Editing Vela (constellation) (section)

===Stars===
{{see also|List of stars in Vela}}
The brightest star in the constellation, Gamma Velorum, is a complex multiple star system. The brighter component, known as Gamma<sup>2</sup> Velorum, shines as a blue-white star of apparent magnitude 1.83.<ref name=ducati>{{cite journal|bibcode=2002yCat.2237....0D|title=VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system|journal=CDS/ADC Collection of Electronic Catalogues|volume=2237|pages=0|last1=Ducati|first1=J. R.|year=2002}}</ref> It is a spectroscopic binary made up of two very hot blue stars orbiting each other every 78.5 days and separated by somewhere between 0.8 and 1.6 Astronomical Units (AU). The brighter component is a hot blue main-sequence star of spectral type O7.5 and is around 280,000 times as luminous,  is around 30 times as massive and is 17 times the diameter of the Sun with a surface temperature of 35,000 K. The second component is an extremely rare example of hot star known as a [[Wolf–Rayet star]], and is the closest and brightest example in the sky. It has a surface temperature of 57,000 and is around 170,000 times as luminous as the Sun, though it radiates most of its energy in the ultraviolet spectrum.<ref name=north>{{cite journal|bibcode=2007MNRAS.377..415N|title=Γ2 Velorum: Orbital solution and fundamental parameter determination with SUSI|journal=Monthly Notices of the Royal Astronomical Society|volume=377|pages=415–424|last1=North|first1=J. R.|last2=Tuthill|first2=P. G.|last3=Tango|first3=W. J.|last4=Davis|first4=J.|date=2007|issue=1|doi=10.1111/j.1365-2966.2007.11608.x|doi-access=free |arxiv = astro-ph/0702375 |s2cid=16425744}}</ref>  Gamma<sup>1</sup> is a blue-white star of spectral type B2III and apparent magnitude 4.3.<ref name=jeffries/>  The two pairs are separated by 41 arcseconds, easily separable in binoculars.<ref name=jeffries>{{Cite journal | doi = 10.1111/j.1365-2966.2008.14162.x| title = The stellar association around Gamma Velorum and its relationship with Vela OB2| year = 2009| last1 = Jeffries | first1 = R. D.| last2 = Naylor | first2 = T.| last3 = Walter | first3 = F. M.| last4 = Pozzo | first4 = M. P.| last5 = Devey | first5 = C. R.| journal = Monthly Notices of the Royal Astronomical Society| volume = 393| issue = 2| pages = 538| doi-access = free|arxiv = 0810.5320 |bibcode = 2009MNRAS.393..538J | s2cid = 17560818}}</ref>  Parallax measurements give a distance of 1,116 light-years,<ref name=hipparcos>{{citation | first=F. | last=van Leeuwen |date=November 2007 | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 |arxiv = 0708.1752 | s2cid=18759600 }}</ref> meaning that they are at least 12,000 AU apart.  Further afield are 7.3-magnitude Gamma Velorum C and 9.4-magnitude Gamma Velorum D, lying 62 and 93 arcseconds south-southeast from Gamma<sup>2</sup>.

[[File:The dusty ring around the aging double star IRAS 08544-4431.jpg|left|thumb|Dusty ring around double star [[IRAS 08544-4431]].<ref>{{cite web|title=Sharpest View Ever of Dusty Disc Around Aging Star|url=http://www.eso.org/public/news/eso1608/|access-date=23 March 2016}}</ref>]]

