Editing Aquarius (constellation) (section)

===Stars===
[[Image:AquariusCC.jpg|thumb|The constellation Aquarius as it can be seen by the naked eye]]

Despite both its prominent position on the zodiac and its large size, Aquarius has no particularly bright stars, its four brightest stars being less bright than {{nobr|[[stellar magnitude|magnitude]] 2.8 .}}{{sfn|Moore|2000}} (The Apparent Magnitude scale is reverse logarithmic, with increasingly bright objects having lower and lower (more negative) magnitudes.) Recent research has shown that there are several stars lying within its borders that possess [[extrasolar planet|planetary systems]].

The two brightest stars, [[Alpha Aquarii|α&nbsp;Aquarii]] and β&nbsp;Aquarii, are luminous yellow supergiants, of spectral types G0Ib and G2Ib respectively,<ref name=mnras402_2_1369/> that were once hot blue-white B-class main sequence stars 5 to 9&nbsp;times as massive as the Sun. The two are also moving through space perpendicular to the plane of the Milky Way.<ref name=apj627_1_L53>{{cite journal | last1=Ayres | first1=Thomas R. | last2=Brown | first2=Alexander | last3=Harper | first3=Graham M. | date=July 2005 | title=Chandra observations of coronal emission from the early G supergiants α and β&nbsp;Aquarii | journal=[[The Astrophysical Journal]] | volume=627 | issue=1 | pages=L53–L56 | doi=10.1086/431977 | bibcode=2005ApJ...627L..53A | doi-access=free }}</ref> β&nbsp;Aquarii is the brightest star in Aquarius with apparent {{nobr|magnitude 2.91}} – only slightly brighter than α&nbsp;Aquarii. It also has the proper name of Sadalsuud. Having cooled and swollen to around 50&nbsp;times the Sun's diameter, it is around 2200&nbsp;times as luminous as the Sun.<ref name=kalerbeta>{{cite web | first=James B. | last=Kaler | title=Sadalsuud (Beta Aquarii) | website=Stars |publisher=[[University of Illinois|U. Illinois]] | series=Astronomy Department | url=http://stars.astro.illinois.edu/sow/sadalsuud.html | access-date=11 October 2016 }}</ref> It is around 6.4&nbsp;times as massive as the Sun and around 56&nbsp;million years old.<ref name=leonid>{{cite journal |last1=Lyubimkov |first1=Leonid S. |last2=Lambert |first2=David L. |last3=Korotin |first3=Sergey A. |last4=Rachkovskaya |first4=Tamara M. |last5=Poklad |first5=Dmitry B. |year=2015 |title=Carbon abundance and the N/C ratio in atmospheres of A-, F- and G-type supergiants and bright giants |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=446 |issue=4 |page=3447 |doi=10.1093/mnras/stu2299 |doi-access=free |s2cid=118473779 |bibcode=2015MNRAS.446.3447L |arxiv=1411.2722}}</ref> Sadalsuud is {{nobr|540 ± 20 light-years}} from Earth.<ref name=vanLeeuwen2007>{{cite journal | first=F. | last=van&nbsp;Leeuwen | year=2007 | title=Validation of the new Hipparcos reduction | journal=[[Astronomy and Astrophysics]] | volume=474 | issue=2 | pages=653–64 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 | arxiv=0708.1752 | s2cid=18759600 }}</ref> α&nbsp;Aquarii, also known as ''Sadalmelik'', has apparent {{nobr|magnitude 2.94 .}} It is {{nobr|520 ± 20 [[light year]]s}} distant from Earth,<ref name=vanLeeuwen2007/> and is around 6.5&nbsp;times as massive as the Sun, and 3000&nbsp;times as luminous. It is 53&nbsp;million years old.<ref name=mnras402_2_1369>{{cite journal | last1=Lyubimkov | first1=Leonid S. | last2=Lambert | first2=David L. | last3=Rostopchin | first3=Sergey I. | last4=Rachkovskaya | first4=Tamara M. | last5=Poklad | first5=Dmitry B. | year=2010 | title=Accurate fundamental parameters for A-, F- and G-type supergiants in the solar neighbourhood | journal=[[Monthly Notices of the Royal Astronomical Society]] | volume=402 | issue=2 | pages=1369–1379 | doi=10.1111/j.1365-2966.2009.15979.x | doi-access=free | bibcode=2010MNRAS.402.1369L |arxiv = 0911.1335 | s2cid=119096173 }}</ref>

