Mu Cassiopeiae

Mu Cassiopeiae
Mu Cassiopeiae A/B
Cassiopeia IAU.svg
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Star map of Cassiopeia. Mu Cassiopeiae is circled.
Observation data
Epoch J2000      Equinox J2000
Constellation Cassiopeia
Right ascension 01h 08m 16.39470s[1]
Declination +54° 55′ 13.2264″[1]
Apparent magnitude (V) 5.159[2]/11
Characteristics
Spectral type G5VIp/M5V
U−B color index +0.10[3]
B−V color index +0.70[3]
Variable type Suspected
Astrometry
Radial velocity (Rv) −98.3[2] km/s
Proper motion (μ) RA: 3,422.23[1] mas/yr
Dec.: −1,598.93[1] mas/yr
Parallax (π) 132.38 ± 0.82[1] mas
Distance 24.6 ± 0.2 ly
(7.55 ± 0.05 pc)
Absolute magnitude (MV) 5.77[2]/11.6
Orbit[4]
Companion μ Cas B
Period (P) 21.75 yr
Semimajor axis (a) 1.01"
Eccentricity (e) 0.56
Inclination (i) 110°
Longitude of the node (Ω) 47.3°
Periastron epoch (T) 1975.74
Argument of periastron (ω)
(secondary)		 152.7°
Details
Mass 0.74/0.17[4] M☉
Radius 0.791 ± 0.008[5]/0.29 R☉
Surface gravity (log g) 4.51[6]
Luminosity 0.442 ± 0.014[5]/0.001 L☉
Temperature 5,332[6] K
Metallicity [Fe/H] −0.84[6] dex
Rotational velocity (v sin i) 8[7] km/s
Age 3.1[2]–5.9[8] Gyr
Other designations
30 Cassiopeiae, Gl 53, HR 321, BD+54°223, HD 6582, LHS 8, LTT 10460, GCTP 219.00, SAO 22024, FK5 1030, LFT 107, HIP 5336, GC 1360, CCDM J01080+5455

Mu Cassiopeiae (μ Cas, μ Cassiopeiae) is a binary star system in the constellation Cassiopeia. This system shares the name Marfak with Theta Cassiopeiae, and the name was from Al Marfik or Al Mirfaq (المرفق), meaning "the elbow".[9]

In 1961 the close binary nature of this system was discovered by Nicholas E. Wagman at the Allegheny Observatory.[10] Since then the orbital elements of the two stars have been fairly well established. The two stars are separated by a semimajor axis of 7.61 AUs with distance range of 3.3-11.9 AUs.[citation needed] In 1966, the individual components were first resolved by the American astronomer Peter A. Wehinger using the 84-inch reflector at the Kitt Peak National Observatory, allowing an initial estimate of separate masses.[11]

Compared to other nearby stars, this pair are moving at a relatively high velocity of 167 km/s through the Milky Way galaxy. They are low metal, Population II stars that are thought to have formed before the galactic disk first appeared.

This star will be in constellation Perseus around 5200 AD.[12]

References

  1. ^ a b c d e van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, Bibcode 2007A&A...474..653V, doi:10.1051/0004-6361:20078357 
  2. ^ a b c d Nordström, B. et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs", Astronomy and Astrophysics 418: 989–1019, arXiv:astro-ph/0405198, Bibcode 2004A&A...418..989N, doi:10.1051/0004-6361:20035959 
  3. ^ a b Carney, B. W. (October 1979), "Subdwarf ultraviolet excesses and metal abundances", Astrophysical Journal, Part 1 233: 211–225, Bibcode 1979ApJ...233..211C, doi:10.1086/157383 
  4. ^ a b Gontcharov, G. A.; Kiyaeva, O. V. (August 2002), "Photocentric orbits from a direct combination of ground-based astrometry with Hipparcos. I. Comparison with known orbits", Astronomy and Astrophysics 391: 647–657, Bibcode 2002A&A...391..647G, doi:10.1051/0004-6361:20020896 
  5. ^ a b Boyajian, Tabetha S. et al. (August 2008), "Angular Diameters of the G Subdwarf μ Cassiopeiae A and the K Dwarfs σ Draconis and HR 511 from Interferometric Measurements with the CHARA Array", The Astrophysical Journal 683 (1): 424–432, Bibcode 2008ApJ...683..424B, doi:10.1086/589554 
  6. ^ a b c Soubiran, C. et al. (March 2008), "Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants", Astronomy and Astrophysics 480 (1): 91–101, Bibcode 2008A&A...480...91S, doi:10.1051/0004-6361:20078788 
  7. ^ Takeda, Yoichi et al. (February 2005), "High-Dispersion Spectra Collection of Nearby F--K Stars at Okayama Astrophysical Observatory: A Basis for Spectroscopic Abundance Standards", Publications of the Astronomical Society of Japan 57 (1): 13–25, Bibcode 2005PASJ...57...13T 
  8. ^ Mamajek, Eric E. et al. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal 687 (2): 1264–1293, Bibcode 2008ApJ...687.1264M, doi:10.1086/591785 
  9. ^ Allen, R. H. (1963), Star Names: Their Lore and Meaning (Reprint ed.), New York: Dover Publications Inc, p. 148, ISBN 0486210790, http://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Cassiopeia*.html, retrieved 2010-12-12 
  10. ^ Lippincott, S. L.; Wyckoff, S. (September 1964), "Parallax and orbital motion of the astrometric binary mu Cassiopeiae from photographs taken with the 24-inch Sproul refractor", Astronomical Journal 69: 471–474, Bibcode 1964AJ.....69..471L, doi:10.1086/109301 
  11. ^ Wehinger, Peter A.; Wyckoff, Susan (February 1966), "Preliminary Mass Determination of μ Cas", Astronomical Journal 71: 185, Bibcode 1966AJ.....71Q.185W, doi:10.1086/110028 
  12. ^ p. 296, Patrick Moore's Data Book of Astronomy, Patrick Moore and Robin Rees, Cambridge, Cambridge University Press, 2011.

External links

v · Cassiopeia
Bayer
α (Schedar) • β (Caph) • γ (Tsih) • δ (Ruchbah) • ε (Segin) • ζ • η (Achird) • θ • ι • κ • λ • μ • ν • ξ • ο • π • ρ • σ • τ • υ1 • υ2 • φ • χ • ψ • ω • A
Flamsteed
1 • 2 • 4 • 5 (τ) • 6 • 7 (ρ) • 8 (σ) • 9 • 10 • 11 (β, Caph) • 12 • 13 • 14 (λ) • 15 (κ) • 16 • 17 (ζ) • 18 (α, Schedar) • 19 (ξ) • 20 (π) • 21 • 22 (ο) • 23 • 24 (η, Achird) • 25 (ν) • 26 (υ1) • 27 (γ, Tsih) • 28 (υ2) • 30 (μ) • 31 • 32 • 33 (θ) • 34 (φ) • 35 • 36 (ψ) • 37 (δ, Ruchbah) • 38 • 39 (χ) • 40 • 42 • 43 • 44 • 45 (ε, Segin) • 46 (ω) • 47 • 48 (A) • 49 • 50 • 51 • 52 • 53 • 54 • 55

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