The next brightest star is [[Delta Velorum]] or Alsephina,<ref name="IAU-LSN">{{cite web | url=https://www.iau.org/public/themes/naming_stars/ | title=Naming Stars |publisher=IAU.org |access-date=8 August 2018}}</ref> also a multiple star system and one of the brightest eclipsing binaries in the sky. Together with [[Kappa Velorum]] or Markeb,<ref name="IAU-LSN"/> [[Iota Carinae]] or Aspidiske<ref name="IAU-LSN"/> and [[Epsilon Carinae]] or Avior,<ref name="IAU-LSN"/> it forms the diamond-shaped [[asterism (astronomy)|asterism]] known as the [[False Cross]]—so called because it is sometimes mistaken for the [[Crux|Southern Cross]], causing errors in [[astronavigation]].<ref>{{cite book|last=Moore|first=Patrick|title=Patrick Moore's Astronomy: Teach Yourself|publisher=Hachette |year=2010|isbn=978-1-4441-2977-9|url=https://books.google.com/books?id=D7M0Rgc1ONAC&pg=PT127}}</ref> Appearing as a white star of magnitude 1.95,<ref>{{cite web |url =http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD+74956 |title = V* Delta Velorum -- Eclipsing binary of Algol type (detached) |work = SIMBAD Astronomical Database|publisher=Centre de Données astronomiques de Strasbourg |access-date = 11 October 2013}}</ref> Delta is actually a triple or possibly quintuple star system located around 80 light-years from the [[Solar System]]. Delta A has a magnitude of 1.99 and is an [[eclipsing binary]] composed of two A-type white stars (Delta Aa and Ab) which orbit each other every  45.2 days and lie 0.5 AU from each other, with a resulting drop in magnitude of 0.4 when the dimmer one passes.in front of the brighter. Delta B is a 5.1 magnitude yellow G-class star of similar dimensions to the Sun which ranges between 26 and 72 AU away from the brighter pair, taking 142 years to complete a revolution. Further out still, at a distance of 1700 AU, are two red dwarfs of magnitudes 11 and 13. If they are part of the multiple system, they take 28000 years to complete an orbit.<ref name="kalerdelta">{{cite web|url=http://stars.astro.illinois.edu/sow/deltavel.html |title=Delta Velorum |last=Kaler|first=Jim|author-link= James B. Kaler |work=Stars|publisher=University of Illinois|access-date=11 October 2013}}</ref> Also called Markeb, Kappa appears as a blue-white star of spectral type B2IV-V and magnitude 2.47 but is in fact a spectroscopic binary.<ref>{{cite web |url = http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Kappa+velorum&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id |title = Kappa Velorum - Spectroscopic binary |work = SIMBAD Astronomical Database|publisher=Centre de Données astronomiques de Strasbourg |access-date = 10 October 2013}}</ref> The two orbit around each other with a period of 116.65 days,<ref name=aaa424_727>{{citation | display-authors=1 | last1=Pourbaix | first1=D. | last2=Tokovinin | first2=A. A. | last3=Batten | first3=A. H. | last4=Fekel | first4=F. C. | last5=Hartkopf | first5=W. I. | last6=Levato | first6=H. | last7=Morrell | first7=N. I. | last8=Torres | first8=G. | last9=Udry | first9=S. | title=S<sub>B</sub>9: The ninth catalogue of spectroscopic binary orbits | journal=Astronomy and Astrophysics | volume=424 | issue=2 | pages=727–732 |date=September 2004 | doi=10.1051/0004-6361:20041213 | bibcode=2004A&A...424..727P |arxiv = astro-ph/0406573 | s2cid=119387088 }}</ref> but the size, mass and nature of the companion are as yet unclear.<ref name="kalermarkeb">{{cite web|url=http://stars.astro.illinois.edu/sow/markeb.html |title=Markeb |last=Kaler|first=Jim|author-link= James B. Kaler |work=Stars|publisher=University of Illinois|access-date=11 October 2013}}</ref>

The orange-hued [[Lambda Velorum]], or Suhail,<ref name="IAU-LSN"/> is the third-brightest star in the constellation. A supergiant of spectral type K4Ib-II, it varies between magnitudes 2.14 and 2.3,<ref name=lambvar>{{cite web |url = http://www.aavso.org/vsx/index.php?view=detail.top&oid=37806 |title = Lambda Velorum |publisher = American Association of Variable Star Observers |work = International Variable Star Index |access-date = 11 October 2013 |date = 25 September 2009}}</ref> and lies 545 light-years distant.<ref>{{cite web |url = http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Lambda+velorum&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id |title = V* Lambda Velorum -- Pulsating Variable Star|work = SIMBAD Astronomical Database|publisher=Centre de Données astronomiques de Strasbourg |access-date = 10 October 2013}}</ref> It has around 11,000 times the luminosity, 9 to 12 times the mass and 207 times the diameter of the Sun.<ref name="kalersuhail">{{cite web|url=http://stars.astro.illinois.edu/sow/suhail.html |title=Suhail |last=Kaler|first=Jim|author-link= James B. Kaler |work=Stars|publisher=University of Illinois|access-date=10 October 2013}}</ref>

