Phi Cassiopeiae

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φ Cassiopeiae
Phi cassiopeiae diagram.jpg
Chart of the Bayer-designated stars in Cassiopeia. Phi Cassiopeiae is circled.
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cassiopeia
Right ascension 01h20m04.9s
Declination +58°13′54″
Apparent magnitude (V) +5.01
Spectral type F0Ia
U−B color index +0.59
B−V color index +0.58
Variable type none
Radial velocity (Rv) −28.39 km/s
Proper motion (μ) RA: −0.59 mas/yr
Dec.: −1.59 mas/yr
Parallax (π) 0.27 ± 0.32 mas
Distance 2300 ly
(710 pc)
Absolute magnitude (MV) −8.76[1]
Mass 6.3[2] M
Radius 263[2] R
Luminosity 170,000[2] L
Surface gravity (log g) 1.0[1] cgs
Temperature 7,341[1] K
Metallicity -0.24[1]
Other designations
34 Cassiopeiae, HR 382, HD 7927, BD+57°260, HIP 6242, SAO 22191, GC 1594, ADS 1073, CCDM J01200+5813
Database references

Phi Cassiopeiae (φ Cas, φ Cassiopeiae) is a star in the constellation Cassiopeia. φ Cassiopeiae is a binary star with an apparent magnitude of +4.95. The primary component of φ Cas is an F0Ia bright supergiant of magnitude 4.95 and the secondary is a 7.08 magnitude B6 supergiant at 134" distance.[3]

It is approximately 2300 light years from Earth. It appears among the stars of the open cluster NGC 457 at approximately the same distance, but it is unclear whether it is a member of the cluster.[4][2]


  1. ^ a b c d Kovtyukh, V. V.; Gorlova, N.; Belik, S. I. (2012). "Accurate luminosities from the oxygen 7771-4 a triplet and the fundamental parameters of F-G supergiants". arXiv:1204.4115v1 [astro-ph.SR].
  2. ^ a b c d Rosenzweig, P.; Anderson, L. (1993). "A determination of the basic atmospheric parameters of Phi Cassiopeiae". The Astrophysical Journal 411: 207. doi:10.1086/172820.  edit
  3. ^ Eggleton, P. P.; Tokovinin, A. A. (2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society 389 (2): 869. doi:10.1111/j.1365-2966.2008.13596.x.  edit
  4. ^ Zhang, X. B.; Luo, C. Q.; Fu, J. N. (2012). "B-Type Variables in the Young Open Cluster Ngc 457". The Astronomical Journal 144 (3): 86. doi:10.1088/0004-6256/144/3/86.  edit