earth.<ref>{{cite web |url=http://simbak.cfa.harvard.edu/simbad/sim-basic?Ident=30+Cygni&submit=SIMBAD+search|archive-url = https://archive.today/20121214195939/http://simbak.cfa.harvard.edu/simbad/sim-basic?Ident=30+Cygni&submit=SIMBAD+search|url-status = dead|archive-date = 14 December 2012 |title=30 Cygni – Variable Star |website=SIMBAD Astronomical Database |publisher=Centre de Données astronomiques de Strasbourg |access-date=31 December 2013}}</ref> 31 Cygni itself is a binary star; the tertiary component is a blue star of magnitude 7.0. [[Psi Cygni|ψ Cygni]] is a binary star visible in small amateur telescopes, with two white components. The primary is of magnitude 5.0 and the secondary is of magnitude 7.5. [[61 Cygni]] is a binary star visible in large binoculars or a small amateur telescope. It is 11.4 light-years from Earth and has a period of 750 years. Both components are orange-hued dwarf ([[main sequence]]) stars; the primary is of magnitude 5.2 and the secondary is of magnitude 6.1. 61 Cygni is significant because [[Friedrich Wilhelm Bessel]] determined its [[parallax]] in 1838, the first star to have a known parallax.<ref>{{Cite journal| doi = 10.1093/mnras/4.17.152| last = Bessel | first = F. W. | author-link = Friedrich Bessel| title = On the parallax of 61 Cygni| journal = Monthly Notices of the Royal Astronomical Society| volume = 4| issue = 17| pages = 152–161| year = 1838| bibcode = 1838MNRAS...4..152B| doi-access = free}}</ref><ref>{{Cite journal | last = Bessel | first = F. W. | author-link = Friedrich Bessel| doi = 10.1002/asna.18390160502 | title = Bestimmung der Entfernung des 61sten Sterns des Schwans | language = de| trans-title = Determination of the distance to 61 Cygni| journal = Astronomische Nachrichten | volume = 16 | issue = 365–366 | pages = 65–96 | year = 1838 |bibcode = 1838AN.....16...65B| url = https://zenodo.org/record/1424605 }}</ref>

Located near [[Eta Cygni|η Cygni]] is the [[X-ray]] source [[Cygnus X-1]], which is now thought to be caused by a [[black hole]] accreting matter in a binary star system. This was the first X-ray source widely believed to be a black hole.<ref name=esa20041105>{{citation | author=Staff | date=2004-11-05 | publisher=ESA | title=Observations: Seeing in X-ray wavelengths | url=http://www.esa.int/Our_Activities/Space_Science/Observations_Seeing_in_X-ray_wavelengths | access-date=2008-08-12 }}</ref><ref>Glister, Paul (2011), "[http://www.centauri-dreams.org/?p=20738 Cygnus X-1: A Black Hole Confirmed]." [http://www.centauri-dreams.org Centauri Dreams: Imagining and Planning Interstellar Exploration], 2011-11-29. Accessed 2016-09-16.</ref> It is located approximately 2.2 kiloparsecs from the [[Sun]].<ref>{{cite journal |last1=Miller-Jones |first1=James C. A. |last2=Bahramian |first2=Arash |last3=Orosz |first3=Jerome A. |last4=Mandel |first4=Ilya |last5=Gou |first5=Lijun |last6=Maccarone |first6=Thomas J. |last7=Neijssel |first7=Coenraad J. |last8=Zhao |first8=Xueshan |last9=Ziółkowski |first9=Janusz |last10=Reid |first10=Mark J. |last11=Uttley |first11=Phil |last12=Zheng |first12=Xueying |last13=Byun |first13=Do-Young |last14=Dodson |first14=Richard |last15=Grinberg |first15=Victoria |last16=Jung |first16=Taehyun |last17=Kim |first17=Jeong-Sook |last18=Marcote |first18=Benito |last19=Markoff |first19=Sera |last20=Rioja |first20=María J. |last21=Rushton |first21=Anthony P. |last22=Russell |first22=David M. |last23=Sivakoff |first23=Gregory R. |last24=Tetarenko |first24=Alexandra J. |last25=Tudose |first25=Valeriu |last26=Wilms |first26=Joern |title=Cygnus X-1 contains a 21–solar mass black hole—Implications for massive star winds |journal=Science |date=5 March 2021 |volume=371 |issue=6533 |pages=1046–1049 |doi=10.1126/science.abb3363|pmid=33602863 |arxiv=2102.09091 |bibcode=2021Sci...371.1046M |s2cid=231951746 }}</ref> There is also [[Supergiant star|supergiant]] [[variable star]] in the system which is known as [[HDE 226868]].<ref>{{Cite journal|arxiv=1401.1035|last1=Ziolkowski|first1=Janusz|title=Masses of the components of the HDE 226868/Cyg X-1 binary system|journal=Monthly Notices of the Royal Astronomical Society: Letters|volume=440|pages=L61|year=2014|doi=10.1093/mnrasl/slu002|doi-access=free |bibcode = 2014MNRAS.440L..61Z |s2cid=54841624}}</ref>

[[File:Albireo.jpg|thumb|right|The two component stars of [[Albireo]] are easily distinguished, even in a small telescope.]]

Cygnus also contains several other noteworthy X-ray sources. [[Cygnus X-3]] is a [[microquasar]] containing a [[Wolf–Rayet star]] in orbit around a very compact object,<ref name="2Kim">{{Cite journal |last1=Kim |first1=J. S. |last2=Kim |first2=S. W. |last3=Kurayama |first3=T. |last4=Honma |first4=M. |last5=Sasao |first5=T. |last6=Kim |first6=S. J. |doi=10.1088/0004-637X/772/1/41 |title=Vlbi Observation of Microquasar Cyg X-3 During an X-Ray State Transition from Soft to Hard in the 2007 May-June Flare |journal=The Astrophysical Journal |volume=772 |issue=1 |pages=41 |year=2013 |arxiv=1307.1226 |bibcode=2013ApJ...772...41K|s2cid=119251416 }}</ref> with a period of only 4.8 hours.<ref name="Becker">{{Cite journal |last1=Becker |first1=R. H. |last2=Robinson-Saba |first2=J. L. |last3=Pravdo |first3=S. H. |last4=Boldt |first4=E. A. |last5=Holt |first5=S. S. |last6=Serlemitsos |first6=P. J. |last7=Swank |first7=J. H. |title=A 4.8-hour periodicity in the spectra of Cygnus X-3 |doi=10.1086/182772 |journal=The Astrophysical Journal |volume=224 |pages=L113 |year=1978 |bibcode=1978ApJ...224L.113B}}</ref> The system is one of the most intrinsically luminous X-ray sources observed.<ref name="Koerding">{{Cite journal |last1=Körding |first1=E. |last2=Colbert |first2=E. |last3=Falcke |first3=H. |doi=10.1051/0004-6361:20042452 |title=A radio monitoring survey of ultra-luminous X-ray sources |journal=Astronomy and Astrophysics |volume=436 |issue=2 |pages=427 |year=2005 |arxiv=astro-ph/0502265 |bibcode=2005A&A...436..427K|s2cid=18693471 }}</ref> The system undergoes periodic outbursts of unknown nature,<ref name="Fender">{{Cite journal |last1=Fender |first1=R. P. |last2=Hanson |first2=M. M. |last3=Pooley |first3=G. G. |doi=10.1046/j.1365-8711.1999.02726.x |title=Infrared spectroscopic variability of Cygnus X-3 in outburst and quiescence |journal=Monthly Notices of the Royal Astronomical Society |volume=308 |issue=2 |pages=473 |year=1999 |doi-access=free |arxiv=astro-ph/9903435 |bibcode=1999MNRAS.308..473F|s2cid=16013132 }}</ref> and during one such outburst, the system was found to be emitting [[muon]]s, likely caused by [[neutrino]]s.