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{{short description|Star in the constellation of Vela}}
{{short description|Evolved K-type star in the constellation of Vela}}
{{Redirect|Suhail|other uses|Souhail (disambiguation){{!}}Souhail|other stars|Suhail (star)}}
{{redirect|Suhail}}
{{Starbox begin
{{Starbox begin
| name = λ Velorum<br>(Suhail)
| name = λ Velorum<br>(Suhail)
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| epoch = [[J2000.0]]
| epoch = [[J2000.0]]
| ra = {{RA|09|07|59.75787}}<ref name=aaa474_2_653/>
| ra = {{RA|09|07|59.75787}}<ref name=aaa474_2_653/>
| dec = {{DEC|&minus;43|25|57.3273}}<ref name=aaa474_2_653/>
| dec = {{DEC|−43|25|57.3273}}<ref name=aaa474_2_653/>
| appmag_v = 2.21<ref name=clpl4_99/> {{nowrap|(2.14 - 2.30<ref name=al32_9_604/>}}
| appmag_v = 2.21<ref name=clpl4_99/> {{nowrap|(2.14–2.30<ref name=al32_9_604/>}}
}}
}})
{{Starbox character
{{Starbox character
| class = K4&nbsp;Ib<ref name=perkins/>
| class = K4&nbsp;Ib<ref name=perkins/>
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{{Starbox astrometry
{{Starbox astrometry
| radial_v = +18.4<ref name=gcsrv/>
| radial_v = +18.4<ref name=gcsrv/>
| prop_mo_ra = &minus;24.01<ref name=aaa474_2_653/>
| prop_mo_ra = −24.01<ref name=aaa474_2_653/>
| prop_mo_dec = +13.52<ref name=aaa474_2_653/>
| prop_mo_dec = +13.52<ref name=aaa474_2_653/>
| parallax = 5.99
| parallax = 5.99
| p_error = 0.11
| p_error = 0.11
| parallax_footnote = <ref name=aaa474_2_653/>
| parallax_footnote = <ref name=aaa474_2_653/>
| absmag_v = &minus;3.99<ref name=setiawan/>
| absmag_v = −3.99<ref name=setiawan/>
}}
}}
{{Starbox detail
{{Starbox detail
| mass = {{nowrap|7 ± 1}}<ref name=carpenter/>
| source = <ref name=harper2022/>
| mass = {{val|7.0|1.5|1.1}}
⚫
| radius = 210<ref name=carpenter/>
| radius = {{val|211|6}}
| gravity = 0.6<ref name=carpenter/>
⚫
| gravity = 0.64<ref name=Rau/>
| metal_fe = +0.06<ref name=luck/>
| metal_fe = +0.06<ref name=luck/>
| age_myr = {{nowrap|31.6 ± 1.7}}<ref name=mnras410_1_190/>
| age_myr = {{nowrap|31.6 ± 1.7}}<ref name=mnras410_1_190/>
| luminosity = 7,900<ref name=carpenter/>
| luminosity = 8,300
| temperature = 3,800 - 4,000<ref name=carpenter/>
| temperature = {{val|3835|100|fmt=commas}}
| rotational_velocity = 6.7<ref name=setiawan/>
| rotational_velocity = {{val|5.6|1.0}}
}}
}}
{{Starbox catalog
{{Starbox catalog
| names=Alsuhail, Al Suhail al Wazn, Suhail, Al' Sukhal', [[Cordoba Durchmusterung|CD]]−42°4990, [[FK5]] 345, [[Henry Draper catalogue|HD]] 78647, [[Hipparcos catalogue|HIP]] 44816, [[Harvard Revised catalogue|HR]] 3634, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]] 220878
| names=Alsuhail, Al Suhail al Wazn, Suhail, Al' Sukhal', [[Cordoba Durchmusterung|CD]]−42°4990, [[FK5]] 345, [[Henry Draper Catalogue|HD]] 78647, [[Hipparcos catalogue|HIP]] 44816, [[Harvard Revised catalogue|HR]] 3634, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]] 220878
}}
}}
{{Starbox reference
{{Starbox reference
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{{Starbox end}}
{{Starbox end}}


