RS Persei is a large cool star with a temperature of 3,500 K. Its size makes it luminous, although much of its radiation is emitted in theinfrared. In 2005, RS Per was calculated to have a bolometric luminosity of 145,000 L☉ and a radius around 1,000 R☉.[6] More recently, across all wavelengths gives the star a lower luminosity of77,600+9,500 −8,400L☉, and a radius of770±30 R☉ based on the distance and the measuredangular diameter by theCHARA array.[5] A 2023 paper gives an even smaller luminosity of 59,000 L☉.[12] Estimates based on measured angular diameters and distances estimated by theGaia DR2 andGaia DR3 give radii of547+9 −7R☉[13] and775+110 −85R☉.[14]
RS Persei has sometimes been considered to be a highly evolved low massAsymptotic Giant Branch (AGB) star,[15] but calculations of its current mass suggest that it is a true red supergiant. NGC 244 is also too young to host AGB stars.[5]
^abcSamus', N. N.; Goranskii, V. P.; Durlevich, O. V.; Zharova, A. V.; Kazarovets, E. V.; Kireeva, N. N.; Pastukhova, E. N.; Williams, D. B.; Hazen, M. L. (2003). "An Electronic Version of the Second Volume of the General Catalogue of Variable Stars with Improved Coordinates".Astronomy Letters.29 (7): 468.Bibcode:2003AstL...29..468S.doi:10.1134/1.1589864.S2CID16299532.
^Saesen, S.; Carrier, F.; Pigulski, A.; Aerts, C.; Handler, G.; Narwid, A.; Fu, J. N.; Zhang, C.; Jiang, X. J.; Vanautgaerden, J.; Kopacki, G.; Stęślicki, M.; Acke, B.; Poretti, E.; Uytterhoeven, K.; Gielen, C.; Østensen, R.; De Meester, W.; Reed, M. D.; Kołaczkowski, Z.; Michalska, G.; Schmidt, E.; Yakut, K.; Leitner, A.; Kalomeni, B.; Cherix, M.; Spano, M.; Prins, S.; Van Helshoecht, V.; Zima, W.; Huygen, R.; Vandenbussche, B.; Lenz, P.; Ladjal, D.; Puga Antolín, E.; Verhoelst, T.; De Ridder, J.; Niarchos, P.; Liakos, A.; Lorenz, D.; Dehaes, S.; Reyniers, M.; Davignon, G.; Kim, S.-L.; Kim, D. H.; Lee, Y.-J.; Lee, C.-U.; Kwon, J.-H.; Broeders, E.; Van Winckel, H.; Vanhollebeke, E.; Waelkens, C.; Raskin, G.; Blom, Y.; Eggen, J. R.; Degroote, P.; Beck, P.; Puschnig, J.; Schmitzberger, L.; Gelven, G. A.; Steininger, B.; Blommaert, J.; Drummond, R.; Briquet, M.; Debosscher, J. (2010). "Photometric multi-site campaign on the open cluster NGC 884".Astronomy and Astrophysics.515: A16.arXiv:1001.1116.Bibcode:2010A&A...515A..16S.doi:10.1051/0004-6361/200913236.ISSN0004-6361.S2CID40932414.
^Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities".Washington.Bibcode:1953GCRV..C......0W.
^abcdBaron, F.; Monnier, J. D.; Kiss, L. L.; Neilson, H. R.; Zhao, M.; Anderson, M.; Aarnio, A.; Pedretti, E.; Thureau, N.; Ten Brummelaar, T. A.; Ridgway, S. T.; McAlister, H. A.; Sturmann, J.; Sturmann, L.; Turner, N. (2014). "CHARA/MIRC Observations of Two M Supergiants in Perseus OB1: Temperature, Bayesian Modeling, and Compressed Sensing Imaging".The Astrophysical Journal.785 (1): 46.arXiv:1405.4032.Bibcode:2014ApJ...785...46B.doi:10.1088/0004-637X/785/1/46.S2CID17085548.