[[Gamma Aquarii|γ&nbsp;Aquarii]], also called ''Sadachbia'',<ref name=IAU-LSN>{{cite web | title=Star Names |publisher=[[International Astronomical Union]] |website=IAU.org | url=https://www.iau.org/public/themes/naming_stars/ |access-date=30 July 2018}}</ref> is a white main sequence star of spectral type star of spectral type A0V that is between 158 and 315&nbsp;million years old and is around 2.5&nbsp;times the Sun's mass ({{solar mass|2.5}}),<ref name=David2015>{{cite journal | last1=David | first1=Trevor J. | last2=Hillenbrand | first2=Lynne A. | year=2015 | title=The ages of early-type stars: Strömgren photometric methods calibrated, validated, tested, and applied to hosts and prospective hosts of directly imaged exoplanets | journal=[[The Astrophysical Journal]] | volume=804 | issue=2 | pages=146 | s2cid=33401607 | bibcode=2015ApJ...804..146D | doi=10.1088/0004-637X/804/2/146 | arxiv=1501.03154 }}<br/>{{cite web |title=Hipparcos&nbsp;102395 |website=[[VizieR]] |type=star data catalog entry |publisher=[[Centre de données astronomiques de Strasbourg|CDS]] |place=Strasbourg, FR |via=[[Harvard University]]–[[Smithsonian Institution]], [[Center for Astrophysics]] |url=https://vizier.cfa.harvard.edu/viz-bin/VizieR?-source=J/ApJ/804/146/table5&HIP=102395&-ref=VIZ649a83a23ca11c}}</ref> and double its radius.<ref name=aaa367_521>{{cite journal | last1=Pasinetti Fracassini | first1=L.E. | last2=Pastori | first2=L. | last3=Covino | first3=S. | last4=Pozzi | first4=A. | title=Catalogue of apparent diameters and absolute radii of stars (CADARS) – third edition – comments and statistics | journal=[[Astronomy and Astrophysics]] | volume=367 | issue=2 | pages=521–524 |date=February 2001 | doi=10.1051/0004-6361:20000451 | bibcode=2001A&A...367..521P | arxiv=astro-ph/0012289| s2cid=425754 }}</ref> Its magnitude is&nbsp;3.85, and it is {{nobr|164 ± 9 light years}} away,<ref name=vanLeeuwen2007/> hence its luminosity is {{Solar luminosity|50}}.{{sfn|Moore|2000}} The name ''Sadachbia'' comes from the Arabic for "lucky stars of the tents", ''sa'd al-akhbiya''.{{sfn|Star Tales}}

[[delta Aquarii|δ&nbsp;Aquarii]], also known as ''Skat''<ref name=IAU-LSN/>{{sfn|Ridpath|2001}} or ''Scheat''{{sfn|Moore|2000}} is a blue-white spectral type A2 star with apparent magnitude&nbsp;3.27 and [[luminosity]] {{Solar luminosity|105}}.{{sfn|Moore|2000}}

[[epsilon Aquarii|ε&nbsp;Aquarii]], also known as ''Albali'',{{sfn|Staal|1988|pp=42–44}} is a blue-white spectral type A1 star with apparent magnitude&nbsp;3.77, [[absolute magnitude]]&nbsp;1.2, and a luminosity of {{Solar luminosity|28}}.{{sfn|Moore|2000}}{{sfn|Ridpath|2001}}

[[zeta Aquarii|ζ&nbsp;Aquarii]] is a spectral type F2 [[double star]]; both stars are white.{{sfn|Ridpath|2001}} In combination, they appear to be magnitude&nbsp;3.6 with luminosity {{Solar luminosity|50}}. The primary has magnitude&nbsp;4.53 and the secondary's magnitude is&nbsp;4.31, but both have absolute {{nobr|magnitude 0.6.}}{{sfn|Moore|2000}} The system's orbital period is 760&nbsp;years; currently the two components are moving farther apart.{{sfn|Ridpath|2001}}

[[theta Aquarii|θ&nbsp;Aquarii]], sometimes called ''Ancha'',{{sfn|Staal|1988|pp=42–44}} is spectral type G8 with apparent magnitude&nbsp;4.16 and an absolute {{nobr|magnitude 1.4.}}{{sfn|Moore|2000}}

[[Kappa Aquarii|κ&nbsp;Aquarii]], also called ''Situla'', has an apparent {{nobr|magnitude 5.03.}}<ref name=IAU-LSN/>

[[lambda Aquarii|λ&nbsp;Aquarii]], also called ''Hudoor'' or ''Ekchusis'',{{sfn|Staal|1988|pp=42–44}} is [[M-type star|spectral type M2]] with magnitude&nbsp;3.74 and luminosity {{Solar luminosity|120}}.{{sfn|Moore|2000}}

[[xi Aquarii|ξ&nbsp;Aquarii]], also called ''Bunda'',<ref name=IAU-LSN/> is [[A-type star|spectral type A7]] with an apparent magnitude&nbsp;4.69 and an absolute {{nobr|magnitude 2.4.}}{{sfn|Moore|2000}}

[[pi Aquarii|π&nbsp;Aquarii]], also called ''Seat'', is [[B-type star|spectral type B0]] with apparent magnitude&nbsp;4.66 and absolute {{nobr|magnitude −4.1.}}{{sfn|Moore|2000}}