Astronomy:HD 143699

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Short description: Star in the constellation of Lupus
HD 143699
Location of HD 143699 (circled in red)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Lupus[1]
Right ascension  16h 03m 24.18956s[2]
Declination −38° 36′ 09.1424″[2]
Apparent magnitude (V) 4.90[1]
Characteristics
Evolutionary stage main sequence[3]
Spectral type B5/7 III/IV[4]
B−V color index −0.146±0.043[1]
Astrometry
Radial velocity (Rv)−1.9±2.8[1] km/s
Proper motion (μ) RA: −18.488[2] mas/yr
Dec.: −28.147[2] mas/yr
Parallax (π)9.2268 ± 0.4693[2] mas
Distance350 ± 20 ly
(108 ± 6 pc)
Absolute magnitude (MV)−0.54[1]
Details
Mass4.58[5] M☉
Radius3.89[6] R☉
Luminosity447[5] L☉
Surface gravity (log g)3.82[6] cgs
Temperature15,480[6] K
Rotation0.894 days[5]
Rotational velocity (v sin i)115[5] km/s
Age60[6] Myr
Other designations
CD−38°10832, FK5 3267, HD 143699, HIP 78655, HR 5967, SAO 207276[7]
Database references
SIMBADdata

HD 143699 is a single[8] star in the southern constellation of Lupus. It is a dim star but visible to the naked eye with an apparent visual magnitude of 4.90.[1] Based upon an annual parallax shift of 9.2 mas,[2] it is located around 350 light years away. It is most likely (90%[9] chance) a member of the Upper Centaurus–Lupus[10] subgroup of the Sco OB2 moving group.

This star has a stellar classification of B5/7 III/IV,[4] suggesting it is an evolving star that is entering the giant stage. However, according to Zorec and Royer (2012) it is only 56% of the way through its main sequence lifespan.[3] It is a chemically peculiar magnetic B star,[11] showing an averaged quadratic field strength of (167.2±140.4)×10−3 T.[12] Helium-weak, it displays an underabundance of helium in its spectrum.[13] Radio emissions have been detected from this source.[11]

HD 143699 has 4.6 times the mass of the Sun[5] and 3.9 times the Sun's radius.[6] It has a high rate of spin with a projected rotational velocity of 115 km/s, resulting in a short rotation period of 0.894 days.[5] The star is radiating 447 times the Sun's luminosity[5] from its photosphere at an effective temperature of 15,480 K.[6]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A  XHIP record for this object at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. 
  3. ↑ 3.0 3.1 Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics 537: A120, doi:10.1051/0004-6361/201117691, Bibcode: 2012A&A...537A.120Z. 
  4. ↑ 4.0 4.1 Houk, Nancy (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, 3, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode: 1982mcts.book.....H. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 Shultz, M. E.; Owocki, S. P.; Ud-Doula, A.; Biswas, A.; Bohlender, D.; Chandra, P.; Das, B.; David-Uraz, A. et al. (2022). "MOBSTER - VI. The crucial influence of rotation on the radio magnetospheres of hot stars". Monthly Notices of the Royal Astronomical Society 513 (1): 1429. doi:10.1093/mnras/stac136. Bibcode: 2022MNRAS.513.1429S. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 Glagolevskij, Yu. V. (2019). "On Properties of Main Sequence Magnetic Stars". Astrophysical Bulletin 74 (1): 66. doi:10.1134/S1990341319010073. Bibcode: 2019AstBu..74...66G. 
  7. ↑ "HD 143699". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+143699. 
  8. ↑ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society 389 (2): 869, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  9. ↑ Rizzuto, Aaron et al. (October 2011), "Multidimensional Bayesian membership analysis of the Sco OB2 moving group", Monthly Notices of the Royal Astronomical Society 416 (4): 3108–17, doi:10.1111/j.1365-2966.2011.19256.x, Bibcode: 2011MNRAS.416.3108R. 
  10. ↑ Bobylev, V. V.; Bajkova, A. T. (September 2007), "Kinematics of the Scorpius–Centaurus OB association", Astronomy Letters 33 (9): 571–583, doi:10.1134/S1063773707090010, Bibcode: 2007AstL...33..571B. 
  11. ↑ 11.0 11.1 Linsky, Jeffrey L. et al. (July 1992), "Radio Emission from Chemically Peculiar Stars", Astrophysical Journal 393: 341, doi:10.1086/171509, Bibcode: 1992ApJ...393..341L. 
  12. ↑ Bychkov, V. D. et al. (2009), "Catalogue of averaged stellar effective magnetic fields - II. Re-discussion of chemically peculiar A and B stars", Monthly Notices of the Royal Astronomical Society 394 (3): 1338, doi:10.1111/j.1365-2966.2008.14227.x, Bibcode: 2009MNRAS.394.1338B. 
  13. ↑ Kilambi, Gopal C. et al. (June 1992), "Mid-ultraviolet and optical photometry of helium stars", Journal of Astrophysics and Astronomy 13 (2): 175–194, doi:10.1007/BF02702309, Bibcode: 1992JApA...13..175K 



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