<ref name="Marshak">{{Cite journal |last1=Marshak |first1=M. |last2=Bartelt |first2=J. |last3=Courant |first3=H. |last4=Heller |first4=K. |last5=Joyce |first5=T. |last6=Peterson |first6=E. |last7=Ruddick |first7=K. |last8=Shupe |first8=M. |last9=Ayres |first9=D. | last10 = Dawson | first10 = J. |last11=Fields |first11=T. |last12=May |first12=E. |last13=Price |first13=L. |last14=Sivaprasad |first14=K. |title=Evidence for Muon Production by Particles from Cygnus X-3 |doi=10.1103/PhysRevLett.54.2079 |journal=Physical Review Letters |volume=54 |issue=19 |pages=2079–2082 |year=1985 |pmid=10031224 |bibcode=1985PhRvL..54.2079M |url=https://zenodo.org/record/1233841 }}</ref> While the compact object is thought to be a [[neutron star]] or possibly a black hole,<ref name="Zdziarski">{{Cite journal |last1=Zdziarski |first1=A. A. |last2=Mikolajewska |first2=J. |last3=Belczynski |first3=K. |title=Cyg X-3: A low-mass black hole or a neutron star |doi=10.1093/mnrasl/sls035 |journal=Monthly Notices of the Royal Astronomical Society: Letters |volume=429 |pages=L104–L108 |year=2012 |doi-access=free |arxiv=1208.5455 |bibcode=2013MNRAS.429L.104Z|s2cid=119185839 }}</ref> it is possible that the object is instead a more exotic stellar remnant, possibly the first discovered [[quark star]], hypothesized due to its production of cosmic rays<ref name="Baym">{{Cite journal |last1=Baym |first1=G. |author-link=Gordon Baym |last2=Kolb |first2=E. W. |author-link2=Edward Kolb |last3=McLerran |first3=L. |last4=Walker |first4=T. P. |last5=Jaffe |first5=R. L. |title=Is Cygnus X-3 strange? |doi=10.1016/0370-2693(85)91489-3 |journal=Physics Letters B |volume=160 |issue=1–3 |pages=181 |year=1985 |bibcode=1985PhLB..160..181B}}</ref> that cannot be explained if the object is a normal neutron star. The system also emits [[cosmic ray]]s and [[gamma ray]]s, and has helped shed insight on to the formation of such rays.<ref name="MacKeown">{{Cite journal |last1=MacKeown |first1=P. K. |last2=Weekes |first2=T. C. |author-link2=Trevor C. Weekes |doi=10.1038/scientificamerican1185-60 |title=Cosmic Rays from Cygnus X-3 |journal=Scientific American |volume=253 |issue=5 |pages=60 |year=1985 |bibcode=1985SciAm.253e..60M}}</ref> [[Cygnus X-2]] is another [[X-ray binary]], containing an A-type giant in orbit around a neutron star with a 9.8-day period.<ref name="Crampton">{{Cite journal |last1=Crampton |first1=D. |last2=Cowley |first2=A. P. |doi=10.1086/130636 |title=Confirmation of a 9.8-day period of Cygnus X-2 |journal=Publications of the Astronomical Society of the Pacific |volume=92 |pages=147 |year=1980 |bibcode=1980PASP...92..147C|doi-access=free }}</ref> The system is interesting due to the rather small mass of the companion star, as most [[millisecond pulsar]]s have much more massive companions.<ref name="King">{{Cite journal |last1=King |first1=A. R. |last2=Ritter |first2=H. |doi=10.1046/j.1365-8711.1999.02862.x |title=Cygnus X-2, super-Eddington mass transfer, and pulsar binaries |journal=Monthly Notices of the Royal Astronomical Society |volume=309 |issue=1 |pages=253 |year=1999 |doi-access=free |arxiv=astro-ph/9812343 |bibcode=1999MNRAS.309..253K|s2cid=6898321 }}</ref> Another black hole in Cygnus is [[V404 Cygni]], which consists of a [[K-type star]] orbiting around a black hole of around 12 solar masses.