V Cephei is a white
main sequence star in the constellation
Cepheus. It only
varies slightly by 0.03 of a
magnitude. It was suspected of being variable by American astronomer
Seth Carlo Chandler noting in 1890 that it varied by 0.7 magnitude but that it needed more confirmation. Subsequent observers were divided in whether they noted variability or not.[9] A subsequent study with photoelectric photometry showed no variability.[10]
^Anders, F.; Khalatyan, A.; Chiappini, C.; Queiroz, A. B.; Santiago, B. X.; Jordi, C.; Girardi, L.; Brown, A. G. A.; Matijevič, G.; Monari, G.; Cantat-Gaudin, T.; Weiler, M.; Khan, S.; Miglio, A.; Carrillo, I.; Romero-Gómez, M.; Minchev, I.; De Jong, R. S.; Antoja, T.; Ramos, P.; Steinmetz, M.; Enke, H. (2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy and Astrophysics. 628: A94.
arXiv:1904.11302.
Bibcode:
2019A&A...628A..94A.
doi:
10.1051/0004-6361/201935765.
S2CID131780028.
^
abDavid, Trevor J.; Hillenbrand, Lynne A. (2015). "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal. 804 (2): 146.
arXiv:1501.03154.
Bibcode:
2015ApJ...804..146D.
doi:
10.1088/0004-637X/804/2/146.
S2CID33401607.
^Hoffleit, Dorrit (1985). "Was Harlow Shapley Right About V Cephei?". The Journal of the American Association of Variable Star Observers. 14 (2): 64–66.
Bibcode:
1985JAVSO..14...64H.
^Fortier, George (1989). "Photoelectric Photometry of V Cephei". The Journal of the American Association of Variable Star Observers. 18 (1): 49–51.
Bibcode:
1989JAVSO..18...49F.