Astronomy:HD 90132

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Short description: Solitary White-hued star and high proper motion star
HD 90132
Antlia constellation map.svg
Red circle.svg
Location of HD 90132 in red
Observation data
Epoch J2000.0   Equinox (celestial coordinates)
Constellation Antlia
Right ascension  10h 23m 29.29608s[1]
Declination −38° 00′ 35.4255″[1]
Apparent magnitude (V) 5.33±0.01[2]
Characteristics
Spectral type A8 V[3]
B−V color index +0.25[4]
Astrometry
Radial velocity (Rv)17±4.2[5] km/s
Proper motion (μ) RA: −158.833[1] mas/yr
Dec.: −53.705[1] mas/yr
Parallax (π)24.2034 ± 0.0725[1] mas
Distance134.8 ± 0.4 ly
(41.3 ± 0.1 pc)
Absolute magnitude (MV)+2.25[6]
Details
Mass1.69±0.27[7] M☉
Radius1.87±0.87[7] R☉
Luminosity9.79±0.06[8] L☉
Surface gravity (log g)4.15[9] cgs
Temperature7,737±263[9] K
Metallicity [Fe/H]−0.13[10] dex
Rotational velocity (v sin i)270[11] km/s
Age70[12] Myr
Other designations
CD−37°6509, CPD−37°4123, FK5 1269, GC 14281, HD 90132, HIP 50888, HR 4086, SAO 201346[13]
Database references
SIMBADdata

HD 90132 (HR 4086) is a solitary[14] white hued star located in the southern constellation Antlia. It has an apparent magnitude of 5.33,[2] making it one of the brighter members of this generally faint constellation. The star is relatively close at a distance of 135 light years[1] but is receding with a heliocentric radial velocity of 17 km/s.[5]

HD 90132 has a stellar classification of A8 V,[3] indicating that it is an ordinary A-type main-sequence star. At present it has 1.69 times the mass of the Sun and 1.87 times the radius of the Sun.[7] Despite a young age of 70 million years,[12] the star has a lower surface gravity than expected.[9] This is due to the equator being 18% larger than the poles,[15] which is due to a high projected rotational velocity of 270 km/s.[11] Nevertheless, it shines with a luminosity of 9.8 solar luminosity[8] from its photosphere at an effective temperature of 7,737 K.[9] HD 90132 is slightly metal deficient with a metallicity 74% that of Sun.[10]

This star was observed for infrared excess suggesting the presence of a circumstellar disk, but as of 2017 no excess have been found.[16]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G.  Gaia EDR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. ISSN 0004-6361. Bibcode: 2000A&A...355L..27H. 
  3. ↑ 3.0 3.1 Houk, N. (1982). Michigan Catalogue of Two-dimensional Spectral Types for the HD stars. Volume_3. Declinations −40° to −26°. Bibcode: 1982mcts.book.....H. 
  4. ↑ Johnson, H. L.; Mitchell, R. I.; Iriarte, B.; Wisniewski, W. Z. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory 4: 99–110. Bibcode: 1966CoLPL...4...99J. 
  5. ↑ 5.0 5.1 Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. ISSN 1063-7737. Bibcode: 2006AstL...32..759G. 
  6. ↑ Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331–346. doi:10.1134/S1063773712050015. ISSN 1063-7737. Bibcode: 2012AstL...38..331A. 
  7. ↑ 7.0 7.1 7.2 Stassun, Keivan G. et al. (9 September 2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal 158 (4): 138. doi:10.3847/1538-3881/ab3467. ISSN 0004-6256. Bibcode: 2019AJ....158..138S. 
  8. ↑ 8.0 8.1 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.  Gaia DR2 record for this source at VizieR.
  9. ↑ 9.0 9.1 9.2 9.3 David, Trevor J.; Hillenbrand, Lynne A. (12 May 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. doi:10.1088/0004-637X/804/2/146. Bibcode: 2015ApJ...804..146D. 
  10. ↑ 10.0 10.1 Netopil, Martin (4 May 2017). "Metallicity calibrations for dwarf stars and giants in the Geneva photometric system". Monthly Notices of the Royal Astronomical Society 469 (3): 3042–3055. doi:10.1093/mnras/stx1077. ISSN 0035-8711. Bibcode: 2017MNRAS.469.3042N. 
  11. ↑ 11.0 11.1 Huang, Su-Shu (September 1953). "A Statistical Study of the Rotation of the Stars.". The Astrophysical Journal 118: 285. doi:10.1086/145751. ISSN 0004-637X. Bibcode: 1953ApJ...118..285H. 
  12. ↑ 12.0 12.1 Vican, Laura (2 May 2012). "Age Determination for 346 Nearby Stars in the Herschel DEBRIS Survey". The Astronomical Journal 143 (6): 135. doi:10.1088/0004-6256/143/6/135. ISSN 0004-6256. Bibcode: 2012AJ....143..135V. 
  13. ↑ "HD 90132". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+90132. 
  14. ↑ Eggleton, P. P.; Tokovinin, A. A. (11 September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society 389 (2): 869–879. doi:10.1111/j.1365-2966.2008.13596.x. ISSN 0035-8711. Bibcode: 2008MNRAS.389..869E. 
  15. ↑ van Belle, Gerard T. (14 March 2012). "Interferometric observations of rapidly rotating stars". The Astronomy and Astrophysics Review 20 (1): 51. doi:10.1007/s00159-012-0051-2. ISSN 0935-4956. Bibcode: 2012A&ARv..20...51V. 
  16. ↑ Meshkat, Tiffany; Mawet, Dimitri; Bryan, Marta L.; Hinkley, Sasha; Bowler, Brendan P.; Stapelfeldt, Karl R.; Batygin, Konstantin; Padgett, Deborah et al. (21 November 2017). "A Direct Imaging Survey ofSpitzer-detected Debris Disks: Occurrence of Giant Planets in Dusty Systems". The Astronomical Journal 154 (6): 245. doi:10.3847/1538-3881/aa8e9a. Bibcode: 2017AJ....154..245M. 
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