Psi6 Aurigae, Latinized from ψ6 Aurigae, is a spectroscopic binary[5] star in the northern constellation of Auriga. It is a dim, naked eye star with an apparent visual magnitude of +5.22.[2] Based upon a measured annual parallax shift of 9.05 ± 0.38 mas,[1] it is approximately 360 light-years (110 parsecs) distant from the Earth.
  | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Auriga |
| Right ascension | 06h 47m 39.57703s[1] |
| Declination | +48° 47′ 22.1222″[1] |
| Apparent magnitude (V) | +5.22[2] |
| Characteristics | |
| Spectral type | K0.5 III[1] |
| U−B color index | +1.04[2] |
| B−V color index | +1.11[2] |
| Astrometry | |
| Radial velocity (Rv) | −6.51±0.30[3] km/s |
| Proper motion (μ) | RA: −4.32[1] mas/yr Dec.: +7.19[1] mas/yr |
| Parallax (π) | 9.05 ± 0.38 mas[1] |
| Distance | 360 ± 20 ly (110 ± 5 pc) |
| Absolute magnitude (MV) | +0.01[4] |
| Orbit[5] | |
| Period (P) | 5,996±26 d |
| Eccentricity (e) | 0.044±0.014 |
| Periastron epoch (T) | 52556 ± 310 MJD |
| Argument of periastron (ω) (secondary) | 222±19° |
| Semi-amplitude (K1) (primary) | 3.24±0.04 km/s |
| Details[6] | |
| ψ6 Aur A | |
| Mass | 2.02±0.28 M☉ |
| Radius | 17.72±0.76 R☉ |
| Luminosity | 123.4±10.2 L☉ |
| Surface gravity (log g) | 2.25±0.07 cgs |
| Temperature | 4,574±26 K |
| Metallicity [Fe/H] | −0.08±0.10 dex |
| Rotational velocity (v sin i) | +10[7] km/s |
| Age | 1.55±0.67 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
This is a single-lined spectroscopic binary star system with an orbital period of 5,996 days (16.4 years) and an eccentricity of 0.044.[5] The visible component is a K-type giant star with a stellar classification of K0.5 III.[1] It is most likely (78% chance) on the red giant branch and is around 1.55 billion years old. As such, it has an estimated double the mass of the Sun and about 18 times the Sun's radius. The star is radiating about 123 times the Sun's luminosity from its photosphere at an effective temperature of 4,574 K.[6]
See also
editReferences
edit- ^ a b c d e f g h 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.
- ^ a b c d Argue, A. N. (1966), "UBV photometry of 550 F, G and K type stars", Monthly Notices of the Royal Astronomical Society, 133 (4): 475–493, Bibcode:1966MNRAS.133..475A, doi:10.1093/mnras/133.4.475.
- ^ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
- ^ 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.
- ^ a b c Griffin, R. F. (February 2010), "Spectroscopic binary orbits from photoelectric radial velocities - Paper 210: Psi2 Aurigae and 34 Pegasi", The Observatory, 130 (1): 17–32, Bibcode:2010Obs...130...17G.
- ^ a b Reffert, Sabine; et al. (2015), "Precise radial velocities of giant stars. VII. Occurrence rate of giant extrasolar planets as a function of mass and metallicity", Astronomy & Astrophysics, 574: A116, arXiv:1412.4634, Bibcode:2015A&A...574A.116R, doi:10.1051/0004-6361/201322360, hdl:10722/215277, S2CID 59334290. The values presented are for the RGB branch model.
- ^ Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities", Contributi Osservatorio Astronomico di Padova in Asiago, 239: 1, Bibcode:1970CoAsi.239....1B.
- ^ "psi06 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-28.