'''Lambda Velorum''' ('''λ Velorum''', abbreviated '''Lambda Vel''', '''λ Vel'''), officially named '''Suhail''' {{IPAc-en|'|s|uː|h|ai|l}},<ref name="IAU-CSN">{{cite web | url=http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt | title=IAU Catalog of Star Names |accessdate=28 July 2016}}</ref> is a [[star]] in the southern [[constellation]] of [[Vela (constellation)|Vela]]. With a mean [[apparent visual magnitude]] of 2.21,<ref name=clpl4_99/> this is the [[List of stars in Vela|third-brightest]] star in the constellation and one of the [[List of brightest stars|brighter stars]] in the sky. The distance to this star can be measured directly using the [[parallax]] technique, yielding an estimated {{Convert|545|ly|pc|abbr=off|lk=on}} from the [[Sun]].<ref name=aaa474_2_653/>
'''Lambda Velorum''' ('''λ Velorum''', abbreviated '''Lambda Vel''', '''λ Vel'''), officially named '''Suhail''' {{IPAc-en|'|s|uː|h|ei|l}},<ref name="IAU-CSN"/> is a [[star]] in the [[Southern celestial hemisphere|southern]] [[constellation]] of [[Vela (constellation)|Vela]]. With a mean [[apparent visual magnitude]] of 2.21,<ref name=clpl4_99/> this is the [[List of stars in Vela|third-brightest star in the constellation]] and one of the [[List of brightest stars|brighter stars]] in the sky. The distance to this star can be measured directly using the [[parallax]] technique, yielding an estimated {{Convert|545|ly|pc|abbr=off|lk=on}} from the [[Sun]].<ref name=aaa474_2_653/>


==Nomenclature==
==Nomenclature==
''λ Velorum'' ([[Latinisation of names|Latinised]] to ''Lambda Velorum'') is the star's [[Bayer designation]].
''λ Velorum'' ([[Latinisation of names|Latinised]] to ''Lambda Velorum'') is the star's [[Bayer designation]].


It bore the traditional [[Arabic]] name السهيل الوزن ''suhayl al-wazn'' (''Al Suhail al Wazn''), but as a modern [[List of selected stars for navigation|navigation star]] this was shortened to ''Suhail''. '[[Suhail]]' (a common Arabic male first name) was traditionally used for at least three other stars: [[Canopus]]; [[Gamma Velorum]] (al Suhail al Muhlif); and [[Zeta Puppis]] (Suhail Hadar). In 2016, the [[International Astronomical Union]] organized a [[IAU Working Group on Star Names|Working Group on Star Names]] (WGSN)<ref name="WGSN">{{citation
It bore the traditional [[Arabic]] name سهيل الوزن ''Suhail al Wazn'', but as a modern [[List of selected stars for navigation|navigation star]] this was shortened to ''Suhail''. '[[Suhail]]' (a common Arabic male first name) was traditionally used for at least three other stars: [[Canopus]]; [[Gamma Velorum]] (Suhail al Muhlif); and [[Zeta Puppis]] (Suhail Hadar). In 2016, the [[International Astronomical Union]] organized a [[Working Group on Star Names]] (WGSN)<ref name="WGSN"/> to catalogue and standardize proper names for stars. The WGSN approved the name ''Suhail'' for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names (''Canopus'' had its name approved as is, and Zeta Puppis was given the name ''Naos'').<ref name="IAU-CSN"/>
⚫
| url=https://www.iau.org/science/scientific_bodies/working_groups/280/
⚫
| title=IAU Working Group on Star Names (WGSN)
⚫
| publisher=[[International Astronomical Union]]
| accessdate=22 May 2016 | postscript=. }}</ref> to catalogue and standardize proper names for stars. The WGSN approved the name ''Suhail'' for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names (''Canopus'' had its name approved as is, and Zeta Puppis was given the name ''Naos'').<ref name="IAU-CSN"/>


In [[Chinese astronomy]], Suhail is called 天記, [[Pinyin]]: Tiānjì, meaning ''Judge for Estimating the Age of Animals'', because this star is marking itself and stands alone in the ''Judge for Estimating the Age of Animals'' [[Asterism (astronomy)|asterism]], [[Ghost (Chinese constellation)|Ghost]] mansion (see : [[Chinese constellation]]).<ref>{{zh icon}} [http://aeea.nmns.edu.tw/2006/0606/ap060629.html AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 6 月 29 日]</ref> 天記 (Tiānjì), westernized into ''Tseen Ke'', but the name ''Tseen Ke'' was designated for [[Psi Velorum]] by R. H. Allen works and the meaning is "Heaven's Record".<ref name=Allen/>
In [[Chinese astronomy]], Suhail is called 天記 ([[Pinyin]]: Tiānjì), meaning ''Judge for Estimating the Age of Animals'', because this star is marking itself and stands alone in the ''Judge for Estimating the Age of Animals'' [[Asterism (astronomy)|asterism]]. [[Ghost (Chinese constellation)|Ghost]] mansion (see: [[Chinese constellation]]),<ref name=zh/> 天記 (Tiānjì), was westernized into ''Tseen Ke'', but the name ''Tseen Ke'' was designated for [[Psi Velorum]] by R. H. Allen works and the meaning is "Heaven's Record".<ref name=Allen/>


