Astronomy:RS Persei
300px RS Persei is the red star closest to the centre of NGC 884, the right hand cluster (north is down). | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Perseus |
| Right ascension | 02h 22m 24.296s[1] |
| Declination | +57° 06′ 34.10″[1] |
| Apparent magnitude (V) | 7.82 – 10.0[2] |
| Characteristics | |
| Evolutionary stage | Red supergiant |
| 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 | 7,650±180 ly (2,345±55 pc) |
| Details[5] | |
| Mass | 12 – 15 M☉ |
| Radius | 770±30 R☉ |
| Luminosity | 77,600+9,500 −8,400 L☉ |
| Surface gravity (log g) | −0.2±0.05 cgs |
| Temperature | 3,470±90 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. It is a member of the cluster NGC 884, χ Persei, one half of the famous Double Cluster.[6]
Variability
In March of 1904, Lidiya Tseraskaya discovered that the star, then referred to as BD+56°583, is a variable star.[8] It was listed with its variable star designation, RS Persei, in Annie Jump Cannon's 1907 work Second Catalog of Variable Stars.[9] 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. Its size 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, across all wavelengths gives the star a lower luminosity of 77,600+9,500
−8,400 L☉, and a radius of 770±30 R☉ based on the distance and the measured angular diameter by the CHARA 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 the Gaia DR2 and Gaia DR3 give radii of 547+9
−7 R☉[13] and 775+110
−85 R☉.[14]
RS Persei has sometimes been considered to be a highly evolved low mass Asymptotic 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]
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.
- ↑ 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.
- ↑ Ceraski, W. (April 1904). "Une nouvelle variable 16.1904 Persei au cluster χ Persei". Astronomische Nachrichten 165 (8): 125–126. doi:10.1002/asna.19041650805. Bibcode: 1904AN....165..125C.
- ↑ Cannon, Annie J. (1907). "Second catalogue of variable stars". Annals of Harvard College Observatory 55: 1–94. Bibcode: 1907AnHar..55....1C.
- ↑ 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 - ↑ 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. doi:10.1093/mnras/stae738. ISSN 0035-8711. Bibcode: 2024MNRAS.529.3630H.
- ↑ Norris, Ryan P. (2019). Seeing Stars Like Never Before: A Long-term Interferometric Imaging Survey of Red Supergiants (PDF) (PhD). Georgia State University.
- ↑ Ryan Norris. "Student Science at NMT: Learning Optical Interferometry Through Projects on Evolved Stars". CHARA. https://www.chara.gsu.edu/files/2023Meeting/Norris_NMT_Students_2023.pdf.
- ↑ 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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