HD 143699
  | |
| Observation data Epoch J2000 Equinox 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 mas[2] |
| Distance | 350 ± 20 ly (108 ± 6 pc) |
| Absolute magnitude (MV) | −0.54[1] |
| Details | |
| Mass | 4.58[5] M☉ |
| Radius | 3.89[6] R☉ |
| Luminosity | 447[5] L☉ |
| Surface gravity (log g) | 3.82[6] cgs |
| Temperature | 15,480[6] K |
| Rotation | 0.894 days[5] |
| Rotational velocity (v sin i) | 115[5] km/s |
| Age | 60[6] Myr |
| Other designations | |
| CD−38°10832, FK5 3267, HD 143699, HIP 78655, HR 5967, SAO 207276[7] | |
| Database references | |
| SIMBAD | data |
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
[edit]- 1 2 3 4 5 6 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. XHIP record for this object at VizieR.
- 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051.
- 1 2 Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
- 1 2 Houk, Nancy (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 3, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode:1982mcts.book.....H.
- 1 2 3 4 5 6 7 Shultz, M. E.; Owocki, S. P.; Ud-Doula, A.; Biswas, A.; Bohlender, D.; Chandra, P.; Das, B.; David-Uraz, A.; Khalack, V.; Kochukhov, O.; Landstreet, J. D.; Leto, P.; Monin, D.; Neiner, C.; Rivinius, Th; Wade, G. A. (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. arXiv:2201.05512. Bibcode:2022MNRAS.513.1429S. doi:10.1093/mnras/stac136.
- 1 2 3 4 5 6 Glagolevskij, Yu. V. (2019). "On Properties of Main Sequence Magnetic Stars". Astrophysical Bulletin. 74 (1): 66. Bibcode:2019AstBu..74...66G. doi:10.1134/S1990341319010073.
- ↑ "HD 143699". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-29.
- ↑ 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, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ↑ 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, arXiv:1106.2857, Bibcode:2011MNRAS.416.3108R, doi:10.1111/j.1365-2966.2011.19256.x, S2CID 54510608.
- ↑ Bobylev, V. V.; Bajkova, A. T. (September 2007), "Kinematics of the Scorpius–Centaurus OB association", Astronomy Letters, 33 (9): 571–583, arXiv:0708.0943, Bibcode:2007AstL...33..571B, doi:10.1134/S1063773707090010, S2CID 15785349.
- 1 2 Linsky, Jeffrey L.; et al. (July 1992), "Radio Emission from Chemically Peculiar Stars", Astrophysical Journal, 393: 341, Bibcode:1992ApJ...393..341L, doi:10.1086/171509.
- ↑ 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, Bibcode:2009MNRAS.394.1338B, doi:10.1111/j.1365-2966.2008.14227.x, S2CID 120268049.
- ↑ Kilambi, Gopal C.; et al. (June 1992), "Mid-ultraviolet and optical photometry of helium stars", Journal of Astrophysics and Astronomy, 13 (2): 175–194, Bibcode:1992JApA...13..175K, doi:10.1007/BF02702309, S2CID 119896529
