Astronomy:HD 96146

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Short description: Binary star in the constellation Antlia
HD 96146
Observation data
Epoch J2000.0   Equinox (celestial coordinates)
Constellation Antlia
Right ascension  11h 04m 54.1966s[1]
Declination −35° 48′ 16.817″[1]
Apparent magnitude (V) 5.41±0.01[2]
Characteristics
Spectral type A0 V[3]
B−V color index +0.03[4]
Astrometry
Radial velocity (Rv)−4.66±6.09[1] km/s
Proper motion (μ) RA: −24.217[1] mas/yr
Dec.: +4.463[1] mas/yr
Parallax (π)4.6163 ± 0.4323[1] mas
Distance710 ± 70 ly
(220 ± 20 pc)
Absolute magnitude (MV)−0.55[5]
Details
Mass3.84[6] M☉
Radius6.17[7] R☉
Luminosity218+47−37[8] L☉
Surface gravity (log g)3.46[9] cgs
Temperature9,750+113−112[8] K
Metallicity [Fe/H]+0.07[9] dex
Rotational velocity (v sin i)10±1[10] km/s
Age291+22−21[11] Myr
Other designations
CD−35°6954, CPD−35°4592, FK5 2885, GC 15238, HD 96146, HIP 54173, HR 4313, SAO 202067, WDS J11049-3548AB[12]
Database references
SIMBADdata

HD 96146 (HR 4313) is a binary star[13] located in the southern constellation Antlia. The system has a combined apparent magnitude of 5.41,[2] making it visible to the naked eye under ideal conditions. Parallax measurements from the Gaia spacecraft place the pair at a distance of 710 light years with a large margin of error. It is currently receding with a poorly constrained heliocentric radial velocity of 4.7 km/s.[1]

The object's status as a double star was not known until a 1991 Hipparcos survey of double stars. Since the pair's current projected separation is around 0.04 arcseconds, it makes it difficult to distinguish both components. Nevertheless, they are located along a position angle of 226°. The secondary has been observed using speckle interferometry to be 1.8 magnitudes fainter than the visible star.[14]

The primary has a stellar classification of A0 V, indicating that it is an ordinary A-type main-sequence star. Zorec and Royer (2012) model it as a dwarf star that is 99.5% through its main sequence lifetime, close to the subgiant phase. It has 3.84 times the mass of the Sun[6] and an enlarged radius of 6.17 R☉.[7] HD 96146 shines with a luminosity 220 times that of the Sun[8] from its photosphere at an effective temperature of 9,750 K, giving a white hue. HD 96146 is currently 291 million years old[11] and unlike most hot stars, spins modestly with a projected rotational velocity of only 10 km/s.[10]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 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. ↑ 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. ↑ 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. 
  6. ↑ 6.0 6.1 Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (20 December 2021). "Stellar and substellar companions from Gaia EDR3". Astronomy & Astrophysics 657: A7. doi:10.1051/0004-6361/202142146. ISSN 0004-6361. Bibcode: 2022A&A...657A...7K. 
  7. ↑ 7.0 7.1 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. Bibcode: 2019AJ....158..138S. 
  8. ↑ 8.0 8.1 8.2 Zorec, J.; Royer, F. (January 2012). "Rotational velocities of A-type stars". Astronomy & Astrophysics 537: A120. doi:10.1051/0004-6361/201117691. ISSN 0004-6361. Bibcode: 2012A&A...537A.120Z. 
  9. ↑ 9.0 9.1 Anders, F. et al. (August 2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy & Astrophysics 628: A94. doi:10.1051/0004-6361/201935765. ISSN 0004-6361. Bibcode: 2019A&A...628A..94A. 
  10. ↑ 10.0 10.1 Royer, F.; Gerbaldi, M.; Faraggiana, R.; Gómez, A. E. (January 2002). "Rotational velocities of A-type stars". Astronomy & Astrophysics 381 (1): 105–121. doi:10.1051/0004-6361:20011422. ISSN 0004-6361. Bibcode: 2002A&A...381..105R. 
  11. ↑ 11.0 11.1 Grosbol, P. J. (June 1978). "Space velocities and ages of nearby early-type stars.". Astronomy and Astrophysics Supplement Series 32: 409–421. ISSN 0365-0138. Bibcode: 1978A&AS...32..409G. 
  12. ↑ "HD 96146". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+96146. 
  13. ↑ 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. 
  14. ↑ Tokovinin, Andrei; Mason, Brian D.; Mendez, Rene A.; Costa, Edgardo; Horch, Elliott P. (2020). "Speckle Interferometry at SOAR in 2019". The Astronomical Journal 160 (1): 7. doi:10.3847/1538-3881/ab91c1. Bibcode: 2020AJ....160....7T. 
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