Astronomy:NR Vulpeculae
From HandWiki
Short description: Star in the constellation Vulpecula
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Vulpecula |
| Right ascension | 19h 50m 11.9280s[2] |
| Declination | 24° 55′ 24.1775″[2] |
| Apparent magnitude (V) | 9.13 - 9.61[3] |
| Characteristics | |
| Evolutionary stage | Red supergiant[4] |
| Spectral type | M1Ia[3] |
| Variable type | LC[3] |
| Astrometry | |
| Proper motion (μ) | RA: −2.320±0.073[2] mas/yr Dec.: −5.807±0.071[2] mas/yr |
| Parallax (π) | 0.5633 ± 0.0516[2] mas |
| Distance | 5,800 ± 500 ly (1,800 ± 200 pc) |
| Details | |
| Mass | 4.92[5] M☉ |
| Radius | 553[6] R☉ |
| Luminosity | 111,000[7] - 223,000[4] L☉ |
| Surface gravity (log g) | −0.13[5] cgs |
| Temperature | 3,986±170[6] K |
| Metallicity [Fe/H] | +0.093[5] dex |
| Other designations | |
| Database references | |
| SIMBAD | data |
NR Vulpeculae is a red supergiant and irregular variable star in the constellation Vulpecula. It has an effective temperature around 4,000 K, a radius of 553 times larger than the sun, which means that if it were in the place of the Sun, its surface would reach beyond Mars's orbit. Consequently, NR Vulpeculae is also a luminous star, radiating 111,000 - 223,000 times as much energy as the sun. It is considered a likely member of the Vulpecula OB1 stellar association.[8]
References
- ↑ "ASAS-SN Variable Stars Database". ASAS-SN. https://asas-sn.osu.edu/variables/lookup.
- ↑ 2.0 2.1 2.2 2.3 2.4 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 NR Vul, database entry, The combined table of GCVS Vols I-III and NL 67-78 with improved coordinates, General Catalogue of Variable Stars , Sternberg Astronomical Institute, Moscow, Russia. Accessed on line November 12, 2010.
- ↑ 4.0 4.1 Dorn-Wallenstein, Trevor Z.; Levesque, Emily M.; Neugent, Kathryn F.; Davenport, James R. A.; Morris, Brett M.; Gootkin, Keyan (2020), "Short-term Variability of Evolved Massive Stars with TESS. II. A New Class of Cool, Pulsating Supergiants", The Astrophysical Journal 902 (1): 24, doi:10.3847/1538-4357/abb318, Bibcode: 2020ApJ...902...24D
- ↑ 5.0 5.1 5.2 Anders, F.; Khalatyan, A.; Chiappini, C.; Queiroz, A. B.; Santiago, B. X.; Jordi, C.; Girardi, L.; Brown, A. G. A. et al. (2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy and Astrophysics 628: A94. doi:10.1051/0004-6361/201935765. Bibcode: 2019A&A...628A..94A.
- ↑ 6.0 6.1 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.
- ↑ Mauron, N.; Josselin, E. (2011). "The mass-loss rates of red supergiants and the de Jager prescription". Astronomy and Astrophysics 526: A156. doi:10.1051/0004-6361/201013993. Bibcode: 2011A&A...526A.156M.
- ↑ Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Josselin, Eric; Maeder, Andre; Meynet, Georges (August 2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not As Cool As We Thought". The Astrophysical Journal 628 (2): 973–985. doi:10.1086/430901. Bibcode: 2005ApJ...628..973L.
 |  |
