HD 96146

In this article, we will explore the significant impact HD 96146 has had on various aspects of modern society. From its influence in the cultural field to its relevance in the scientific field, HD 96146 has left an indelible mark on the history of humanity. Over the decades, HD 96146 has been the subject of study and debate, arousing conflicting opinions and triggering important changes in the way we perceive the world around us. Through the detailed analysis of different perspectives and relevant events, this article aims to shed light on the significance of HD 96146 and its implications in contemporary society.

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 +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.