==Properties==
==Properties==
[[File:LambdaVelLightCurve.png|thumb|left|A [[light curve]] for Lambda Velorum, plotted from ''[[Hipparcos]]'' data<ref name=HipDataAccess/>]]
The outer envelope of λ Velorum has an [[effective temperature]] of about 4,000 [[Kelvin|K]], giving it the cool orange hue of a K-type star.<ref name=csiro/> It is an Lc-type, [[slow irregular variable|slow irregular]] [[variable star]] with its brightness varying between apparent magnitudes +2.14 to +2.30.<ref name=al32_9_604/>
It has an [[spectral type|spectral classification]] of K4 Ib,<ref name=perkins/> with the [[luminosity class]] Ib meaning that it is a lower luminosity [[red supergiant]] star. The outer envelope of λ Velorum has an [[effective temperature]] of about {{val|3835|ul=K|fmt=commas}},<ref name=harper2022/> giving it the cool orange hue of a [[K-type star]].<ref name=csiro/> It is an Lc-type, [[slow irregular variable|slow irregular]] [[variable star]] with its brightness varying between apparent magnitudes +2.14 to +2.30.<ref name=al32_9_604/>


λ Velorum is an [[stellar evolution|evolved]] star that has exhausted the hydrogen in its core region. It has about seven times the mass of the Sun. It is likely to be on or approaching the [[asymptotic giant branch]] (AGB), although its properties do not exclude it being a slightly more massive star on the [[red giant branch]] (RGB).<ref name=carpenter1998/> As an AGB star it has an inert core of carbon and oxygen and is alternately fusing helium and hydrogen in two shells outside the core. The star's outer envelope has expanded to form a deep, [[convection zone|convective]], [[hydrogen burning]] layer that is generating a [[stellar magnetic field|magnetic field]]. The surface strength of this field has been measured at {{nowrap|1.72 ± 0.33 [[Gauss (unit)|G]]}}.<ref name=mnras408_4_2290/> Massive stars use their [[hydrogen]] "fuel" much faster than do smaller stars and Lambda Velorum is estimated to be only some 32 million years old.<ref name=mnras410_1_190/>
λ Velorum is an [[stellar evolution|evolved]] star that has exhausted the hydrogen in its core region. It has about seven times the mass of the Sun. Despite having the luminosity class of a red [[supergiant]] star, it is likely to be on or approaching the [[asymptotic giant branch]] (AGB), although its properties do not exclude it being a slightly more massive star on the [[red giant branch]] (RGB).<ref name=carpenter1998/> As an AGB star it has an inert core of carbon and oxygen and is alternately fusing helium and hydrogen in two shells outside the core. The star's outer envelope has expanded to form a deep, [[convection zone|convective]], [[Hydrogen burning|hydrogen-burning]] layer that is generating a [[stellar magnetic field|magnetic field]]. The surface strength of this field has been measured at {{nowrap|1.72 ± 0.33 [[Gauss (unit)|G]]}}.<ref name=mnras408_4_2290/> Massive stars use their hydrogen "fuel" much faster than do smaller stars and Lambda Velorum is estimated to be only some 32 million years old.<ref name=mnras410_1_190/>


λ Velorum is near the upper end of the mass range for intermediate stars, which end their lives by producing a [[planetary nebula]] and a [[white dwarf]] remnant. It may be massive enough to produce an [[electron capture]] [[supernova]].<ref name=nomoto/>
λ Velorum is near the upper end of the mass range for intermediate stars, which end their lives by producing a [[planetary nebula]] and a [[white dwarf]] remnant. It may be massive enough to produce an [[electron-capture]] [[supernova]] (like the supernova that formed the [[Crab Nebula]]), and hence a [[neutron star]].<ref name=nomoto/>


==References==
==References==
{{Reflist|refs=
{{Reflist|refs=


<ref name=harper2022>{{cite journal |bibcode=2022AJ....164...16H |title=HST STIS Observations of ζ Aurigae A's Irradiated Atmosphere |last1=Harper |first1=Graham M. |last2=Bennett |first2=Philip D. |last3=Brown |first3=Alexander |last4=Ayres |first4=Thomas R. |last5=Ohnaka |first5=Keiichi |last6=Griffin |first6=Elizabeth |journal=The Astronomical Journal |year=2022 |volume=164 |issue=1 |page=16 |doi=10.3847/1538-3881/ac6feb |s2cid=250101470 |doi-access=free }}</ref>
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<ref name=aaa474_2_653>{{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 }}</ref>

