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Lambda Velorum - Wikipedia

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λ Velorum
(Suhail)
Observation data Epoch J2000.0 Equinox J2000.0
Location of λ Velorum (circled)
Constellation	Vela
Right ascension	09^h 07^m 59.75787^s^[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 (R_v)	+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]
Distance	545 ± 10 ly (167 ± 3 pc)
Absolute magnitude (M_V)	−3.99^[6]

Details^[7]

Mass	7.0+1.5 −1.1 `M`_☉
Radius	211±6 `R`_☉
Luminosity	8,300 `L`_☉
Surface gravity (log g)	0.64^[8] cgs
Temperature	3,835±100 K
Metallicity [Fe/H]	+0.06^[9] dex
Rotational velocity (v sin i)	5.6±1.0 km/s
Age	31.6 ± 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
SIMBAD	data

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

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

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

^ ^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
^ ^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
^ ^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.
^ ^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.
^ 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.
^ 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.
^ ^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.
^ 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.
^ 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.
^ ^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
^ ^a ^b "IAU Catalog of Star Names". Retrieved 28 July 2016.
^ IAU Working Group on Star Names (WGSN), International Astronomical Union, retrieved 22 May 2016.
^ (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
^ Allen, Richard Hinckley, Star Names — Their Lore and Meaning: Argo Navis
^ "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
^ "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
^ 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.
^ 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
^ 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.

Constellation of Vela

Stars

Bayer	γ (Regor) δ (Alsephina) κ (Markeb) λ (Suhail) μ ο φ (Tseen Ke) ψ
Variable	T W AH AI GP (X-1) GX GZ HU HX HY IM KQ MV (J) NX V378 V382 V390
HR	3294 (B) 3358 (A) 3407 (C) 3426 (e) 3445 (b) 3452 (n) 3477 (d) 3487 (a) 3497 3520 (g) 3570 3574 (H) 3591 (w) 3614 (c) 3682 (l) 3684 (k) 3753 (I) 3803 (N) 3819 (L) 3831 3836 (M) 3912 (m) 3990 (Q) 4023 (q) 4080 (r) 4134 4143 (t) 4167 (p) 4180 (x) 4293 (i)
HD	73526 74438 83443 (Kalausi) 85390 (Natasha) 85512 93385 300933
Other	DENIS J082303.1−491201 Gliese 367 (Añañuca) GJ 1132 Luhman 16 PSR J0855−4644 WASP-19

Exoplanets	Gliese 367 b (Tahay) c d GJ 1132 b HD 73526 b c HD 75289 b HD 85390 b HD 83443 b c WASP-19b

Star
clusters

NGC	2547 2659 3201 3228
Other	IC 2391 IC 2395 IC 2488 RCW 38 Trumpler 10

Nebulae

NGC	NGC 2626 NGC 2736 NGC 2792 NGC 2899 NGC 3132
Other	Gum 15 HH 46/47 RCW 34 Vela Supernova Remnant

Galaxies

NGC	3256

Galaxy clusters	Vela Supercluster