HD 88955
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Vela |
Right ascension | 09h 51m 44.15792s[1] |
Declination | −46° 32′ 18.9851″[1] |
Apparent magnitude (V) | 3.85[2] |
Characteristics | |
Spectral type | A2 V[2] |
B−V color index | ±0.005 +0.051[3] |
Astrometry | |
Radial velocity (Rv) | ±2.7 +7.4[4] km/s |
Proper motion (μ) | RA: −151.532[1] mas/yr Dec.: +49.171[1] mas/yr |
Parallax (π) | 32.7054 ± 0.3218[1] mas |
Distance | 99.7 ± 1.0 ly (30.6 ± 0.3 pc) |
Absolute magnitude (MV) | 1.39[3] |
Details | |
Mass | 2.17[5] M☉ |
Radius | 2.11[5] R☉ |
Luminosity | 23.24[5] L☉ |
Surface gravity (log g) | ±0.14 4.08[6] cgs |
Temperature | ±321 9,451[6] K |
Metallicity [Fe/H] | −0.02[7] dex |
Rotational velocity (v sin i) | ±4 100[8] km/s |
Age | 410[5] Myr |
Other designations | |
Database references | |
SIMBAD | data |
HD 88955 is a single,[10] white-hued star in the southern constellation of Vela. It can be viewed with the naked eye, having an apparent visual magnitude of 3.85.[2] The distance to HD 88955 can be determined from its annual parallax shift of mas, 32.7[1] which yields a separation of 100 light years from the Sun. It is moving further from the Earth with a heliocentric radial velocity of +7 km/s.[4] Bayesian analysis suggests HD 88955 is a member of the Argus Association,[11] a group of co-moving stars usually associated with the IC 2391 open cluster.
This is an A-type main-sequence star with a stellar classification of A2 V.[2] It is about 410[5] million years old with a projected rotational velocity of 100 km/s.[8] The star has 2.17[5] times the mass of the Sun and 2.11[5] times the Sun's radius. It is radiating 23[5] times the Sun's luminosity from its photosphere at an effective temperature of 9,451 K.[6] An infrared excess has been detected from HD 88955, which analysis suggests is a ±3.0)×10−7 M⊕ (3.6debris disc with a mean temperature of ±21 K orbiting the host star at an average distance of 138±5.7 AU. 19.3[12]
References
- 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 3 4 Malagnini, M. L.; Morossi, C. (November 1990), "Accurate absolute luminosities, effective temperatures, radii, masses and surface gravities for a selected sample of field stars", Astronomy and Astrophysics Supplement Series, 85 (3): 1015–1019, Bibcode:1990A&AS...85.1015M.
- 1 2 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.
- 1 2 de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, A61.
- 1 2 3 4 5 6 7 8 Gáspár, András; et al. (August 2016), "The Correlation between Metallicity and Debris Disk Mass", The Astrophysical Journal, 826 (2): 14, arXiv:1604.07403, Bibcode:2016ApJ...826..171G, doi:10.3847/0004-637X/826/2/171, 171.
- 1 2 3 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146.
- ↑ Saffe, C.; et al. (October 2008), "Spectroscopic metallicities of Vega-like stars", Astronomy and Astrophysics, 490 (1): 297–305, arXiv:0805.3936, Bibcode:2008A&A...490..297S, doi:10.1051/0004-6361:200810260.
- 1 2 Hales, Antonio S.; et al. (April 2017), "Atomic gas in debris discs", Monthly Notices of the Royal Astronomical Society, 466 (3): 3582–3593, arXiv:1612.05465, Bibcode:2017MNRAS.466.3582H, doi:10.1093/mnras/stw3274.
- ↑ "HD 85622". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-08-08.
- ↑ 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.
- ↑ Malo, Lison; et al. (January 2013), "Bayesian Analysis to Identify New Star Candidates in Nearby Young Stellar Kinematic Groups", The Astrophysical Journal, 762 (2): 50, arXiv:1209.2077, Bibcode:2013ApJ...762...88M, doi:10.1088/0004-637X/762/2/88, 88.
- ↑ Thureau, N. D.; et al. (2014), "An unbiased study of debris discs around A-type stars with Herschel", Monthly Notices of the Royal Astronomical Society, 445 (3): 2558, Bibcode:2014MNRAS.445.2558T, doi:10.1093/mnras/stu1864.