<ref name=zh>{{in lang|zh}} [http://aeea.nmns.edu.tw/2006/0606/ap060629.html AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 6 月 29 日] {{Webarchive|url=https://web.archive.org/web/20210605100121/http://aeea.nmns.edu.tw/2006/0606/ap060629.html |date=2021-06-05 }}</ref>

<ref name="WGSN">{{citation
⚫
| url=https://www.iau.org/science/scientific_bodies/working_groups/280/
⚫
| title=IAU Working Group on Star Names (WGSN)
⚫
| publisher=[[International Astronomical Union]]
| access-date=22 May 2016 | postscript=. }}</ref>

<ref name="IAU-CSN">{{cite web | url=http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt | title=IAU Catalog of Star Names |access-date=28 July 2016}}</ref>

<ref name=HipDataAccess>{{cite web |title=Hipparcos Tools Interactive Data Access |url=https://www.cosmos.esa.int/web/hipparcos/interactive-data-access |website=Hipparcos |publisher=ESA |access-date=8 December 2021}}</ref>

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<ref name=aaa474_2_653>{{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>


<ref name=gcsrv>{{cite journal | last=Wilson | first=R. E. | date=1953 | title=General Catalogue of Stellar Radial Velocities | journal=Carnegie Institute Washington D.C. Publication | publisher=[[Carnegie Institute of Washington D.C.]] | bibcode=1953GCRV..C......0W }}</ref>
<ref name=gcsrv>{{cite journal | last=Wilson | first=R. E. | date=1953 | title=General Catalogue of Stellar Radial Velocities | journal=Carnegie Institute Washington D.C. Publication | publisher=[[Carnegie Institute of Washington D.C.]] | bibcode=1953GCRV..C......0W }}</ref>
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<ref name=clpl4_99>{{citation | display-authors=1 | last1=Johnson | first1=H. L. | last2=Iriarte | first2=B. | last3=Mitchell | first3=R. I. | last4=Wisniewskj | first4=W. Z. | title=UBVRIJKL photometry of the bright stars | journal=Communications of the Lunar and Planetary Laboratory | volume=4 | issue=99 | pages=99 | date=1966 | bibcode=1966CoLPL...4...99J }}</ref>
<ref name=clpl4_99>{{citation | display-authors=1 | last1=Johnson | first1=H. L. | last2=Iriarte | first2=B. | last3=Mitchell | first3=R. I. | last4=Wisniewskj | first4=W. Z. | title=UBVRIJKL photometry of the bright stars | journal=Communications of the Lunar and Planetary Laboratory | volume=4 | issue=99 | pages=99 | date=1966 | bibcode=1966CoLPL...4...99J }}</ref>


<ref name=mnras410_1_190>{{citation | last1=Tetzlaff | first1=N. | last2=Neuhäuser | first2=R. | last3=Hohle | first3=M. M. | title=A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun | journal=[[Monthly Notices of the Royal Astronomical Society]] | volume=410 | issue=1 | pages=190–200 |date=January 2011 | doi=10.1111/j.1365-2966.2010.17434.x | bibcode=2011MNRAS.410..190T |arxiv = 1007.4883 }}</ref>
<ref name=mnras410_1_190>{{citation | last1=Tetzlaff | first1=N. | last2=Neuhäuser | first2=R. | last3=Hohle | first3=M. M. | title=A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun | journal=[[Monthly Notices of the Royal Astronomical Society]] | volume=410 | issue=1 | pages=190–200 |date=January 2011 | doi=10.1111/j.1365-2966.2010.17434.x | doi-access=free | bibcode=2011MNRAS.410..190T |arxiv = 1007.4883 | s2cid=118629873 }}</ref>


<ref name=mnras408_4_2290>{{citation | display-authors=1 | last1=Grunhut | first1=J. H. | last2=Wade | first2=G. A. | last3=Hanes | first3=D. A. | last4=Alecian | first4=E. | title=Systematic detection of magnetic fields in massive, late-type supergiants | journal=Monthly Notices of the Royal Astronomical Society | volume=408 | issue=4 | pages=2290–2297 |date=November 2010 | doi=10.1111/j.1365-2966.2010.17275.x | bibcode=2010MNRAS.408.2290G |arxiv = 1006.5891 }}</ref>
<ref name=mnras408_4_2290>{{citation | display-authors=1 | last1=Grunhut | first1=J. H. | last2=Wade | first2=G. A. | last3=Hanes | first3=D. A. | last4=Alecian | first4=E. | title=Systematic detection of magnetic fields in massive, late-type supergiants | journal=Monthly Notices of the Royal Astronomical Society | volume=408 | issue=4 | pages=2290–2297 |date=November 2010 | doi=10.1111/j.1365-2966.2010.17275.x | doi-access=free | bibcode=2010MNRAS.408.2290G |arxiv = 1006.5891 | s2cid=118564860 }}</ref>


