Gamma Cephei
 Location of γ Cephei (top center). |
|
| Observation data Epoch J2000.0 Equinox J2000.0 |
|
|---|---|
| Constellation | Cepheus |
| Right ascension | 23h 39m 20.85s[1] |
| Declination | +77° 37′ 56.2″[1] |
| Apparent magnitude (V) | 3.22 |
| Characteristics | |
| Gamma Cephei A | |
| Spectral type | K1IVe |
| U−B color index | 0.94 |
| B−V color index | 1.03 |
| Variable type | Suspected |
| Gamma Cephei B | |
| Spectral type | M4V[2] |
| Astrometry | |
| Radial velocity (Rv) | 8.8 km/s |
| Proper motion (μ) | RA: -47.96 ± 0.45[1] mas/yr Dec.: 126.59 ± 0.40[1] mas/yr |
| Parallax (π) | 72.69 ± 0.41[2] mas |
| Distance | 44.9 ± 0.3 ly (13.76 ± 0.08 pc) |
| Absolute magnitude (MV) | 2.51 |
| Orbit[2] | |
| Primary | A |
| Companion | B |
| Period (P) | 67.5 ± 1.4 yr |
| Semimajor axis (a) | 1.467 ± 0.046" (20.18 ± 0.66 AU) |
| Eccentricity (e) | 0.4112 ± 0.0063 |
| Inclination (i) | 119.3 ± 1.0° |
| Longitude of the node (Ω) | 18.04 ± 0.98° |
| Periastron epoch (T) | 1991.605 ± 0.031 |
| Argument of periastron (ω) (secondary) |
161.01 ± 0.40° |
| Details | |
| Gamma Cephei A | |
| Mass | 1.40 ± 0.12[2] M☉ |
| Radius | 4.79 ± 0.06[3] R☉ |
| Age | 6.6[4] Gyr |
| Gamma Cephei B | |
| Mass | 0.409 ± 0.018[2] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| Extrasolar Planets Encyclopaedia |
data |
Gamma Cephei (γ Cep, γ Cephei), traditionally named Errai, Er Rai, and or Alrai, is a binary star system approximately 45 light-years away in the constellation of Cepheus. Gamma Cephei contains an apparent magnitude of 3.22. The visible part of the system is a stellar class K1III-IV orange subgiant star on its first ascent off the main sequence. It is about 6.6 billion years old (based on Fe/H metallicity).[4] Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified.[5]
Gamma Cephei is the naked-eye star that will succeed Polaris as the Earth's northern pole star, due to the precession of the equinoxes. It will be closer to the northern celestial pole than Polaris around 3000 CE and will make its closest approach around 4000 CE. The "title" will pass to ι Cephei some time around 5200 CE.
The star has a companion star with a mass approximately 0.409 times that of our Sun.[2] Gamma Cephei B is of stellar mass and is assumed to be of similar age to its primary. It is probably a red dwarf of class M4, 6.2 degrees of magnitude fainter than the K-type primary star.[2]
Contents |
Etymology [edit]
Gamma Cephei's traditional name derives from the Arabic الراعي ar-rā‘ī, meaning "the shepherd". Confusingly, the star β Ophiuchi is sometimes also called Alrai, but it is more commonly known as Cebalrai or Kelb Alrai, meaning "shepherd's dog".
