HD 96146

Last updated
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]
Distance 710 ± 70  ly
(220 ± 20  pc)
Absolute magnitude  (MV)−0.55 [5]
Details
Mass 3.84 [6]   M☉
Radius 6.17 [7]   R☉
Luminosity 218+47
−37 [8]   L☉
Surface gravity (log g)3.46 [9]   cgs
Temperature 9,750+113
−112 [8]   K
Metallicity [Fe/H]+0.07 [9]   dex
Rotational velocity (v sin i)10±1 [10]  km/s
Age 291+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
SIMBAD data

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]

Related Research Articles

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<span class="mw-page-title-main">HD 26764</span> Star in the constellation Camelopardalis

HD 26764, also known as HR 1314 or rarely 14 H. Camelopardalis, is a solitary white hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.19, making it faintly to the naked eye if viewed under good conditions. Gaia DR3 parallax measurements place the object at a distance of 266 light years and is drifting closer with a poorly constrained heliocentric radial velocity of 3 km/s. At its current distance, HD 26764's brightness is diminished by 0.26 magnitudes due to interstellar dust.

HD 29559 is a solitary star in the southern constellation Caelum. It has an apparent magnitude of 6.40, placing it near the max naked eye visibility. The star is situated at a distance 408 light years based on parallax measurements but is receding with a heliocentric radial velocity of 24.2 km/s.

<span class="mw-page-title-main">Eta Octantis</span> Star in the constellation of Octans

Eta Octantis, Latinized from η Octantis, is a solitary star located in the southern circumpolar constellation Octans. It has an apparent magnitude of 6.19, making it faintly visible to the naked eye. The object is situated at a distance of 358 light years but is approaching the Solar System with a heliocentric radial velocity of −1.7 km/s.

<span class="mw-page-title-main">HD 27022</span> Star in the constellation Camelopardalis

HD 27022, also known as HR 1327, is a star located in the northern circumpolar constellation Camelopardalis. The object has also been designated as 20 H. Camelopardalis, but is not commonly used in modern times. It has an apparent magnitude of 5.27, allowing it to be faintly visible to the naked eye. Based on parallax measurements from Gaia DR3, the star has been estimated to be 347 light years away. It appears to be approaching the Solar System, having a heliocentric radial velocity of −19.5 km/s.

13 Delphini is a binary star in the equatorial constellation Delphinus, with a combined apparent magnitude of 5.64. The system is located at a distance of 471 light years but is approaching the Solar System with a heliocentric radial velocity of about −7 km/s.

HD 75171, also known as HR 3495, is a solitary, white hued star located in the southern constellation of Volans. It has an apparent magnitude of 6.02, making it faintly visible to the naked eye under ideal conditions. The object is relatively close at a distance of 191 light years but is receding with a heliocentric radial velocity of 10.7 km/s. Eggen (1995) lists it as a probable member of the Hyades Supercluster.

<span class="mw-page-title-main">CW Octantis</span> Star in the constellation of Octans

CW Octantis, also known as HD 148542, is a solitary, white hued variable star located in the southern circumpolar constellation Octans. It has an apparent magnitude of 6.03, allowing it to be faintly visible to the naked eye. Parallax measurements from Gaia DR3 place the object at a distance of 629 light years. It appears to be receding from the Solar System with a heliocentric radial velocity of 7.1 km/s.

HD 31529, also known as HR 1584, is a solitary, orange hued star located in the southern constellation Caelum, the chisel. It has an apparent magnitude of 6.09, making it faintly visible to the naked eye if viewed under ideal conditions. This object is located relatively far at a distance of 932 light years based on parallax measurements from Gaia DR3, but is receding with a heliocentric radial velocity of 28.4 km/s. Eggen (1989) lists it as a member of the old disk population.

HD 32820, also known as HR 1651, is a yellowish-white hued star located in the southern constellation Caelum, the chisel. It has an apparent magnitude of 6.3, placing it near the limit of naked eye visibility. The object is located relatively close at a distance of 103 light years based on parallax measurements from Gaia DR3, but is receding with a heliocentric radial velocity of 29.8 km/s.

HD 26670, also known as HR 1305, is a star located in the northern circumpolar constellation of Camelopardalis, the giraffe. The object has been designated as 26 H. Camelopardalis, but is not commonly used in modern times. It has an apparent magnitude of 5.70, allowing it to be faintly visible to the naked eye. Based on parallax measurements from Gaia DR3, the object is estimated to be 491 light years away from the Solar System. It appears to be slowly receding with a heliocentric radial velocity of 0.4 km/s.