<ref name="Rau">{{Cite journal|last1=Rau|first1=Gioia|last2=Nielsen|first2=Krister E.|last3=Carpenter|first3=Kenneth G.|last4=Airapetian|first4=Vladimir|date=December 2018|title=HST/GHRS Observations of Cool, Low-gravity Stars. VI. Mass-loss Rates and Wind Parameters for M Giants|journal=The Astrophysical Journal|language=en|volume=869|issue=1|pages=1|doi=10.3847/1538-4357/aaf0a0|issn=0004-637X|arxiv=1811.10679|bibcode=2018ApJ...869....1R|s2cid=119364960 |doi-access=free }}</ref>
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<ref name=csiro>{{citation|title=The Colour of Stars |date=December 21, 2004 |work=Australia Telescope, Outreach and Education |publisher=[[Commonwealth Scientific and Industrial Research Organisation]] |url=http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |accessdate=2012-01-16 |url-status=dead |archiveurl=https://web.archive.org/web/20120222183238/http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |archivedate=February 22, 2012 }}</ref>


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<!-- <ref name=csiro>{{citation|title=The Colour of Stars |date=December 21, 2004 |work=Australia Telescope, Outreach and Education |publisher=[[Commonwealth Scientific and Industrial Research Organisation]] |url=http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |access-date=2012-01-16 |url-status=dead |archive-url=https://web.archive.org/web/20120222183238/http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |archive-date=February 22, 2012 }}</ref> -->
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<ref name=al32_9_604>{{citation | display-authors=1 | last1=Ruban | first1=E. V. | last2=Alekseeva | first2=G. A. | last3=Arkharov | first3=A. A. | last4=Hagen-Thorn | first4=E. I. | last5=Galkin | first5=V. D. | last6=Nikanorova | first6=I. N. | last7=Novikov | first7=V. V. | last8=Pakhomov | first8=V. P. | last9=Puzakova | first9=T. Yu. | title==Spectrophotometric observations of variable stars | journal=Astronomy Letters | volume=32 | issue=9 | pages=604–607 |date=September 2006 | doi=10.1134/S1063773706090052 | bibcode=2006AstL...32..604R }}. See the [http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/PAZh/32/672 J/PAZh/32/672] VizieR catalogue entry.</ref>


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<ref name=al32_9_604>{{citation | display-authors=1 | last1=Ruban | first1=E. V. | last2=Alekseeva | first2=G. A. | last3=Arkharov | first3=A. A. | last4=Hagen-Thorn | first4=E. I. | last5=Galkin | first5=V. D. | last6=Nikanorova | first6=I. N. | last7=Novikov | first7=V. V. | last8=Pakhomov | first8=V. P. | last9=Puzakova | first9=T. Yu. | title=Spectrophotometric observations of variable stars | journal=Astronomy Letters | volume=32 | issue=9 | pages=604–607 |date=September 2006 | doi=10.1134/S1063773706090052 | bibcode=2006AstL...32..604R | s2cid=121747360 }}. See the [http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/PAZh/32/672 J/PAZh/32/672] VizieR catalogue entry.</ref>
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<ref name=Allen>{{citation | url=http://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Argo_Navis*.html | first1=Richard Hinckley | last1=Allen | title=Star Names — Their Lore and Meaning: Argo Navis }}</ref>

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<ref name=Allen>{{citation | url=https://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Argo_Navis*.html | first1=Richard Hinckley | last1=Allen | title=Star Names — Their Lore and Meaning: Argo Navis }}</ref>


<ref name=perkins>{{cite journal|bibcode=1989ApJS...71..245K|title=The Perkins catalog of revised MK types for the cooler stars|journal=Astrophysical Journal Supplement Series|volume=71|pages=245|last1=Keenan|first1=Philip C.|last2=McNeil|first2=Raymond C.|year=1989|doi=10.1086/191373}}</ref>
<ref name=perkins>{{cite journal|bibcode=1989ApJS...71..245K|title=The Perkins catalog of revised MK types for the cooler stars|journal=Astrophysical Journal Supplement Series|volume=71|pages=245|last1=Keenan|first1=Philip C.|last2=McNeil|first2=Raymond C.|year=1989|doi=10.1086/191373}}</ref>