In Chinese, 紫微左垣 (Zǐ Wēi Zuǒ Yuán), meaning Left Wall of Purple Forbidden Enclosure, refers to an asterism consisting of γ Cephei, ι Draconis, θ Draconis, η Draconis, ζ Draconis, υ Draconis, 73 Draconis and 23 Cassiopeiae.[6] Consequently, γ Cephei itself is known as 紫微左垣七 (Zǐ Wēi Zuǒ Yuán qī, English: the Seventh Star of Left Wall of Purple Forbidden Enclosure.),[7] representing 右樞 (Shǎowèi), meaning The Second Imperial Guard[8] or Minor Guard[9]
Planetary system [edit]
A planet orbiting Gamma Cephei A was tentatively identified by a Canadian team consisting of Bruce Campbell, Gordon Walker and Stephenson Yang in 1988.[10] Its existence was also announced by Anthony Lawton and P Wright in 1989.[11] This would have been the first confirmed extrasolar planet and its ostensible discovery was based on the same radial velocity technique later used successfully by others. However, the claim was retracted in 1992 because the quality of the data was not good enough to establish discovery. But in 2002, evidence of the planet was considerably strengthened by new measurements by Artie Hatzes and his collaborators at the McDonald Observatory.[12]
The secondary star B orbits A at only 9.5 times the semimajor axis of A's planet. The orbits are probably coplanar.[4]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥1.60 ± 0.13 MJ | 2.044 ± 0.057 | 902.9 ± 3.5 | 0.115 ± 0.058 | — | — |
See also [edit]
References [edit]
- ^ a b c d van Leeuwen, F. (2007). "HIP 116727". Hipparcos, the New Reduction. Retrieved 2009-12-06.
- ^ a b c d e f g Neuhäuser, R. et al. (2007). "Direct detection of exoplanet host star companion γ Cep B and revised masses for both stars and the sub-stellar object". Astronomy and Astrophysics 462 (2): 777–780. arXiv:astro-ph/0611427. Bibcode:2007A&A...462..777N. doi:10.1051/0004-6361:20066581.
- ^ Nordgren, Tyler E. et al. (December 1999), "Stellar Angular Diameters of Late-Type Giants and Supergiants Measured with the Navy Prototype Optical Interferometer", The Astronomical Journal 118 (6): 3032–3038, Bibcode:1999AJ....118.3032N, doi:10.1086/301114
- ^ a b c Torres, Guillermo (2007). "The Planet Host Star γ Cephei: Physical Properties, the Binary Orbit, and the Mass of the Substellar Companion". The Astrophysical Journal 654 (2): 1095–1109. arXiv:astro-ph/0609638. Bibcode:2007ApJ...654.1095T. doi:10.1086/509715.
- ^ Garrison, R. F. (December 1993), "Anchor Points for the MK System of Spectral Classification", Bulletin of the American Astronomical Society 25: 1319, Bibcode:1993AAS...183.1710G, retrieved 2012-02-04
- ^ (Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN 978-986-7332-25-7.
- ^ (Chinese) 香港太空館 - 研究資源 - 亮星中英對照表, Hong Kong Space Museum. Accessed on line November 23, 2010.
- ^ (Chinese) English-Chinese Glossary of Chinese Star Regions, Asterisms and Star Name, Hong Kong Space Museum. Accessed on line November 23, 2010.
- ^ Richard Hinckley Allen: Star Names — Their Lore and Meaning: Cepheus
- ^ Campbell et al.; Walker, G. A. H.; Yang, S. (1988). "A search for substellar companions to solar-type stars". The Astrophysical Journal 331: 902–921. Bibcode:1988ApJ...331..902C. doi:10.1086/166608.
- ^ Lawton, A. T.; Wright, P. (1989). "A planetary system for Gamma Cephei?". British Interplanetary Society 42: 335–336. Bibcode:1989JBIS...42..335L.
- ^ Hatzes, Artie P. et al. (2003). "A Planetary Companion to Gamma Cephei A". The Astrophysical Journal 599 (2): 1383–1394. arXiv:astro-ph/0305110. Bibcode:2003ApJ...599.1383H. doi:10.1086/379281.
External links [edit]
- http://jumk.de/astronomie/exoplanets/errai.shtml
- McDonald Observatory: Planet Search finds first planet orbiting close-in binary star
- A Planetary Companion to the Binary Star Gamma Cephei
- SolStation: Errai 2
- Extrasolar Visions: Gamma Cephei A + Gamma Cephei Ab + Gamma cephei B
| Preceded by Polaris |
Pole Star 3000–5200 |
Succeeded by Iota Cephei |
Coordinates: 
23h 39m 20.8s, +77° 37′ 56″
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