<ref name="Shahbaz">{{cite journal |title=The mass of the black hole in V404 Cygni |last1=Shahbaz |first1=T. |journal=MNRAS |year=1994 |volume=271 |pages=L1–L14 |bibcode=1994MNRAS.271L..10S |last2=Ringwald |first2=F. A. |last3=Bunn |first3=J. C. |last4=Naylor |first4=T. |last5=Charles |first5=P. A. |last6=Casares |first6=J. |doi=10.1093/mnras/271.1.L10 |doi-access=free }}</ref> The black hole, similar to that of Cygnus X-3, has been hypothesized to be a quark star.<ref name="Kovács">{{Cite journal |last1=Kovács |first1=Z. |last2=Cheng |first2=K. S. |last3=Harko |first3=T. |doi=10.1111/j.1365-2966.2009.15571.x |title=Can stellar mass black holes be quark stars? |journal=Monthly Notices of the Royal Astronomical Society |volume=400 |issue=3 |pages=1632–1642 |year=2009 |doi-access=free |arxiv=0908.2672 |bibcode=2009MNRAS.400.1632K|s2cid=18263809 }}</ref> [[4U 2129+ 47]] is another X-ray binary containing a neutron star which undergoes outbursts,<ref name="Nowak">{{Cite journal |last1=Nowak |first1=M. A. |last2=Heinz |first2=S. |last3=Begelman |first3=M. C. |doi=10.1086/340757 |title=Hiding in Plain Sight:ChandraObservations of the Quiescent Neutron Star 4U 2129+47 in Eclipse |journal=The Astrophysical Journal |volume=573 |issue=2 |pages=778 |year=2002 |arxiv=astro-ph/0204503 |bibcode=2002ApJ...573..778N|s2cid=15872343 }}</ref> as is [[EXO 2030+ 375]].<ref name="WilsonC">{{Cite journal |last1=Wilson |first1=C. A. |last2=Finger |first2=M. H. |last3=Camero-Arranz |first3=A. N. |doi=10.1086/587134 |title=Outbursts Large and Small from EXO 2030+375 |journal=The Astrophysical Journal |volume=678 |issue=2 |pages=1263 |year=2008 |arxiv=0804.1375 |bibcode=2008ApJ...678.1263W|s2cid=17283290 }}</ref>

Cygnus is also home to several [[variable star]]s. [[SS Cygni]] is a [[dwarf nova]] which undergoes outbursts every 7–8 weeks. The system's total magnitude varies from 12th magnitude at its dimmest to 8th magnitude at its brightest. The two objects in the system are incredibly close together, with an orbital period of less than 0.28 days.<ref name="Honey">{{cite journal |author=Honey, W.B. | display-authors=etal |title=Quiescent and Outburst Photometry of the Dwarf Nova SS Cygni |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=236 |issue=4 |year=1989 |pages=727–34 |bibcode=1989MNRAS.236..727H |doi=10.1093/mnras/236.4.727 | doi-access=free |url=https://academic.oup.com/mnras/article-pdf/236/4/727/3924363/mnras236-0727.pdf |archive-url=https://web.archive.org/web/20170922074915/https://academic.oup.com/mnras/article-pdf/236/4/727/3924363/mnras236-0727.pdf |archive-date=2017-09-22 |url-status=live}}</ref> [[Chi Cygni|χ Cygni]] is a [[red giant]] and the second-brightest [[Mira variable]] star at its maximum. It ranges between magnitudes 3.3 and 14.2, and spectral types S6,2e to S10,4e (MSe) over a period of 408 days;<ref name=AAVSOchi>{{cite web |url=http://www.aavso.org/vsx/index.php?view=detail.top&oid=13285 |title=khi Cygni |last=BSJ |date=4 January 2010 |website=AAVSO Website |publisher=American Association of Variable Star Observers |access-date=22 December 2013}}</ref> it has a diameter of 300 [[solar diameter]]s and is 350 light-years from Earth. [[P Cygni]] is a [[luminous blue variable]] that brightened suddenly to 3rd magnitude in 1600 AD. Since 1715, the star has been of 5th magnitude,<ref>{{cite book |first=Robert Jr. |last=Burnham |year=1978 |title=Burnham's Celestial Handbook: An Observer's Guide to the Universe Beyond the Solar System |edition=Revised and Enlarged |volume=2 |location=[[New York City|New York]] |publisher=Dover Publications |pages=772–773}}</ref> despite being more than 5000 light-years from Earth. The star's [[stellar spectrum|spectrum]] is unusual in that it contains very strong emission lines resulting from surrounding nebulosity.