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
Mass 4.2  M☉
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]

Related Research Articles

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HR 7703 is a binary star system in the constellation of Sagittarius. The brighter component has an apparent visual magnitude of 5.31, which means it is visible from suburban skies at night. The two stars are separated by an angle of 7.10″, which corresponds to an estimated semimajor axis of 56.30 AU for their orbit.

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<span class="mw-page-title-main">14 Aurigae</span> Quadruple star system in the constellation Auriga

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<span class="mw-page-title-main">28 Cancri</span> Binary star in the constellation Cancer

28 Cancri is a star system in the zodiac constellation of Cancer. It is a variable star with the designation CX Cancri, and is close to the lower limit of visibility with the naked eye, having a mean apparent visual magnitude of 6.05. The annual parallax shift seen from Earth's orbit is 8.5 mas, which provides a distance estimate of about 384 light years. It is moving away from the Sun with a radial velocity of around +9 km/s.

66 Cancri is a binary star system near the northern border of the zodiac constellation of Cancer, located 474 light years away from the Sun. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.87. The pair are moving closer to the Earth with a heliocentric radial velocity of −13 light years. As of 2003, the magnitude 8.56 companion was located at an angular separation of 4.43″ along a position angle of 134° from the primary.

<span class="mw-page-title-main">Beta Crateris</span> Binary star system in the constellation Crater

Beta Crateris, Latinized from β Crateris, is a binary star system in the southern constellation of Crater. It is visible to the naked eye with an apparent visual magnitude of 4.46. Based upon an annual parallax shift of 9.59 mas as seen from Earth, it is located around 340 light years from the Sun.

Gliese 412 is a pair of stars that share a common proper motion through space and are thought to form a binary star system. The pair have an angular separation of 31.4″ at a position angle of 126.1°. They are located 15.8 light-years distant from the Sun in the constellation Ursa Major. Both components are relatively dim red dwarf stars.

Gliese 86 is a K-type main-sequence star approximately 35 light-years away in the constellation of Eridanus. It has been confirmed that a white dwarf orbits the primary star. In 1998 the European Southern Observatory announced that an extrasolar planet was orbiting the star.

HD 33564 is a single star with an exoplanetary companion in the northern constellation of Camelopardalis. It has an apparent visual magnitude of 5.08, which means it is a 5th magnitude star that is faintly visible to the naked eye. The system is located at a distance of 68 light years from the Sun based on parallax, and it is drifting closer with a radial velocity of −11 km/s. It is a candidate member of the Ursa Major Moving Group.

<span class="mw-page-title-main">Zeta Cygni</span> Star in the constellation Cygnus

Zeta Cygni is a binary star system in the northern constellation of Cygnus, the swan. It has an apparent visual magnitude of 3.26 and, based upon parallax measurements, is about 143 light-years away.

HD 81817 is a possible binary star system with two brown dwarf companions in the northern circumpolar constellation of Draco. It has an orange hue and is visible to the naked eye with an apparent visual magnitude of 4.28. The system is located at a distance of approximately 990 light years from the Sun based on parallax, and is drifting closer with a radial velocity of −7 km/s. It is a member of the IC 2391 moving group.

<span class="mw-page-title-main">18 Draconis</span> Star in the constellation Draco

18 Draconis is a likely binary star system in the northern circumpolar constellation of Draco. With an apparent visual magnitude of 4.84, it is just bright enough to be faintly visible to the naked eye. The distance to this system, as estimated from an annual parallax shift of 4.5 mas, is roughly 720 light years. It is moving closer to the Sun with a heliocentric radial velocity of −1.4 km/s, and is a probable member of the Sirius stream of co-moving stars.

<span class="mw-page-title-main">7 Vulpeculae</span> Star in the constellation Vulpecula

7 Vulpeculae is a binary star system approximately 910 light years away in the slightly northern constellation of Vulpecula. It is a challenge to view with the naked eye, having an apparent visual magnitude of 6.3. The system currently has a heliocentric radial velocity of −38 km/s.

Theta Hydrae, Latinized from θ Hydrae, is a binary star system in the constellation Hydra. It is visible to the naked eye with an apparent visual magnitude of 3.9. The star system has a high proper motion with an annual parallax shift of 28.4 mas, indicating a distance of about 115 light years. Theta Hydrae forms a double with a magnitude 9.9 star located at an angular separation of 29 arcseconds.

56 Persei is at least a triple star and possibly a quadruple star system in the northern constellation of Perseus. It is visible to the naked eye as a dim point of light with a combined apparent visual magnitude of 5.77. The system is located 139 light-years (42.5 pc) distant from the Sun based on parallax, but is drifting closer with a radial velocity of −32 km/s.

HD 128429 is a binary star system located at a distance of 88 light years from the Sun in the southern zodiac constellation of Libra. It has a yellow-white hue and is just barely visible to the naked eye with an apparent visual magnitude of 6.20. The system is drifting closer to the Sun with a radial velocity of −66 km/s and has a high proper motion, traversing the celestial sphere at the rate of 0.945″ per year. It is a well-known high velocity star system with a net heliocentric velocity of 158.8 km/s. The system is orbiting the through the galaxy with a high eccentricity of 0.62, which carries it from as close as 4.1 out to 17.5 kpc away from the Galactic Center.

HD 60803 is a binary star system in the equatorial constellation of Canis Minor, located less than a degree to the northwest of the prominent star Procyon. It has a yellow hue and is visible to the naked eye as a dim point of light with a combined apparent visual magnitude of 5.904. The distance to this system is 135 light years as determined using parallax measurements, and is drifting further away with a radial velocity of +4.6 km/s.

HD 44120 is a wide binary star system in the southern constellation of Pictor. Although visible to the naked eye, it is a challenge to view having an apparent visual magnitude of 6.44. The system is located at a distance of 118 light years from the Sun based on parallax, but it is drifting closer with a radial velocity of −2 km/s. It has an absolute magnitude of 3.57.

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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