60 Andromedae is a star system in the northern constellation of Andromeda, located to the east-northeast of Gamma Andromedae. 60 Andromedae is the Flamsteed designation (abbreviated 60 And), though the star also bears the Bayer designation b Andromedae.[11] It is bright enough to be seen by the naked eye on a dark night, having an apparent visual magnitude of 4.82.[3] Based upon parallax measurements, it is located at a distance of approximately 620 light-years (190 parsecs) from Earth.[2] The system is drifting closer with a heliocentric radial velocity of –46 km/s.[5]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Andromeda[1] |
Right ascension | 02h 13m 13.322s[2] |
Declination | +44° 13′ 53.93″[2] |
Apparent magnitude (V) | +4.82[3] |
Characteristics | |
Spectral type | K3.5 III Ba0.4[4] |
U−B color index | +1.74[3] |
B−V color index | +1.48[3] |
Astrometry | |
Radial velocity (Rv) | –46.3[5] km/s |
Proper motion (μ) | RA: –20.90 mas/yr[6] Dec.: –14.46 mas/yr[6] |
Parallax (π) | 5.2634±0.2576 mas[2] |
Distance | 620 ± 30 ly (190 ± 9 pc) |
Absolute magnitude (MV) | −1.19[1] |
Orbit[7] | |
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[8] M☉ |
Luminosity | 685[1] L☉ |
Surface gravity (log g) | 1.70±0.44[9] cgs |
Temperature | 4,054±42[9] K |
Metallicity [Fe/H] | −0.13±0.12[9] dex |
Age | 2.02[10] Gyr |
60 And B | |
Mass | 0.5±0.1[8] M☉ |
Other designations | |
b Andromedae[11], BD+43 447, HD 13520, HIP 10340, HR 643, SAO 37867, PPM 44882, IRAS 02100+4359[12] | |
Database references | |
SIMBAD | data |
This system is known to have three components. The primary is an aging giant star with a stellar classification of K3.5 III Ba0.4, meaning that an overabundance of singly-ionized barium (Ba+ ion) is observed in the spectrum of the star, making it a barium star. This star is about 2[10] billion years old with double the mass of the Sun.[8] It is radiating 685[1] times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,054 K.[9] The secondary component is likely a degenerate white dwarf with a orbital period of 748.2 days and an eccentricity of 0.34. There is a third component at an angular separation of 0.22 arcseconds.[4]
References
edit- ^ a b c d 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 d 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.
- ^ 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.
- ^ a b 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.
- ^ 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.
- ^ 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 c 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 d 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.
- ^ a b Luck, R. Earle (2015), "Abundances in the Local Region. I. G and K Giants", Astronomical Journal, 150 (3), 88, arXiv:1507.01466, Bibcode:2015AJ....150...88L, doi:10.1088/0004-6256/150/3/88, S2CID 118505114.
- ^ a b 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.
- ^ "60 And". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2025-03-26.