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.
| 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] |
| Distance | 4,880+720 −561 ly (1,497+221 −172 pc)[5] |
| Absolute magnitude (MV) | −6.18[6] |
| Details | |
| Mass | 12 – 15[7] M☉ |
| Radius | 547+9 −7[5] R☉ |
| Luminosity | 59,000[8] L☉ |
| Surface gravity (log g) | −0.2±0.05[7] cgs |
| Temperature | 3,470±90[7] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
Location edit
RS Persei is a member of the cluster NGC 884, χ Persei, one half of the famous Double Cluster.[9]
Variability edit
RS Persei is classified as a semiregular variable star, with its brightness varying from magnitude 7.82 to 10.0 over 245 days,[2] Detailed studies show that it also pulsates with a long secondary period of 4,200±1,500 days.[11]
Properties edit
RS Persei is a large cool star with a temperature of 3,500 K. This makes it luminous, although much of its radiation is emitted in the infrared. 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, 2014 calculations across all wavelengths gives the star a lower luminosity of 77,600+9,500
−8,400 L☉ based on an assumed distance, and a radius of 770±30 R☉ based on the measured angular diameter and luminosity.[7] A 2023 paper gives an even smaller luminosity of 59,000 L☉.
[8]
The angular diameter of RS Persei was measured at 3.4±0.03 mas. At a distance of 1497 parsecs, this corresponds to a radius of 547 R☉.[5] It is surrounded by dust that has condensed from material lost by the star.[12]
RS Persei has sometimes been considered to be a highly evolved low mass Asymptotic Giant Branch (AGB) star,[13] but calculations of its current mass suggest that it is a low mass supergiant. NGC 244 is also too young to host AGB stars.[7]
See also edit
References edit
- ^ 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.
- ^ a b c 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.
- ^ 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. ISSN 0004-6361. S2CID 40932414.
- ^ Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Washington. Bibcode:1953GCRV..C......0W.
- ^ a b c Norris, Ryan P. (2019). Seeing Stars Like Never Before: A Long-term Interferometric Imaging Survey of Red Supergiants (PDF) (PhD). Georgia State University.
- ^ a b 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.
- ^ a b c d e 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.
- ^ a b 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.
- ^ Mermilliod, J. C.; Mayor, M.; Udry, S. (2008). "Red giants in open clusters. XIV. Mean radial velocities for 1309 stars and 166 open clusters". Astronomy and Astrophysics. 485 (1): 303–314. Bibcode:2008A&A...485..303M. doi:10.1051/0004-6361:200809664.
- ^ "OMC Archive". OMC Archive. The Astronomical Data Centre at CAB. Retrieved 19 December 2021.
- ^ Kiss, L. L.; Szabó, Gy. M.; Bedding, T. R. (2006). "Variability in red supergiant stars: Pulsations, long secondary periods and convection noise". Monthly Notices of the Royal Astronomical Society. 372 (4): 1721–1734. arXiv:astro-ph/0608438. Bibcode:2006MNRAS.372.1721K. doi:10.1111/j.1365-2966.2006.10973.x. S2CID 5203133.
- ^ Verhoelst, T.; Van Der Zypen, N.; Hony, S.; Decin, L.; Cami, J.; Eriksson, K. (2009). "The dust condensation sequence in red supergiant stars". Astronomy and Astrophysics. 498 (1): 127–138. arXiv:0901.1262. Bibcode:2009A&A...498..127V. doi:10.1051/0004-6361/20079063. S2CID 18383796.
- ^ Yoon, Dong-Hwan; Cho, Se-Hyung; Kim, Jaeheon; Yun, Young joo; Park, Yong-Sun (2014). "SiO and H2O Maser Survey toward Post-asymptotic Giant Branch and Asymptotic Giant Branch Stars". The Astrophysical Journal Supplement. 211 (1): 15. Bibcode:2014ApJS..211...15Y. doi:10.1088/0067-0049/211/1/15. S2CID 73561291.