Gamma Cephei (γ Cephei, abbreviated Gamma Cep, γ Cep) is a binary star system approximately 45 light-years away in the northern constellation of Cepheus. The primary (designated Gamma Cephei A, officially named Errai/ɛˈreɪ.iː/, the traditional name of the system)[11][12] is a stellar class K1 orange giant or subgiant star; it has a red dwarf companion (Gamma Cephei B). An exoplanet (designated Gamma Cephei Ab, later named Tadmor) has been confirmed to be orbiting the primary.
Gamma Cephei is the naked-eye star that will succeed Polaris as the Earth's northern pole star, due to axial precession. It will be closer to the northern celestial pole than Polaris around 3230 CE and will make its closest approach around 4300 CE. The 'title' will pass to Iota Cephei some time around 5200 CE.
Description
Gamma Cephei has an apparent magnitude of 3.21, nearly all of which is accounted for by the primary component, Gamma Cephei A. It is a binary star system with an orbital period of 66.8 years and an eccentricity (ovalness) of 0.14.[8] The pair are orbiting at a separation of 19.6 AU.[8]
The primary is about 5.7 billion years old and has evolved off the main sequence, having fused all of the hydrogen in its core. It has 1.3 times the mass of the Sun and has expanded to 4.7 times the Sun's radius.[9] The star is radiating nearly 12[10] times the luminosity of the Sun from its photosphere at an effective temperature of 4,806 K.[9] The secondary component, Gamma Cephei B, has a mass approximately 0.40 times that of the Sun.[5] It is probably a red dwarf of class M4, 6.2 magnitudes fainter than the primary.[5] It is assumed to be of similar age to its primary.
The spectrum of this star has served as one of the stable anchor points by which other stars are classified. It was listed as a standard star for the spectral class K1 IV in 1943, 1953 and 1973.[13] However, in 1989, it was given as a spectral standard for K1 III-IV. Its spectrum is notable for the strength of the cyano radical (CN) bands.[3] Analysis of the spectrum in 2018 gave a best match for a spectral type of K1 III.[10]
γ Cephei is catalogued as a suspected variable star with a brightness range between magnitudes 3.18 and 3.24,[4] based on its inclusion in an 1884 list of suspected variable stars.[14]
Nomenclature
γ Cephei (Latinised to Gamma Cephei) is the system's Bayer designation. Under the rules for naming objects in multiple star systems the two components are designated A and B.[15] Following its discovery the planet was designated Gamma Cephei Ab.
The system bore a traditional name variously spelled as Errai, Er Rai or Alrai, deriving from the Arabic الراعي (ar-rā‘ī), meaning 'the shepherd'. (The star Beta Ophiuchi is sometimes also called Alrai, but it is more commonly known as Cebalrai or Kelb Alrai, meaning 'shepherd's dog'.) In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[16] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[17] included a table of the first two batches of names approved by the WGSN; which included Errai for Gamma Cephei A.
In July 2014 the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets.[18] The process involved public nomination and voting for the new names.[19] In December 2015, the IAU announced the winning name was Tadmor for this planet.[20] It was submitted by the Syrian Astronomical Association and is the ancient Semitic name and modern Arabic name for the city of Palmyra, a World Heritage Site.[21]
A planet orbiting Gamma Cephei A with a 2.7-year period was discovered in 1988.[24] Its existence was also announced in 1989.[25] This was 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 challenged in 1992 by a paper[26] which favoured K-giant variability with a period equal to the stellar rotation, but in 2002, the existence of a planet with an orbital period of about 2.5 years was confirmed.[27]
Astrometric measurements have shown that the planet's orbital inclination is between 3.7° and 15.5°, meaning that its true mass is between 6.6 and 28.1 MJ.[9]
The secondary star B orbits A at only 9.8 times the semimajor axis of A's planet.[28] The orbit of the planet is roughly perpendicular to the orbit of the binary. Dynamical modelling suggests that the Kozai–Lidov mechanism is at play here.[29]
^ abcHoffleit, D.; Warren, W. H. (1995). "VizieR Online Data Catalog: Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)". VizieR On-line Data Catalog: V/50. Originally Published in: 1964BS....C......0H. 5050: V/50. Bibcode:1995yCat.5050....0H.
^ abSamus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
^ abJofré, E; Petrucci, R; Saffe, C; Saker, L; Artur de la Villarmois, E; Chavero, C; Gómez, M; Mauas, P. J. D (2015). "Stellar parameters and chemical abundances of 223 evolved stars with and without planets". Astronomy & Astrophysics. 574: A50. arXiv:1410.6422. Bibcode:2015A&A...574A..50J. doi:10.1051/0004-6361/201424474. S2CID53666931.
^Gore, J. E (1884). "A Catalogue of Suspected Variable Stars. With Notes and Observations". Proceedings of the Royal Irish Academy. Science. 4: 267–410. Bibcode:1885PRIA....4..411G. JSTOR20635921.
^Lawton, A. T.; Wright, P. (1989). "A planetary system for Gamma Cephei?". British Interplanetary Society. 42: 335–336. Bibcode:1989JBIS...42..335L.
^Walker, Gordon A.H.; Bohlender, David A.; Walker, Andrew R. (1992). "Gamma Cephei: Rotation or Planetary Companion?". Astrophysical Journal Letters. 396: L91–L94. Bibcode:1992ApJ...396L..91W. doi:10.1086/186524.
^Endl, Michael; et al. (2011). News from the γ Cephei Planetary System. PLANETARY SYSTEMS BEYOND THE MAIN SEQUENCE: Proceedings of the International Conference. AIP Conference Proceedings. Vol. 1331. pp. 88–94. arXiv:1101.2588. Bibcode:2011AIPC.1331...88E. doi:10.1063/1.3556187.
