HD 88955
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Vela |
| Right ascension | 10h 14m 14 44.1579s[1] |
| Declination | −42° 07′ 18.9852″[1] |
| Apparent magnitude (V) | 3.85[2] |
| Characteristics | |
| Spectral type | A2 V[2] |
| B−V color index | +0.051±0.005[3] |
| Astrometry | |
| Radial velocity (Rv) | +7.4±2.7[4] km/s |
| Proper motion (μ) | RA: −151.532[1] mas/yr Dec.: +49.171[1] mas/yr |
| Parallax (π) | 32.7054 ± 0.3218 mas[1] |
| 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) | 4.08±0.14[6] cgs |
| Temperature | 9,451±321[6] K |
| Metallicity [Fe/H] | −0.02[7] dex |
| Rotational velocity (v sin i) | 100±4[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 32.7 mas,[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 (3.6±3.0)×10−7 M🜨 debris disc with a mean temperature of 138±21 K orbiting the host star at an average distance of 19.3±5.7 AU.[12]
References
- ^ a b c d e f 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. Gaia DR2 record for this source at VizieR.
- ^ a b c d 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.
- ^ a b 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, S2CID 119257644.
- ^ a b 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, S2CID 59451347, A61.
- ^ a b c d e f g h 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, S2CID 119241004, 171.
- ^ a b c 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, S2CID 33401607.
- ^ 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, S2CID 15059920.
- ^ a b 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, S2CID 119223132.
- ^ "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, S2CID 14878976.
- ^ 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, S2CID 118497872, 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.