[[AH Velorum]] is a Cepheid variable located less than a degree to the northeast of Gamma.<ref name="motz"/> A yellow-white supergiant of spectral type F7Ib-II, it pulsates between magnitudes 5.5 and 5.89 over 4.2 days.<ref name=AHvar>{{cite web |url = http://www.aavso.org/vsx/index.php?view=detail.top&oid=37478 |title = AH Velorum |publisher = American Association of Variable Star Observers |work = International Variable Star Index |access-date = 11 October 2013 |date = 4 January 2010}}</ref> Also lying close to Gamma,<ref name="moorebinocs">{{cite book|last=Moore|first=Patrick|title=Exploring the Night Sky with Binoculars|publisher=Cambridge University Press|location=Cambridge, United Kingdom|year=2010|pages=144|isbn=978-0-521-79390-2|url=https://books.google.com/books?id=Jvbtl2Vyxm4C&pg=PA144}}</ref> [[V Velorum]] is a Cepheid of spectral type F6-F9II ranging from magnitude 7.2 to 7.9 over 4.4 days.<ref name=vvar>{{cite web |url = http://www.aavso.org/vsx/index.php?view=detail.top&oid=37421 |title = V Velorum |publisher = American Association of Variable Star Observers |work = International Variable Star Index |access-date = 11 October 2013 |date = 4 January 2010}}</ref> [[AI Velorum]] is located 2.8 degrees north-northeast of Gamma,<ref name="motz"/> a Delta Scuti variable of spectral type A2p-F2pIV/V that ranges between magnitudes 6.15 and 6.76 in around 2.7 hours.<ref name=AIvar>{{cite web |url = https://www.aavso.org/vsx/index.php?view=detail.top&oid=37479 |title = AI Velorum |publisher = American Association of Variable Star Observers |work = International Variable Star Index |access-date = 10 August 2022 |date = 11 September 2011}}</ref>

[[V390 Velorum]] is an aged star that has been found to be surrounded by a dusty disk. An [[RV Tauri variable]], it has a spectral type of F3e and ranges between magnitudes 9.01 and 9.27 over nearly 95 days.<ref name=V390var>{{cite web |url =http://www.aavso.org/vsx/index.php?view=detail.top&oid=136435 |title = V0390 Velorum |publisher = American Association of Variable Star Observers |work = International Variable Star Index |access-date = 11 October 2013 |date = 25 May 2011}}</ref>

[[Omicron Velorum]] is a blue-white subgiant of spectral type B3III-IV located around 495 light-years from the Solar System. A slowly pulsating B star, it ranges between magnitudes 3.57 and 3.63 over 2.8 days.<ref name=omvar>{{cite web |url = http://www.aavso.org/vsx/index.php?view=detail.top&oid=37807 |title = Omicron Velorum |publisher = American Association of Variable Star Observers |work = International Variable Star Index |access-date = 11 October 2013 |date = 10 February 2012}}</ref> It is the brightest star in, and gives its name to, the Omicron Velorum Cluster, also known as [[IC 2391]], an [[open cluster]] located around 500 light-years away.

Seven star systems have been found to have [[exoplanet|planets]]. [[HD 75289]] is a Sun-like star of spectral type G0V with a [[hot Jupiter]] planetary companion that takes only about 3.51 days to revolve at an [[orbital distance]] of 0.0482 [[Astronomical Unit|AU]]. [[WASP-19]] is a star of apparent magnitude 12.3 located 815 light-years away, which has a hot Jupiter-like planet that orbits every 0.7 days. [[HD 73526]] is a Sun-like star of spectral type G6V that has two planets around double the mass of Jupiter each with orbits of 187 and 377 days, respectively.

[[HD 85390]] is an orange dwarf of spectral type K1.5V lying around 111 light-years distant with a planet 42 times as massive as Earth orbiting every 788 days.

[[HD 93385]] is a Sun-like star of spectral type G2/G3V located around 138 light-years away that is orbited by two super-Earths with periods of 13 and 46 days and masses 8.3 and 10.1 times that of Earth, respectively.