Astronomy:Mu Andromedae

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Short description: Binary star in the constellation Andromeda
μ Andromedae
Andromeda constellation map.svg
Red circle.svg
Location of μ Andromedae (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Andromeda
Right ascension  00h 56m 45.21211s[1]
Declination +38° 29′ 57.6380″[1]
Apparent magnitude (V) 3.87[2]
Characteristics
Spectral type A5 V[3]
U−B color index +0.15[2]
B−V color index +0.12[2]
Astrometry
Radial velocity (Rv)+7.6[4] km/s
Proper motion (μ) RA: +153.48[1] mas/yr
Dec.: +36.49[1] mas/yr
Parallax (π)25.14 ± 0.86[1] mas
Distance130 ± 4 ly
(40 ± 1 pc)
Absolute magnitude (MV)+0.86[5]
Orbit[6]
Period (P)550.7 ± 0.2 d
Semi-major axis (a)46.66 ± 0.06 mas
Eccentricity (e)0.8405 ± 0.0009
Inclination (i)52.5 ± 0.3°
Longitude of the node (Ω)−17.6 ± 0.2°
Periastron epoch (T)55765.45 ± 0.04 MJD
Argument of periastron (ω)
(secondary)		168.9 ± 0.3°
Semi-amplitude (K1)
(primary)		11.1 ± 0.5 km/s
Details
Mass2.0[7] M☉
Radius2.4[7] R☉
Luminosity21[7] L☉
Surface gravity (log g)3.99[7] cgs
Temperature7,959[8] K
Metallicity [Fe/H]+0.03[8] dex
Rotational velocity (v sin i)75[9] km/s
Age600[10] Myr
Other designations
μ Andromedae, μ And, Mu And, 37 Andromedae, BD+37°175, FK5 33, HD 5448, HIP 4436, HR 269, SAO 54281, PPM 65785
Database references
SIMBADdata

Mu Andromedae (Mu And, μ Andromedae, μ And) is the Bayer designation for a star in the northern constellation of Andromeda. It has an apparent visual magnitude of 3.87,[2] making it readily visible to the naked eye. Based upon parallax measurements, it is approximately 130 light-years (40 parsecs) from Earth.[1] In the constellation, the star is situated about halfway between the bright star Mirach to the southwest and the Andromeda Galaxy (M31) to the northeast.[11]

The spectrum of this star matches a stellar classification of A5 V,[3] indicating that it is an A-type main sequence star. It has double the mass of the Sun and 2.4 times the Sun's radius.[7] The star is radiating about 21[7] times the luminosity of the Sun from its outer envelope at an effective temperature of 7,959 K,[8] giving it the characteristic white glow of an A-type star.[12] It is estimated to be about 600 million years old,[10] with a relatively high projected rotational velocity of 75 km/s.[9] Mu Andromedae has recently been found to be a binary system. The two stars orbit each other every 550.7 days.[6]

Naming

In Chinese, 奎宿 (Kuí Sù), meaning Legs (asterism), refers to an asterism consisting of μ Andromedae, η Andromedae, 65 Piscium, ζ Andromedae, ε Andromedae, δ Andromedae, π Andromedae, ν Andromedae, β Andromedae, σ Piscium, τ Piscium, 91 Piscium, υ Piscium, φ Piscium, χ Piscium and ψ¹ Piscium. Consequently, the Chinese name for μ Andromedae itself is 奎宿八 (Kuí Sù bā, English: the Eighth Star of Legs.)[13]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V. 
  2. ↑ 2.0 2.1 2.2 2.3 Johnson, H. L. et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory 4 (99): 99, Bibcode: 1966CoLPL...4...99J. 
  3. ↑ 3.0 3.1 Cowley, A. et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal 74: 375–406, doi:10.1086/110819, Bibcode: 1969AJ.....74..375C. 
  4. ↑ Wilson, R. E. (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication (Carnegie Institute of Washington D.C.), Bibcode: 1953GCRV..C......0W. 
  5. ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  6. ↑ 6.0 6.1 Roettenbacher, R.M.; Monnier, J.D.; Korhonen, H.; Aarnio, A.N.; Baron, F.; Che, X.; Harmon, R.O.; Kővári, Zs. et al. (2016). "No Sun-like dynamo on the active star ζ Andromedae from starspot asymmetry". Nature 533 (7602): 217–220. doi:10.1038/nature17444. PMID 27144357. Bibcode: 2016Natur.533..217R. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 7.5 Malagnini, M. L.; Morossi, C. (November 1990), "Accurate absolute luminosities, effective temperatures, radii, masses and surface gravities for a selected sample of field stars", Astronomy and Astrophysics Supplement Series 85 (3): 1015–1019, Bibcode: 1990A&AS...85.1015M. 
  8. ↑ 8.0 8.1 8.2 Gardiner, R. B.; Kupka, F.; Smalley, B. (July 1999), "Testing convection theories using Balmer line profiles of A, F, and G stars", Astronomy and Astrophysics 347: 876–890, Bibcode: 1999A&A...347..876G. 
  9. ↑ 9.0 9.1 Royer, F.; Zorec, J.; Gómez, A. E. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics 463 (2): 671–682, doi:10.1051/0004-6361:20065224, Bibcode: 2007A&A...463..671R. 
  10. ↑ 10.0 10.1 Rieke, G. H. et al. (February 2005), "Decay of Planetary Debris Disks", The Astrophysical Journal 620 (2): 1010–1026, doi:10.1086/426937, Bibcode: 2005ApJ...620.1010R. 
  11. ↑ Reddy, Francis (2011), Celestial Delights: The Best Astronomical Events Through 2020 (3rd ed.), Springer, p. 236, ISBN 978-1461406099, https://books.google.com/books?id=OcGsCZPlDIoC&pg=PA236. 
  12. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html, retrieved 2012-01-16. 
  13. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 19 日

External links



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