Astronomy:NR Vulpeculae
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Vulpecula |
| Right ascension | 19h 50m 11.928s[2] |
| Declination | 24° 55′ 24.18″[2] |
| Apparent magnitude (V) | 9.13 - 9.61[3] |
| Characteristics | |
| Evolutionary stage | red supergiant[4] |
| Spectral type | M1Ia[3] or K3I[4] |
| Variable type | LC[3] |
| Astrometry | |
| Radial velocity (Rv) | 11.58±0.33[2] km/s |
| Proper motion (μ) | RA: −2.023±0.016[2] mas/yr Dec.: −6.024±0.023[2] mas/yr |
| Parallax (π) | 0.3225 ± 0.0251[2] mas |
| Distance | 8,844+711 −538 ly (2,713+218 −165 pc) |
| Details | |
| Mass | 23[4][lower-alpha 1] M☉ |
| Radius | 923+62 −50[5] R☉ |
| Luminosity | 197,000[6] L☉ |
| Surface gravity (log g) | −0.20[4] cgs |
| Temperature | 3,986[6] K |
| Metallicity [Fe/H] | +0.093[7] dex |
| Other designations | |
| Database references | |
| SIMBAD | data |
NR Vulpeculae is a red supergiant and irregular variable star in the constellation Vulpecula. It has an apparent magnitude varying between 9.13 and 9.61, which is too faint to be seen to the naked eye.
Characteristics
It has an spectral classification of M1Ia, meaning that it is a supergiant star of higher luminosity and spectral type M.[3] Levesque et al. (2005) published a different spectral type of K3I, meaning that it is a K-type supergiant star.[4] NR Vulpeculae has expanded to 920[5] times the Sun's size and is currently emitting 200,000 times its luminosity.[6] If placed in the Solar System, its photosphere would reach beyond Mars' orbit. It has a cool surface temperature of around 4,000 K,[6] giving it the typical orange color of a K-type star.[8]
NR Vulpeculae is also a slow irregular variable, with an apparent magnitude ranging from 9.13 to 9.61.[3]
It is considered a likely member of the Vulpecula OB1 stellar association.[4]
Notes
- ↑ Calculated using the star's absolute bolometric magnitude of −8.63 in the following equation:
log(M) = 0.50−0.1
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This results in a mass logarithm of 1.363, and 101.363 is equal to 23 solar masses.
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 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.
- ↑ 3.0 3.1 3.2 3.3 3.4 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 4.2 4.3 4.4 4.5 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.
- ↑ 5.0 5.1 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.
- ↑ 6.0 6.1 6.2 6.3 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.
- ↑ 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.
- ↑ "The Colour of Stars". https://www.atnf.csiro.au/outreach/education/senior/astrophysics/photometry_colour.html.
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