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60 Andromedae

From Wikipedia, the free encyclopedia
Star system in the constellation Andromeda
This article is about b Andromedae; it is not to be confused withβ Andromedae.
60 Andromedae
Location of 60 Andromedae (circled)
Observation data
Epoch J2000      Equinox J2000
ConstellationAndromeda[1]
Right ascension02h 13m 13.322s[2]
Declination+44° 13′ 53.93″[2]
Apparent magnitude (V)+4.82[3]
Characteristics
Spectral typeK3.5 III Ba0.4[4]
U−Bcolor index+1.74[3]
B−Vcolor index+1.48[3]
Astrometry
Radial velocity (Rv)–46.3[5] km/s
Proper motion (μ)RA: –20.90mas/yr[6]
Dec.: –14.46mas/yr[6]
Parallax (π)5.2634±0.2576 mas[2]
Distance620 ± 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°
Periastronepoch (T)37886±11 HJD
Argument of periastron (ω)
(secondary)
358±6°
Semi-amplitude (K1)
(primary)
4.88 km/s
Details
60 And A
Mass2.0+0.7
−0.3
[8] M
Luminosity685[1] L
Surface gravity (log g)1.70±0.44[9] cgs
Temperature4,054±42[9] K
Metallicity[Fe/H]−0.13±0.12[9] dex
Age2.02[10] Gyr
60 And B
Mass0.5±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
SIMBADdata

60 Andromedae is astar system in the northernconstellation ofAndromeda, located to the east-northeast ofGamma Andromedae.60 Andromedae is theFlamsteed designation (abbreviated60 And), though the star also bears theBayer designationb Andromedae.[11] It is bright enough to be seen by thenaked eye on a dark night, having anapparent visual magnitude of 4.82.[3] Based uponparallax measurements, it is located at a distance of approximately 620light-years (190parsecs) from Earth.[2] The system is drifting closer with a heliocentricradial velocity of –46 km/s.[5]

This system is known to have three components. The primary is an aginggiant star with astellar classification ofK3.5 III Ba0.4, meaning that an overabundance of singly-ionizedbarium (Ba+ ion) is observed in the spectrum of the star, making it abarium 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 enlargedphotosphere at aneffective temperature of 4,054 K.[9] The secondary component is likely adegeneratewhite dwarf with anorbital period of 748.2 days and aneccentricity of 0.34. There is a third component at anangular separation of 0.22 arcseconds.[4]

References

[edit]
  1. ^abcdAnderson, 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.
  2. ^abcdBrown, 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 atVizieR.
  3. ^abcdArgue, 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.
  4. ^abEggleton, 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.
  5. ^abWilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities",Carnegie Institute Washington D.C. Publication, Washington:Carnegie Institution of Washington,Bibcode:1953GCRV..C......0W.
  6. ^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.
  7. ^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.
  8. ^abcPourbaix, 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.
  9. ^abcdKoleva, 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.
  10. ^abLuck, 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.
  11. ^abTirion; 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.
  12. ^"60 And".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2025-03-26.

External links

[edit]
  1. "* 60 And".SIMBAD.Centre de données astronomiques de Strasbourg.
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