Astronomy:5 Aurigae

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Short description: Triple star system in the constellation Auriga
5 Aurigae
Observation data
Equinox J2000.0]] (ICRS)
Constellation Auriga
Right ascension  05h 00m 18.33887s[1]
Declination +39° 23′ 40.9241″[1]
Apparent magnitude (V) 5.95[2] (6.02 + 9.50)[3]
Characteristics
Spectral type F5 V[4]
U−B color index −0.03[5]
B−V color index +0.42[5]
Astrometry
Radial velocity (Rv)+6.0±1.3[6] km/s
Proper motion (μ) RA: −10.87[1] mas/yr
Dec.: −1.08[1] mas/yr
Parallax (π)16.74 ± 0.71[1] mas
Distance195 ± 8 ly
(60 ± 3 pc)
Absolute magnitude (MV)2.07[2]
Orbit[7]
Period (P)1,598.04±50.35 yr
Semi-major axis (a)5.379±0.388
Eccentricity (e)0.536±0.031
Inclination (i)56.1±0.8°
Longitude of the node (Ω)155.4±0.7°
Periastron epoch (T)3,242.73±8.96
Argument of periastron (ω)
(secondary)
333.4±4.5°
Details
5 Aur A
Mass1.48[8] or 1.70[7] M
Luminosity12.46[2] L
Surface gravity (log g)4.14[8] cgs
Temperature6,603±225[8] K
Metallicity [Fe/H]−0.02±0.07[9] dex
Age2.205[8] Gyr
5 Aur B
Mass0.82[7] M
Other designations
BD+39° 1133, GC 6084, HD 31761, HIP 23261, HR 1599, SAO 57559, PPM 69817, ADS 3589, CCDM J05003+3924, WDS J05003+3924, TYC 2899-369-1[10]
Database references
SIMBADdata

5 Aurigae is a triple star[7] system in the northern constellation of Auriga,[10] located about 195 light years away from the Sun based on parallax.[1] It is just visible to the naked eye as a dim, yellow-white hued star with an apparent visual magnitude of 5.95.[2] The system is moving away from the Earth with a heliocentric radial velocity of +6 km/s,[6] having come within 62.4 light-years some 8.7 million years ago.[2]

This was initially discovered to be a binary star system by Otto Struve. The outer pair has an orbital period of 1,598 years with an eccentricity of 0.536.[7] The magnitude 6.02[3] primary, component A, is itself a binary system consisting of two stars of similar mass, roughly 1.5 times the mass of the Sun each, with an orbital period of 8.08 years.[11] It has a stellar classification of F5 V,[4] matching an F-type main-sequence star.

As of 2017, component B is a magnitude 9.50 star at an angular separation of 4.10 from the primary along a position angle of 285°.[3]

References

  1. 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode2007A&A...474..653V. 
  2. 2.0 2.1 2.2 2.3 2.4 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode2012AstL...38..331A. 
  3. 3.0 3.1 3.2 Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal 122 (6): 3466. doi:10.1086/323920. Bibcode2001AJ....122.3466M.  Vizier catalog entry
  4. 4.0 4.1 Abt, Helmut A. (2008). "Visual Multiples. IX. MK Spectral Types". The Astrophysical Journal Supplement Series 176 (1): 216–217. doi:10.1086/525529. Bibcode2008ApJS..176..216A. 
  5. 5.0 5.1 Guetter, H. H. (1980). "UBV Photoelectric Photometry of 259 PZT Stars". Publications of the Astronomical Society of the Pacific 92: 215. doi:10.1086/130650. Bibcode1980PASP...92..215G. 
  6. 6.0 6.1 Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. Bibcode2006AstL...32..759G. 
  7. 7.0 7.1 7.2 7.3 7.4 Cvetkovic, Z.; Novakovic, B. (December 2006). "Orbits For Sixteen Binaries". Serbian Astronomical Journal 173 (173): 73–82. doi:10.2298/SAJ0673073C. Bibcode2006SerAJ.173...73C. 
  8. 8.0 8.1 8.2 8.3 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal 804 (2): 146, doi:10.1088/0004-637X/804/2/146, Bibcode2015ApJ...804..146D. 
  9. Gáspár, András et al. (2016). "The Correlation between Metallicity and Debris Disk Mass". The Astrophysical Journal 826 (2): 171. doi:10.3847/0004-637X/826/2/171. Bibcode2016ApJ...826..171G. 
  10. 10.0 10.1 "5 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=5+Aur. 
  11. Tokovinin, Andrei (2014). "From Binaries to Multiples. Ii. Hierarchical Multiplicity of F and G Dwarfs". The Astronomical Journal 147 (4): 87. doi:10.1088/0004-6256/147/4/87. Bibcode2014AJ....147...87T. 

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