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HD 96146

HD 96146
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
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 mas/yr[1]
Dec.: +4.463 mas/yr[1]
Parallax (π)4.6163 ± 0.4323 mas[1]
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
85 G. Antliae[12], CD−35°6954, CPD−35°4592, FK5 2885, GC 15238, HD 96146, HIP 54173, HR 4313, SAO 202067, WDS J11049-3548AB[13]
Database references
SIMBADdata

HD 96146 (HR 4313) is a binary star[14] 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.[15]

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. ^ a b c d e f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN 0004-6361.
  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. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN 1562-6873. ISSN 1063-7737. S2CID 255204555.
  6. ^ a b Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (20 December 2021). "Stellar and substellar companions from Gaia EDR3". Astronomy & Astrophysics. 657: A7. arXiv:2109.10912. Bibcode:2022A&A...657A...7K. doi:10.1051/0004-6361/202142146. eISSN 1432-0746. ISSN 0004-6361.
  7. ^ a b Stassun, Keivan G.; et al. (9 September 2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694. Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467. eISSN 1538-3881.
  8. ^ a b c Zorec, J.; Royer, F. (January 2012). "Rotational velocities of A-type stars". Astronomy & Astrophysics. 537: A120. arXiv:1201.2052. Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691. eISSN 1432-0746. ISSN 0004-6361.
  9. ^ a b 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. arXiv:1904.11302. Bibcode:2019A&A...628A..94A. doi:10.1051/0004-6361/201935765. eISSN 1432-0746. ISSN 0004-6361.
  10. ^ a b Royer, F.; Gerbaldi, M.; Faraggiana, R.; Gómez, A. E. (January 2002). "Rotational velocities of A-type stars". Astronomy & Astrophysics. 381 (1): 105–121. arXiv:astro-ph/0110490. Bibcode:2002A&A...381..105R. doi:10.1051/0004-6361:20011422. eISSN 1432-0746. ISSN 0004-6361.
  11. ^ a b Grosbol, P. J. (June 1978). "Space velocities and ages of nearby early-type stars". Astronomy and Astrophysics Supplement Series. 32: 409–421. Bibcode:1978A&AS...32..409G. ISSN 0365-0138.
  12. ^ Gould, Benjamin Apthorp (1878). "Uranometria Argentina : brillantez y posicion de las estrellas fijas, hasta la septima magnitud, comprendidas dentro de cien grados del polo austral : con atlas". Resultados del Observatorio Nacional Argentino. 1. Bibcode:1879RNAO....1.....G.
  13. ^ "HD 96146". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved September 20, 2015.
  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. arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. eISSN 1365-2966. ISSN 0035-8711.
  15. ^ 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. arXiv:2005.05305. Bibcode:2020AJ....160....7T. doi:10.3847/1538-3881/ab91c1.
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