<ref name="Markova">{{cite journal |title=An analysis of emission lines in the spectrum of P Cygni |last1=Markova |first1=N. |last2=de Groot |first2=M. |journal=The Astronomical Journal |volume=326 |pages=1111–16 |year=1997 |bibcode=1997A&A...326.1111M }}</ref> [[W Cygni]] is a [[semi-regular variable]] [[red giant]] star, 618 light-years from Earth.It has a maximum magnitude of 5.10 and a minimum magnitude 6.83; its period of 131 days.  It is a [[red giant]] ranging between spectral types M4e-M6e(Tc:)III,<ref name=AAVSOW>{{cite web |url=http://www.aavso.org/vsx/index.php?view=detail.top&oid=10926 |title=W Cygni |last=BSJ |date=19 August 2011 |website=AAVSO Website |publisher=American Association of Variable Star Observers |access-date=31 December 2013}}</ref> [[NML Cygni]] is a red [[hypergiant]] semi-regular variable star located at 5,300 light-years away from Earth. It is [[List of largest known stars|one of largest stars currently known]] in the galaxy with a radius exceeding 1,000 [[Solar radius|solar radii]].<ref>{{Cite journal|last1=De Beck|first1=E.|last2=Decin|first2=L.|last3=de Koter|first3=A.|last4=Justtanont|first4=K.|last5=Verhoelst|first5=T.|last6=Kemper|first6=F.|last7=Menten|first7=K. M.|date=November 2010|title=Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles|journal=Astronomy & Astrophysics|volume=523|pages=A18|doi=10.1051/0004-6361/200913771|issn=0004-6361|arxiv=1008.1083|bibcode=2010A&A...523A..18D|s2cid=16131273}}</ref> Its magnitude is around 16.6, its period is about 940 days.<ref name="Imaging the Cool Hypergiant NML Cygni’s Dusty Circumstellar Envelope with Adaptive Optics">{{Cite journal |last1=Schuster |first1=M. T. |last2=Marengo |first2=M. |last3=Hora |first3=J. L. |last4=Fazio |first4=G. G. |last5=Humphreys |first5=R. M. |last6=Gehrz |first6=R. D. |last7=Hinz |first7=P. M. |last8=Kenworthy |first8=M. A. |last9=Hoffmann |first9=W. F. |author-link5=Roberta M. Humphreys |doi=10.1088/0004-637X/699/2/1423 |title=Imaging the Cool Hypergiant NML Cygni's Dusty Circumstellar Envelope with Adaptive Optics |journal=The Astrophysical Journal |volume=699 |issue=2 |pages=1423–1432 |year=2009 |arxiv=0904.4690 |bibcode=2009ApJ...699.1423S|s2cid=17699562 }}</ref>

The star [[KIC 8462852]] (Tabby's Star) has received widespread press coverage because of unusual light fluctuations.<ref>{{cite journal |title=Orphaned Exomoons: Tidal Detachment and Evaporation Following an Exoplanet-Star Collision |journal=[[Monthly Notices of the Royal Astronomical Society]] |last1=Martinez |first1=Miguel A. S. |last2=Stone |first2=Nicholas C. |last3=Metzger |first3=Brian D. |display-authors=1 |volume=489 |issue=4 |pages=5119–5135 |date=November 2019 |doi=10.1093/mnras/stz2464 |doi-access=free |bibcode=2019MNRAS.489.5119M|arxiv=1906.08788 |s2cid=195316956 }}</ref>