<ref name=setiawan>{{cite journal|bibcode=2004A&A...421..241S|title=Precise radial velocity measurements of G and K giants. Multiple systems and variability trend along the Red Giant Branch|journal=Astronomy and Astrophysics|volume=421|pages=241|last1=Setiawan|first1=J.|last2=Pasquini|first2=L.|last3=Da Silva|first3=L.|last4=Hatzes|first4=A. P.|last5=von Der Lühe|first5=O.|last6=Girardi|first6=L.|last7=De Medeiros|first7=J. R.|last8=Guenther|first8=E.|year=2004|doi=10.1051/0004-6361:20041042-1}}</ref>
<ref name=setiawan>{{cite journal|bibcode=2004A&A...421..241S|title=Precise radial velocity measurements of G and K giants. Multiple systems and variability trend along the Red Giant Branch|journal=Astronomy and Astrophysics|volume=421|pages=241|last1=Setiawan|first1=J.|last2=Pasquini|first2=L.|last3=Da Silva|first3=L.|last4=Hatzes|first4=A. P.|last5=von Der Lühe|first5=O.|last6=Girardi|first6=L.|last7=De Medeiros|first7=J. R.|last8=Guenther|first8=E.|year=2004|issue=1 |doi=10.1051/0004-6361:20041042-1|doi-access=free}}</ref>


<ref name=carpenter>{{cite journal|bibcode=1999ApJ...521..382C|title=GHRS Observations of Cool, Low-Gravity Stars. V. The Outer Atmosphere and Wind of the Nearby K Supergiant λ Velorum|journal=The Astrophysical Journal|volume=521|issue=1|pages=382–406|last1=Carpenter|first1=Kenneth G.|last2=Robinson|first2=Richard D.|last3=Harper|first3=Graham M.|last4=Bennett|first4=Philip D.|last5=Brown|first5=Alexander|last6=Mullan|first6=Dermott J.|year=1999|doi=10.1086/307520}}</ref>
<!-- <ref name=carpenter>{{cite journal|bibcode=1999ApJ...521..382C|title=GHRS Observations of Cool, Low-Gravity Stars. V. The Outer Atmosphere and Wind of the Nearby K Supergiant λ Velorum|journal=The Astrophysical Journal|volume=521|issue=1|pages=382–406|last1=Carpenter|first1=Kenneth G.|last2=Robinson|first2=Richard D.|last3=Harper|first3=Graham M.|last4=Bennett|first4=Philip D.|last5=Brown|first5=Alexander|last6=Mullan|first6=Dermott J.|year=1999|doi=10.1086/307520|s2cid=121891971 |doi-access=free}}</ref> -->


<ref name=luck>{{cite journal|bibcode= 2014AJ....147..137L|title= Parameters and Abundances in Luminous Stars|journal= The Astronomical Journal|volume= 147|issue= 6|pages= 137|last1= Luck|first1= R. Earle|year= 2014|doi= 10.1088/0004-6256/147/6/137}}</ref>
<ref name=luck>{{cite journal|bibcode= 2014AJ....147..137L|title= Parameters and Abundances in Luminous Stars|journal= The Astronomical Journal|volume= 147|issue= 6|pages= 137|last1= Luck|first1= R. Earle|year= 2014|doi= 10.1088/0004-6256/147/6/137|doi-access= free}}</ref>


<ref name=carpenter1998>{{cite journal|bibcode=1998IAUS..191P.206C|title=The Structure of the Outer Atmosphere and Wind of lambda Vel|journal=Asymptotic Giant Branch Stars|volume=191|pages=P206|last1=Carpenter|first1=Kenneth G.|year=1998}}</ref>
<ref name=carpenter1998>{{cite journal|bibcode=1998IAUS..191P.206C|title=The Structure of the Outer Atmosphere and Wind of lambda Vel|journal=Asymptotic Giant Branch Stars|volume=191|pages=206|last1=Carpenter|first1=Kenneth G.|year=1998}}</ref>


<ref name=nomoto>{{cite journal|bibcode=1984ApJ...277..791N|title=Evolution of 8-10 solar mass stars toward electron capture supernovae. I - Formation of electron-degenerate O + NE + MG cores|journal=Astrophysical Journal|volume=277|pages=791|last1=Nomoto|first1=K.|year=1984|doi=10.1086/161749}}</ref>
<ref name=nomoto>{{cite journal|bibcode=1984ApJ...277..791N|title=Evolution of 8-10 solar mass stars toward electron capture supernovae. I - Formation of electron-degenerate O + NE + MG cores|journal=Astrophysical Journal|volume=277|pages=791|last1=Nomoto|first1=K.|year=1984|doi=10.1086/161749|doi-access=free}}</ref>

<ref name=csiro>{{citation | title=The Colour of Stars | date=December 21, 2004 | work=Australia Telescope, Outreach and Education | publisher=Commonwealth Scientific and Industrial Research Organisation | url=http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html | accessdate=2012-01-16 | archive-date=2013-12-03 | archive-url=https://web.archive.org/web/20131203222826/http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html | url-status=dead }}</ref>


