T Cephei is aMira variable star in the constellationCepheus. Located approximately 600 light-years (180 parsecs) distant, it varies between magnitudes 5.2 and 11.3 over a period of around 388 days.[9][2] When it is near its maximum brightness, it is faintly visible to thenaked eye under good observing conditions.
Vitold Ceraski announced his discovery that the star is avariable star, in 1879.[12] It appeared with itsvariable star designation, T Cephei, inAnnie Jump Cannon's 1907 publicationSecond catalogue of variable stars.[13] T Cephei is ared giant of spectral type M6-9e with an effective temperature 2,400K, a radius of 329 R☉, a mass of 0.55 M☉, and a luminosity of 5,700 L☉. If it were in the place of theSun, itsphotosphere would at least engulf the orbit ofMars. This star is believed to be in a late stage of its life, theasymptotic giant branch phase, blowing off its own atmosphere to form awhite dwarf in a distant future.
^abDucati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system".CDS/ADC Collection of Electronic Catalogues.2237.Bibcode:2002yCat.2237....0D.
^Tuchman, Y. (1991). "The mode of pulsation in Mira variables determined by the observed acceleration data".The Astrophysical Journal.383: 779.Bibcode:1991ApJ...383..779T.doi:10.1086/170836.
^Weigelt, Gerd; Beckmann, Udo; Berger, Jean-Philippe; Bloecker, Thomas; Brewer, Michael K.; Hofmann, Karl-Heinz; Lacasse, Marc G.; Malanushenko, Victor; Millan-Gabet, Rafael; et al. (2003). "JHK-band spectro-interferometry of T Cep with the IOTA interferometer". In Traub, Wesley A (ed.).Interferometry for Optical Astronomy II. Proc. SPIE. Vol. 4838. Society of Photo-optical Instrumentation Engineers (SPIE). pp. 181–184.Bibcode:2003SPIE.4838..181W.doi:10.1117/12.458659.ISBN9780819446176.S2CID123045204.
^abcDanilovich, T.; Teyssier, D.; Justtanont, K.; Olofsson, H.; Cerrigone, L.; Bujarrabal, V.; Alcolea, J.; Cernicharo, J.; Castro-Carrizo, A.; García-Lario, P.; Marston, A. (2015). "New observations and models of circumstellar CO line emission of AGB stars in the Herschel SUCCESS programme".Astronomy & Astrophysics.581: A60.arXiv:1506.09065.Bibcode:2015A&A...581A..60D.doi:10.1051/0004-6361/201526705.S2CID55109956.
^Guha Niyogi, Suklima; Speck, Angela K.; Onaka, Takashi (2011). "A Temporal Study of the Oxygen-rich Pulsating Variable Asymptotic Giant Branch Star, T Cep: Investigation on Dust Formation and Dust Properties".The Astrophysical Journal.733 (2): 93.arXiv:1103.5040.Bibcode:2011ApJ...733...93G.doi:10.1088/0004-637X/733/2/93.S2CID118332811.
