RS Persei

RS Persei

RS Persei is the red star closest to the centre of NGC 884, the right hand cluster (north is down).
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 2h 22m 24.296s[1]
Declination +57° 06′ 34.10″[1]
Apparent magnitude (V) 7.82-10.0[2]
Characteristics
Spectral type M4Iab[3]
Variable type SRc[2]
Astrometry
Radial velocity (Rv)−38.0±2[4] km/s
Proper motion (μ) RA: −0.602[1] mas/yr
Dec.: −1.107[1] mas/yr
Parallax (π)0.3874 ± 0.0450 mas[1]
Distance4,880+720
−561
 ly
(1,497+221
−172
 pc)[5]
Absolute magnitude (MV)−6.18[6]
Details
Mass12 – 15[7] M
Radius547+9
−7
[5] – 775+110
−85
[8] R
Luminosity59,000[9] L
Surface gravity (log g)−0.2±0.05[7] cgs
Temperature3,470±90[7] K
Other designations
RS Per, HD 14488, BD+56°583, 2MASS J02222428+5706340, AAVSO 0215+56A
Database references
SIMBADdata

RS Persei is a red supergiant variable star located in the Double Cluster in Perseus. The star's apparent magnitude varies from 7.82 to 10.0, meaning it is never visible to the naked eye.

  1. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b Samus', 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. S2CID 16299532.
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  4. ^ Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Washington. Bibcode:1953GCRV..C......0W.
  5. ^ a b Norris, Ryan P. (2019). Seeing Stars Like Never Before: A Long-term Interferometric Imaging Survey of Red Supergiants (PDF) (PhD). Georgia State University.
  6. ^ Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Josselin, Eric; Maeder, Andre; Meynet, Georges (2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not As Cool As We Thought". The Astrophysical Journal. 628 (2): 973–985. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901. S2CID 15109583.
  7. ^ a b c Baron, 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. S2CID 17085548.
  8. ^ Ryan Norris. "Student Science at NMT: Learning Optical Interferometry Through Projects on Evolved Stars" (PDF). CHARA.
  9. ^ Healy, Sarah; Horiuchi, Shunsaku; Molla, Marta Colomer; Milisavljevic, Dan; Tseng, Jeff; Bergin, Faith; Weil, Kathryn; Tanaka, Masaomi (2024-03-23). "Red Supergiant Candidates for Multimessenger Monitoring of the Next Galactic Supernova". Monthly Notices of the Royal Astronomical Society. 529 (4): 3630–3650. arXiv:2307.08785. Bibcode:2024MNRAS.529.3630H. doi:10.1093/mnras/stae738. ISSN 0035-8711.