Observations of the open cluster NGC 7419 in 1954 showed that four of its members were luminous red stars, most likely red supergiants. In addition, an unusually red star was found to be variable and probably an even more luminous supergiant.[11] This star was given the variable star designation MY Cephei in 1973 in the 59th name-list of variable stars.[12]
MY Cephei is classified as semiregular variable star of sub-type SRc, indicating it is a cool supergiant, although its pulsational period is not known. It has been observed as bright as magnitude 14.4 and as faint as magnitude 15.5.[2] The star, along with another late red supergiant star, S Persei, are sometimes considered prototypes for the class of M6–7 supergiants.[13]
The spectral type of MY Cephei is given in the General Catalogue of Variable Stars as M6–7 Iab, indicating the star is an intermediate-size luminous supergiant star,[2] although most authors gives M7–M7.5 I.[6] Classification is difficult because of the lack of comparable standard stars, but its spectrum appears to be later than M5, earlier than VX Sagittarii when at M9, and more luminous than M7 giant stars.[13] A 2021 study gives a spectral class of M3 based on infrared observations, and a correspondingly higher temperature.[5]
MY Cephei is a very luminous, cool and large extreme supergiant star, with a luminosity more than 100,000 times that of the Sun (L☉) and a radius in excess of a thousand times the Sun's radius (R☉). It is likely the most luminous, coolest, and the largest supergiant star in its open cluster,[6] and occupies the upper-right hand corner of the Hertzsprung–Russell diagram.
A 2018 paper gives the star a temperature of 3,400 K, corresponding a radius of 1,134 R☉ based on a luminosity of 155,000 L☉.[15] The mass of MY Cephei is uncertain, but expected to be around 14.5 times the Sun's mass (M☉).[9] Mass is being lost at (2.3±0.3)×10−5M☉ per year, one of highest mass loss rates known for a supergiant star.[6]
A study from 2020 based on SED integration gives an unexpectedly higher bolometric luminosity of 310,000±70,000 L☉, close to the empirical upper luminosity limit of red supergiants (i.e. Humphreys–Davidson limit). This implies a higher radius of 2,061 ± 233 R☉ based on an effective temperature of 3,000 K derived using the DUSTY model, considerably larger than the upper radius limit of red supergiants at roughly 1,500 R☉ respectively.[16][6] Older studies frequently calculated even more lower temperatures and an estimated radius of 2,400 R☉.[13]
^Calculated using the following equation: , where mbol is the star's apparent bolometric magnitude and d is the distance in parsecs. The values used for the mbol are 4.29±0.35 and 4.07±0.69, while the value used for the distance is 3,240 parsecs.
^Beauchamp, Alain; Moffat, Anthony F. J.; Drissen, Laurent (1994). "The galactic open cluster NGC 7419 and its five red supergiants". Astrophysical Journal Supplement Series. 93: 187. Bibcode:1994ApJS...93..187B. doi:10.1086/192051.
^ abCutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
^Kukarkin, B. V.; Kholopov, P. N.; Kukarkina, N. P.; Perova, N. B. (1973). "59th Name-List of Variable Stars". Information Bulletin on Variable Stars. 834: 1. Bibcode:1973IBVS..834....1K.