}}
}}


{{Stars of Vela}}
{{Stars of Vela}}
{{Portal bar|Astronomy|Stars|Outer space}}


{{Authority control}}
⚫
[[Category:Bayer objects|Velorum, Lambda]]

{{DEFAULTSORT:Lambda Velorum}}
[[Category:K-type supergiants]]
[[Category:K-type supergiants]]
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[[Category:Slow irregular variables]]
[[Category:Vela (constellation)]]
[[Category:Vela (constellation)]]
[[Category:Stars with proper names]]
[[Category:Bayer objects|Velorum, Lambda]]
[[Category:HR objects|3634]]
[[Category:Durchmusterung objects]]
[[Category:Henry Draper Catalogue objects|078647]]
[[Category:Henry Draper Catalogue objects|078647]]
[[Category:Hipparcos objects|044816]]
[[Category:Hipparcos objects|044816]]
[[Category:Durchmusterung objects]]
[[Category:Bright Star Catalogue objects|3634]]
[[Category:Stars with proper names|Suhail]]
⚫
[[Category:TIC objects]]
⚫
[[Category:Slow irregular variables]]

Latest revision as of 12:59, 9 September 2024

"Suhail" redirects here. For other uses, see Souhail. For other stars, see Suhail (star).
λ Velorum
(Suhail)
Location of λ Velorum (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Vela
Right ascension 09h 07m 59.75787s[1]
Declination −43° 25′ 57.3273″[1]
Apparent magnitude (V) 2.21[2] (2.14–2.30[3])
Characteristics
Spectral type K4 Ib[4]
U−B color index +1.80[2]
B−V color index +1.65[2]
Variable type LC[3]
Astrometry
Radial velocity (Rv)+18.4[5] km/s
Proper motion (μ) RA: −24.01[1] mas/yr
Dec.: +13.52[1] mas/yr
Parallax (π)5.99 ± 0.11 mas[1]
Distance545 ± 10 ly
(167 ± 3 pc)
Absolute magnitude (MV)−3.99[6]
Details[7]
Mass7.0+1.5
−1.1 M☉
Radius211±6 R☉
Luminosity8,300 L☉
Surface gravity (log g)0.64[8] cgs
Temperature3,835±100 K
Metallicity [Fe/H]+0.06[9] dex
Rotational velocity (v sin i)5.6±1.0 km/s
Age31.6 ± 1.7[10] Myr
Other designations
Alsuhail, Al Suhail al Wazn, Suhail, Al' Sukhal', CD−42°4990, FK5 345, HD 78647, HIP 44816, HR 3634, SAO 220878
Database references
SIMBADdata

Lambda Velorum (λ Velorum, abbreviated Lambda Vel, λ Vel), officially named Suhail /ˈsuːheɪl/,[11] is a star in the southern constellation of Vela. With a mean apparent visual magnitude of 2.21,[2] this is the third-brightest star in the constellation and one of the brighter stars in the sky. The distance to this star can be measured directly using the parallax technique, yielding an estimated 545 light-years (167 parsecs) from the Sun.[1]

Nomenclature

[edit]

λ Velorum (Latinised to Lambda Velorum) is the star's Bayer designation.

It bore the traditional Arabic name سهيل الوزن Suhail al Wazn, but as a modern navigation star this was shortened to Suhail. 'Suhail' (a common Arabic male first name) was traditionally used for at least three other stars: Canopus; Gamma Velorum (Suhail al Muhlif); and Zeta Puppis (Suhail Hadar). In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[12] to catalogue and standardize proper names for stars. The WGSN approved the name Suhail for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names (Canopus had its name approved as is, and Zeta Puppis was given the name Naos).[11]

In Chinese astronomy, Suhail is called 天記 (Pinyin: Tiānjì), meaning Judge for Estimating the Age of Animals, because this star is marking itself and stands alone in the Judge for Estimating the Age of Animals asterism. Ghost mansion (see: Chinese constellation),[13] 天記 (Tiānjì), was westernized into Tseen Ke, but the name Tseen Ke was designated for Psi Velorum by R. H. Allen works and the meaning is "Heaven's Record".[14]

Properties

[edit]
A light curve for Lambda Velorum, plotted from Hipparcos data[15]

It has an spectral classification of K4 Ib,[4] with the luminosity class Ib meaning that it is a lower luminosity red supergiant star. The outer envelope of λ Velorum has an effective temperature of about 3,835 K,[7] giving it the cool orange hue of a K-type star.[16] It is an Lc-type, slow irregular variable star with its brightness varying between apparent magnitudes +2.14 to +2.30.[3]

