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HD 88955

From Wikipedia, the free encyclopedia

This article is about q Velorum. For Q Velorum, see HD 88206.
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]
Distance99.7 ± 1.0 ly
(30.6 ± 0.3 pc)
Absolute magnitude (MV)1.39[3]
Details
Mass2.17[5] M☉
Radius2.11[5] R☉
Luminosity23.24[5] L☉
Surface gravity (log g)4.08±0.14[6] cgs
Temperature9,451±321[6] K
Metallicity [Fe/H]−0.02[7] dex
Rotational velocity (v sin i)100±4[8] km/s
Age410[5] Myr
Other designations
q Velorum, CD−41° 5713, FK5 382, GC 14076, HD 88955, HIP 50191, HR 4023, SAO 221895[9]
Database references
SIMBADdata

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

  1. ^ 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.
  2. ^ 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.
  3. ^ 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.
  4. ^ 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.
  5. ^ 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.
  6. ^ 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.
  7. ^ 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.
  8. ^ 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.
  9. ^ "HD 85622". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-08-08.
  10. ^ 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.
  11. ^ 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.
  12. ^ 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, hdl:10023/6011.
This page was last edited on 5 January 2024, at 08:04
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