<span class="mw-page-title-main">HD 31134</span> Star in the constellation of Camelopardalis

HD 31134, also designated as HR 1561, is a solitary star located in the northern circumpolar constellation Camelopardalis, the giraffe. It is faintly visible to the naked eye as a white-hued star with an apparent magnitude of 5.74. Gaia DR3 parallax measurements place it 473 light years away. It appears to be approaching the Solar System with a heliocentric radial velocity of −15.1 km/s. At its current distance, HD 31134's brightness is diminished by 0.35 magnitudes due to interstellar dust. It has an absolute magnitude of +0.19.

<span class="mw-page-title-main">HD 174500</span> Star in the constellation of Telescopium

HD 174500, also designated as HR 7097 or rarely 34 G. Telescopii, is a solitary white-hued star located in the southern constellation Telescopium. It has an apparent magnitude of 6.16, placing it near the limit for naked eye visibility. Gaia DR3 parallax measurements place the object 692 light years away, and it is currently receding with a heliocentric radial velocity of 35 km/s. At its current distance, HD 174500's brightness is diminished by 0.39 magnitudes due to interstellar dust. It has an absolute magnitude of −0.82.

<span class="mw-page-title-main">HD 170384</span> A-type dwarf; Corona Australis

HD 170384, also known as HR 6931 or rarely 11 G. Coronae Australis, is a solitary white-hued star located in the southern constellation Corona Australis. It has an apparent magnitude of 6.02, making it barely visible to the naked eye, even under ideal conditions. The object is located relatively close at a distance of 229.1 light-years based on Gaia DR3 parallax measurements and it is drifting closer with a heliocentric radial velocity of −11.4 km/s. At its current distance, HD 170384's brightness is diminished by interstellar extinction of 0.28 magnitudes and it has an absolute magnitude of +1.86.

<span class="mw-page-title-main">HD 27322</span> A-type dwarf; Camelopardalis

HD 27322, also known as HR 1342, is a binary star located in the northern circumpolar constellation Camelopardalis. The visible component is faintly visible to the naked eye as a white-hued point of light with an apparent magnitude of 5.92. The object is located relatively close at a distance of 313 light-years based on Gaia DR3 parallax measurements, and it is drifting closer with a heliocentric radial velocity of approximately −13 km/s. At its current distance, HD 27322's brightness is diminished by 0.24 magnitudes due to interstellar extinction and it has an absolute magnitude of +0.98.

<span class="mw-page-title-main">HD 28780</span> A-type star in the constellation Camelopardalis

HD 28780, also known as HR 1440, is a solitary white-hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.91, making it faintly viisble to the naked eye under ideal conditions. Gaia DR3 parallax measurements imply a distance of 488 light-years, and it is currently drifting closer with a heliocentric radial velocity of −22.6 km/s. At its current distance, HD 28780's brightness is diminished by 0.33 magnitudes due to interstellar extinction and it has an absolute magnitude of +0.26.

<span class="mw-page-title-main">HD 4222</span> Binary star; Cassiopeia constellation

HD 4222, also known as HR 196, is the primary of a binary star located in the northern constellation Cassiopeia. It is faintly visible to the naked eye as a white-hued point of light with an apparent magnitude of 5.41. Gaia DR3 parallax measurements imply a distance of 353 light-years and it is drifting closer with a heliocentric radial velocity of −8.5 km/s. At its current distance, HD 4222's brightness is diminished by an interstellar extinction of 0.13 magnitudes and it has an absolute magnitude of +0.44.

<span class="mw-page-title-main">HD 10390</span> B-type main-sequence star; Triangulum

HD 10390 is a solitary star located in the northern constellation Triangulum. It is faintly visible to the naked eye as a bluish-white hued point of light with an apparent magnitude of 5.64. The object is located relatively close at a distance of 292 light-years based on Gaia DR3 parallax measurements and it is drifting closer with a heliocentric radial velocity of −1.9 km/s. At its current distance, HD 10390's brightness is diminished by an interstellar extinction of only five-hundredths of a magnitude and it has an absolute magnitude of +1.00.

References

  1. 1 2 3 4 5 6 7 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. 1 2 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. 1 2 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. 1 2 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. 1 2 3 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. 1 2 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. 1 2 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. 1 2 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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