λ Velorum is an evolved star that has exhausted the hydrogen in its core region. It has about seven times the mass of the Sun. Despite having the luminosity class of a red supergiant star, it is likely to be on or approaching the asymptotic giant branch (AGB), although its properties do not exclude it being a slightly more massive star on the red giant branch (RGB).[17] As an AGB star it has an inert core of carbon and oxygen and is alternately fusing helium and hydrogen in two shells outside the core. The star's outer envelope has expanded to form a deep, convective, hydrogen-burning layer that is generating a magnetic field. The surface strength of this field has been measured at 1.72 ± 0.33 G.[18] Massive stars use their hydrogen "fuel" much faster than do smaller stars and Lambda Velorum is estimated to be only some 32 million years old.[10]

λ Velorum is near the upper end of the mass range for intermediate stars, which end their lives by producing a planetary nebula and a white dwarf remnant. It may be massive enough to produce an electron-capture supernova (like the supernova that formed the Crab Nebula), and hence a neutron star.[19]

References

[edit]
  1. ^ a b c d e f van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600
  2. ^ a b c d Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J
  3. ^ a b c Ruban, E. V.; et al. (September 2006), "Spectrophotometric observations of variable stars", Astronomy Letters, 32 (9): 604–607, Bibcode:2006AstL...32..604R, doi:10.1134/S1063773706090052, S2CID 121747360. See the J/PAZh/32/672 VizieR catalogue entry.
  4. ^ a b Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
  5. ^ Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Carnegie Institute of Washington D.C. Bibcode:1953GCRV..C......0W.
  6. ^ Setiawan, J.; Pasquini, L.; Da Silva, L.; Hatzes, A. P.; von Der Lühe, O.; Girardi, L.; De Medeiros, J. R.; Guenther, E. (2004). "Precise radial velocity measurements of G and K giants. Multiple systems and variability trend along the Red Giant Branch". Astronomy and Astrophysics. 421 (1): 241. Bibcode:2004A&A...421..241S. doi:10.1051/0004-6361:20041042-1.
  7. ^ a b Harper, Graham M.; Bennett, Philip D.; Brown, Alexander; Ayres, Thomas R.; Ohnaka, Keiichi; Griffin, Elizabeth (2022). "HST STIS Observations of ζ Aurigae A's Irradiated Atmosphere". The Astronomical Journal. 164 (1): 16. Bibcode:2022AJ....164...16H. doi:10.3847/1538-3881/ac6feb. S2CID 250101470.
  8. ^ Rau, Gioia; Nielsen, Krister E.; Carpenter, Kenneth G.; Airapetian, Vladimir (December 2018). "HST/GHRS Observations of Cool, Low-gravity Stars. VI. Mass-loss Rates and Wind Parameters for M Giants". The Astrophysical Journal. 869 (1): 1. arXiv:1811.10679. Bibcode:2018ApJ...869....1R. doi:10.3847/1538-4357/aaf0a0. ISSN 0004-637X. S2CID 119364960.
  9. ^ Luck, R. Earle (2014). "Parameters and Abundances in Luminous Stars". The Astronomical Journal. 147 (6): 137. Bibcode:2014AJ....147..137L. doi:10.1088/0004-6256/147/6/137.
  10. ^ a b Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873
  11. ^ a b "IAU Catalog of Star Names". Retrieved 28 July 2016.
  12. ^ IAU Working Group on Star Names (WGSN), International Astronomical Union, retrieved 22 May 2016.
  13. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 6 月 29 日 Archived 2021-06-05 at the Wayback Machine
  14. ^ Allen, Richard Hinckley, Star Names — Their Lore and Meaning: Argo Navis
  15. ^ "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
  16. ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on 2013-12-03, retrieved 2012-01-16
  17. ^ Carpenter, Kenneth G. (1998). "The Structure of the Outer Atmosphere and Wind of lambda Vel". Asymptotic Giant Branch Stars. 191: 206. Bibcode:1998IAUS..191P.206C.
  18. ^ Grunhut, J. H.; et al. (November 2010), "Systematic detection of magnetic fields in massive, late-type supergiants", Monthly Notices of the Royal Astronomical Society, 408 (4): 2290–2297, arXiv:1006.5891, Bibcode:2010MNRAS.408.2290G, doi:10.1111/j.1365-2966.2010.17275.x, S2CID 118564860
  19. ^ Nomoto, K. (1984). "Evolution of 8-10 solar mass stars toward electron capture supernovae. I - Formation of electron-degenerate O + NE + MG cores". Astrophysical Journal. 277: 791. Bibcode:1984ApJ...277..791N. doi:10.1086/161749.
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