Zeta Cephei

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Zeta Cephei
Observation data
Epoch J2000      Equinox J2000
Constellation Cepheus
Right ascension 22h 10m 51.277s[1]
Declination +58° 12′ 04.55″[1]
Apparent magnitude (V) 3.39[2]
Characteristics
Spectral type K1.5 Ib[2]
B−V color index +1.57[2]
Variable type Suspected
Astrometry
Proper motion (μ) RA: 13.52 ± 0.10[1] mas/yr
Dec.: 5.24 ± 0.09[1] mas/yr
Parallax (π) 3.90 ± 0.10[1] mas
Distance 840 ± 20 ly
(256 ± 7 pc)
Details
Mass 7.9 M
Radius 110.0 R
Luminosity 5,660[2] L
Surface gravity (log g) 0.75[2] cgs
Temperature 3,853[2] K
Metallicity [Fe/H] +0.2 dex
Rotational velocity (v sin i) 8 km/s
Age 50 million years
Other designations
Tsao Fu, 21 Cephei, HR 8465, BD +57°2475, HD 210745, GCTP 5139.00, SAO 84137, FK5 836, HIP 105199

Zeta Cephei (ζ Cep, ζ Cephei) is a star in the constellation of Cepheus. Zeta Cephei marks the left shoulder of Cepheus, the King of Joppa (Ethiopia).

Zeta Cephei is an orange supergiant star of spectral type K1.5 Ib, with a surface temperature of 3,853 K[2] and eight times more massive then the Sun. The luminosity of Zeta Cephei is approximately 3600 times that of the Sun. At a distance of about 840 light-years,[1] Zeta Cephei has an apparent magnitude (m) of 3.39 and an absolute magnitude (M) of -3.35. The star has a metallicity approximately 1.6 times that of the Sun; i.e., it contains 1.6 times as much heavy-element material as the sun.

At the edge of the 8 to 10 solar mass limit at which stars develop iron cores and then explode as supernovae, Zeta Cephei's most likely fate is to produce a very massive white dwarf near the Chandrasekhar limit (1.4 solar mass) at which such dense remnants can survive. If Zeta Cephei is a binary star; i.e., if there is a stellar companion, and it is close enough to feed sufficient matter to the white-dwarf-to-be, it is marginally possible that the limit could be overflowed, resulting in the white dwarf's collapse and a Type Ia supernova explosion.

Hekkel et al. (2008) have detected a periodicity of 533 days, hinting at the possible presence of an as yet unseen companion.[3]

References[edit]

  1. ^ a b c d e f van Leeuwen, F. (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. Vizier catalog entry
  2. ^ a b c d e f g Mallik, Sushma V. (December 1999), "Lithium abundance and mass", Astronomy and Astrophysics 352: 495–507, Bibcode:1999A&A...352..495M 
  3. ^ Hekker et al. (2008). "Precise radial velocities of giant stars. IV. A correlation between surface gravity and radial velocity variation and a statistical investigation of companion properties". Astronomy and Astrophysics 480 (1): 215–222. arXiv:0809.0359. Bibcode:2008A&A...480..215H. doi:10.1051/0004-6361:20078321. 

External links[edit]

  • [1] by Jim Kaler