Astronomy:RS Persei
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| 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[1] mas |
| Distance | approx. 8,400 ly (approx. 2,600 pc) |
| Details | |
| Mass | 12-15[5] M☉ |
| Radius | 491[6] - 547[7] R☉ |
| Luminosity | 33,000 - 34,000[6] L☉ |
| Surface gravity (log g) | −0.2±0.05 cgs |
| Temperature | 3,535±170[6] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
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.
Location
RS Persei is a member of the cluster NGC 884, χ Persei, one half of the famous Double Cluster.[8]
Variability
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.[10]
Properties
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☉.[11] 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.[5]
Even more recent measurements based on its Gaia Data Release 2 parallax gives a luminosity below 40,000 L☉ with a corresponding radius of 491 R☉.[6] 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.[5]
See also
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 Samus', N. N.; Goranskii, V. P.; Durlevich, O. V.; Zharova, A. V.; Kazarovets, E. V.; Kireeva, N. N.; Pastukhova, E. N.; Williams, D. B. et al. (2003). "An Electronic Version of the Second Volume of the General Catalogue of Variable Stars with Improved Coordinates". Astronomy Letters 29 (7): 468. doi:10.1134/1.1589864. Bibcode: 2003AstL...29..468S.
- ↑ Saesen, S.; Carrier, F.; Pigulski, A.; Aerts, C.; Handler, G.; Narwid, A.; Fu, J. N.; Zhang, C. et al. (2010). "Photometric multi-site campaign on the open cluster NGC 884". Astronomy and Astrophysics 515: A16. doi:10.1051/0004-6361/200913236. ISSN 0004-6361. Bibcode: 2010A&A...515A..16S.
- ↑ Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Washington. Bibcode: 1953GCRV..C......0W.
- ↑ 5.0 5.1 5.2 Baron, F.; Monnier, J. D.; Kiss, L. L.; Neilson, H. R.; Zhao, M.; Anderson, M.; Aarnio, A.; Pedretti, E. et al. (2014). "CHARA/MIRC Observations of Two M Supergiants in Perseus OB1: Temperature, Bayesian Modeling, and Compressed Sensing Imaging". The Astrophysical Journal 785 (1): 46. doi:10.1088/0004-637X/785/1/46. Bibcode: 2014ApJ...785...46B.
- ↑ 6.0 6.1 6.2 6.3 Messineo, M.; Brown, A. G. A. (2019). "A Catalog of Known Galactic K-M Stars of Class I Candidate Red Supergiants in Gaia DR2". The Astronomical Journal 158 (1): 20. doi:10.3847/1538-3881/ab1cbd. Bibcode: 2019AJ....158...20M.
- ↑ Norris, Ryan P. (2019). Seeing Stars Like Never Before: A Long-term Interferometric Imaging Survey of Red Supergiants (PDF) (PhD). Georgia State University.
- ↑ 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. doi:10.1051/0004-6361:200809664. Bibcode: 2008A&A...485..303M.
- ↑ "OMC Archive". The Astronomical Data Centre at CAB. https://sdc.cab.inta-csic.es/omc/secure/form_busqueda.jsp?resetForm=true.
- ↑ 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. doi:10.1111/j.1365-2966.2006.10973.x. Bibcode: 2006MNRAS.372.1721K.
- ↑ Cite error: Invalid
<ref>tag; no text was provided for refs namedlevesque - ↑ 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. doi:10.1051/0004-6361/20079063. Bibcode: 2009A&A...498..127V.
- ↑ 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. doi:10.1088/0067-0049/211/1/15. Bibcode: 2014ApJS..211...15Y.
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