Lambda Leporis
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Lepus
Right ascension 05h 19m 34.52405s[1]
Declination −13° 10′ 36.4408″[1]
Apparent magnitude (V) +4.286±0.005[2]
Characteristics
Spectral type B0.5 V[2]
U−B color index −1.010±0.005[2]
B−V color index −0.273±0.015[2]
Astrometry
Radial velocity (Rv)+20.2±2.7[3] km/s
Proper motion (μ) RA: −3.30[1] mas/yr
Dec.: −4.91[1] mas/yr
Parallax (π)3.83 ± 0.24 mas[1]
Distance850 ± 50 ly
(260 ± 20 pc)
Absolute magnitude (MV)−2.77±0.15[2]
Details[2]
Mass15.0±3.5 M☉
Radius4.5±0.3 R☉
Luminosity15,488 L☉
Surface gravity (log g)4.30±0.05 cgs
Temperature30,400±300 K
Metallicity [Fe/H]−0.15 dex
Rotational velocity (v sin i)30±1 km/s
Age8±2[4] Myr
Other designations
λ Lep, 6 Lep, BD−13° 1127, HD 34816, HIP 24845, HR 1756, SAO 150340[5]
Database references
SIMBADdata

Lambda Leporis, which is the Latinized form of λ Leporis, is a solitary,[6] blue-white hued star in the southern constellation of Lepus. It is visible to the naked eye with an apparent visual magnitude of +4.29.[2] Based upon an annual parallax shift of 3.83 mas,[1] it is estimated to lie roughly 850 light years from the Sun. Relative to its neighbors, this star has a peculiar velocity of 16.3±2.8 km/s.[3] It is a member of the Orion OB1 association (Ori OB1),[7] and it has been identified as a high-velocity runaway star.[8]

This is a massive, B-type main-sequence star with a corrected stellar classification of B0.5 V. It is an estimated eight[4] million years old and is spinning with a projected rotational velocity of 30 km/s.[2] This star has around 15 times the mass of the Sun and 4.5 times the Sun's radius. It is radiating 15,488 times the Sun's luminosity from its photosphere at an effective temperature of 30,400 K.[2]

References

  1. 1 2 3 4 5 6 van Leeuwen, F. (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. 1 2 3 4 5 6 7 8 9 Nieva, M.-F. (February 2013), "Temperature, gravity, and bolometric correction scales for non-supergiant OB stars", Astronomy & Astrophysics, 550: A26, arXiv:1212.0928, Bibcode:2013A&A...550A..26N, doi:10.1051/0004-6361/201219677, S2CID 119275940.
  3. 1 2 Bobylev, V. V.; Bajkova, A. T. (August 2013), "Galactic kinematics from a sample of young massive stars", Astronomy Letters, 39 (8): 532–549, arXiv:1307.1677, Bibcode:2013AstL...39..532B, doi:10.1134/S106377371308001X, S2CID 118568203.
  4. 1 2 Tetzlaff, N.; et al. (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.
  5. ↑ "lam Lep". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-08-16.{{cite web}}: CS1 maint: postscript (link)
  6. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  7. ↑ Alexeeva, Sofya; et al. (June 2020), "Neon Abundances of B Stars in the Solar Neighborhood", The Astrophysical Journal, 896 (1): 59, arXiv:2005.11027, Bibcode:2020ApJ...896...59A, doi:10.3847/1538-4357/ab9306, S2CID 218862999, 59.
  8. ↑ Proffitt, Charles R.; Quigley, Mark F. (February 2001), "Boron Abundances in Early B Stars: Results from the B III Resonance Line in IUE Data", The Astrophysical Journal, 548 (1): 429–438, Bibcode:2001ApJ...548..429P, doi:10.1086/318673.
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