HR 3643

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HR 3643
Observation data
Epoch J2000        Equinox J2000
Constellation Carina
Right ascension 09h 05m 08.81309s [1]
Declination −72° 36′ 09.7437″ [1]
Apparent magnitude  (V)4.48 + 14.50 [2]
Characteristics
Spectral type F8II [3] + DA1.6 [2]
B−V color index +0.607±0.010 [4]
Astrometry
Radial velocity (Rv)+22.5±0.7 [5]  km/s
Proper motion (μ)RA: −8.81 [1]   mas/yr
Dec.: −5.26 [1]   mas/yr
Parallax (π)8.14 ± 0.15  mas [1]
Distance 401 ± 7  ly
(123 ± 2  pc)
Absolute magnitude  (MV)−0.98 [4]
Details
A
Radius 13.15+1.03
−0.53 [6]   R☉
Luminosity 206.2±5.4 [6]   L☉
Temperature 6,030+127
−222 [6]   K
Metallicity [Fe/H]−0.04±0.04 [4]   dex
Rotational velocity (v sin i)53 [7]  km/s
B
Mass 0.74 [2]   M☉
Surface gravity (log g)7.47 [8]   cgs
Temperature 21,551 [8]   K
Age 25 [8]   Myr
Other designations
G Car, CPD−72°779, FK5  2720, GC  12595, HD  78791, HIP  44599, HR  3643, SAO  256582, WDS J17039+1941, WD  0905-724 [9]
Database references
SIMBAD data

HR 3643 is a binary star [2] [7] system in the southern constellation of Carina. It has the Bayer designation G Carinae, with HR 3643 being the star's designation in the Bright Star Catalogue . The system is visible to the naked eye with an apparent visual magnitude of 4.48. [2] It is located at a distance of approximately 401  light years from the Sun based on parallax, [1] and is drifting further away with a radial velocity of +22.5 km/s. [5]

The binary nature of this system was first detected as an ultraviolet excess in 1996. No radial velocity variation has been detected so it must be a wide system with an orbital period of up to 21 years. [10] The estimated semimajor axis of their orbit is 10.90  AU . [2] The pair were not resolved using the Hubble Space Telescope WFPC2 instrument. [10]

The primary is an evolved bright giant star with a yellow-white hue and a stellar classification of F8II. [3] With the supply of hydrogen exhausted at its core, it has expanded to 13 [6] times the Sun's radius. It has a relatively high projected rotational velocity of 53 km/s for a star of this class, suggesting it is an intermediate-mass star with 2–5 times the mass of the Sun. [7] The star is radiating 206 [6] times the luminosity of the Sun from its photosphere at an effective temperature of 6,030 K. [6]

The magnitude 14.50 [2] companion is a white dwarf with a class of DA1.6. [2] It has a mass estimated at 74% [2] of the mass of the Sun and a temperature of 21,551 K, indicating a cooling time of 25 million years. [8] This object is a source for hard X-ray emission. [11] The primary is one of the most massive stars known to have a white dwarf companion. [7]

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HD 136138, or HR 5692, is a binary star system in the Serpens Caput segment of the Serpens constellation. It has a golden hue like the Sun and is dimly visible to the naked eye with an apparent visual magnitude of 5.68; the light contribution from the companion is effectively negligible. This system is located at a distance of approximately 420 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −7.7 km/s and has a proper motion of 23.5 mas·yr−1.

References

  1. 1 2 3 4 5 6 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv: 0708.1752 , Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID   18759600.
  2. 1 2 3 4 5 6 7 8 9 Holberg, J. B.; et al. (2013), "Where are all the Sirius-like binary systems?", Monthly Notices of the Royal Astronomical Society, 435 (3): 2077, arXiv: 1307.8047 , Bibcode:2013MNRAS.435.2077H, doi: 10.1093/mnras/stt1433 .
  3. 1 2 Skiff, B. A. (October 2014), "Catalogue of Stellar Spectral Classifications", VizieR On-line Data Catalog: B/mk. Originally published in: Lowell Observatory (October 2014), Bibcode:2014yCat....1.2023S.
  4. 1 2 3 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971 , Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID   119257644.
  5. 1 2 Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv: 1606.08053 , Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065, S2CID   119231169.
  6. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  7. 1 2 3 4 Landsman, Wayne; et al. (March 1996), "The White-Dwarf Companions of 56 Persei and HR 3643", Publications of the Astronomical Society of the Pacific, 108: 250, arXiv: astro-ph/9512117 , Bibcode:1996PASP..108..250L, doi:10.1086/133718, S2CID   14398914.
  8. 1 2 3 4 Barstow, M. A.; et al. (May 2014), "Evidence for an external origin of heavy elements in hot DA white dwarfs", Monthly Notices of the Royal Astronomical Society, 440 (2): 1607–1625, arXiv: 1402.2164 , Bibcode:2014MNRAS.440.1607B, doi: 10.1093/mnras/stu216 .
  9. ↑ "G Car". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-12-11.
  10. 1 2 Barstow, M. A.; et al. (April 2001), "Resolving Sirius-like binaries with the Hubble Space Telescope", Monthly Notices of the Royal Astronomical Society , 322 (4): 891–900, arXiv: astro-ph/0010645 , Bibcode:2001MNRAS.322..891B, doi: 10.1046/j.1365-8711.2001.04203.x , S2CID   12232120.
  11. ↑ Bilíková, Jana; et al. (November 2010), "Hard X-ray Emission Associated with White Dwarfs. III", The Astronomical Journal, 140 (5): 1433–1443, Bibcode:2010AJ....140.1433B, doi: 10.1088/0004-6256/140/5/1433 .
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