60 Andromedae (abbreviated 60 And) is a star system in the northern constellation of Andromeda, located to the west-northwest of Gamma Andromedae. 60 Andromedae is the Flamsteed designation though the star also bears the Bayer designation b Andromedae. It is bright enough to be seen by the naked eye with an apparent visual magnitude of 4.82.[2] Based upon parallax measurements made during the Hipparcos mission, it is at a distance of roughly 530 light-years (160 parsecs) from Earth.[1]
  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Andromeda |
| Right ascension | 02h 13m 13.32387s[1] |
| Declination | +44° 13′ 53.9546″[1] |
| Apparent magnitude (V) | +4.82[2] |
| Characteristics | |
| Spectral type | K3.5 III Ba0.4[3] |
| U−B color index | +1.74[2] |
| B−V color index | +1.48[2] |
| Astrometry | |
| Radial velocity (Rv) | –46.3[4] km/s |
| Proper motion (μ) | RA: –20.90[1] mas/yr Dec.: –14.46[1] mas/yr |
| Parallax (π) | 6.15 ± 0.63 mas[1] |
| Distance | approx. 530 ly (approx. 160 pc) |
| Orbit[5] | |
| Period (P) | 748.2±0.4 days |
| Semi-major axis (a) | 2.4±0.6 mas |
| Eccentricity (e) | 0.80 |
| Inclination (i) | 54.1±19.9° |
| Longitude of the node (Ω) | 344.5±10.3° |
| Periastron epoch (T) | 37886±11 HJD |
| Argument of periastron (ω) (secondary) | 358±6° |
| Semi-amplitude (K1) (primary) | 4.88 km/s |
| Details | |
| 60 And A | |
| Mass | 2.0+0.7 −0.3[6] M☉ |
| Surface gravity (log g) | 1.70±0.44[7] cgs |
| Temperature | 4054±42[7] K |
| Metallicity [Fe/H] | −0.13±0.12[7] dex |
| 60 And B | |
| Mass | 0.5±0.1[6] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
This system is known to have three components. The primary is a giant star with a stellar classification of K3.5 III Ba0.4, meaning that an overabundance of barium ionized one time is observed in the spectrum of the star, making it a barium star. The secondary component is likely a white dwarf with a period of 748.2 days and an eccentricity of 0.34. There is a third component at an angular separation of 0.22 arcseconds.[3]
References
edit- ^ a b c d e f van Leeuwen, F. (November 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.
- ^ a b Eggleton, P. P.; Tokovinin, A. A. (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, S2CID 14878976.
- ^ Wilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication, Washington: Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W.
- ^ Ren, Shulin; Fu, Yanning (March 2013), "Hipparcos Photocentric Orbits of 72 Single-lined Spectroscopic Binaries", The Astronomical Journal, 145 (3): 7, Bibcode:2013AJ....145...81R, doi:10.1088/0004-6256/145/3/81, S2CID 120199240, 81.
- ^ a b Pourbaix, D.; Boffin, H. M. J. (February 2003), "Reprocessing the Hipparcos Intermediate Astrometric Data of spectroscopic binaries. II. Systems with a giant component", Astronomy and Astrophysics, 398 (3): 1163–1177, arXiv:astro-ph/0211483, Bibcode:2003A&A...398.1163P, doi:10.1051/0004-6361:20021736, S2CID 12361870.
- ^ a b c Koleva, M.; Vazdekis, A. (February 2012), "Stellar population models in the UV. I. Characterisation of the New Generation Stellar Library", Astronomy & Astrophysics, 538: A143, arXiv:1111.5449, Bibcode:2012A&A...538A.143K, doi:10.1051/0004-6361/201118065, S2CID 53999614.
- ^ Tirion; Rappaport; Lovi (1987). Willmann-Bell, Inc. (ed.). Uranometria 2000.0 - Volume II - The Southern Hemisphere to +6°. Richmond, Virginia, USA. ISBN 0-943396-15-8.