NR Vulpeculae

NR Vulpeculae

The visual band light curve for NR Vulpeculae, plotted from ASAS-SN data[1]
Observation data
Epoch J2000      Equinox J2000
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 mas/yr[2]
Dec.: −6.024±0.023 mas/yr[2]
Parallax (π)0.3225 ± 0.0251 mas[2]
Distance8,844+711
−538 ly
(2,713+218
−165 pc)[5]
Details
Mass23[4][a] M☉
Radius923+62
−50[6] R☉
Luminosity197,000[7] L☉
Surface gravity (log g)−0.20[4] cgs
Temperature3,986[7] K
Metallicity [Fe/H]+0.093[8] dex
Other designations
NR Vulpeculae, TYC 2144-1244-1, GSC 02144-01244, IRC+20438, 2MASS J19501193+2455240, IRAS 19480+2447, AAVSO 1946+24, BD+24 3902, HD 339034, RAFGL 2462, UCAC2 40577951
Database references
SIMBADdata

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 difference spectral type of K3I, meaning that it is a K-type supergiant star.[4] NR Vulpeculae has expanded to 920[6] times the Sun's size and is currently emitting 200,000 times its luminosity.[7] If placed in the Solar System, its photosphere would reach beyond Mars' orbit. It has a cool surface temperature of around 4,000 K,[7] giving it the typical orange color of a K-type star.[9]

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

  1. ^ Calculated using the star's absolute bolometric magnitude of −8.63 in the following equation:
    log(M) = 0.50−0.1 • Mbol.
    This results in a mass logarithm of 1.363, and 101.363 is equal to 23 solar masses.

References

  1. ^ "ASAS-SN Variable Stars Database". ASAS-SN Variable Stars Database. ASAS-SN. Retrieved 6 January 2022.
  2. ^ 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.
  3. ^ a b c d e NR Vul, database entry, The combined table of GCVS Vols I-III and NL 67-78 with improved coordinates, General Catalogue of Variable Stars Archived 2017-06-20 at the Wayback Machine, Sternberg Astronomical Institute, Moscow, Russia. Accessed on line November 12, 2010.
  4. ^ a b c d e f 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. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901. S2CID 15109583.
  5. ^ Bailer-Jones, C. A. L.; Rybizki, J.; Fouesneau, M.; Demleitner, M.; Andrae, R. (2021-03-01). "Estimating distances from parallaxes. V: Geometric and photogeometric distances to 1.47 billion stars in Gaia Early Data Release 3". The Astronomical Journal. 161 (3): 147. arXiv:2012.05220. Bibcode:2021AJ....161..147B. doi:10.3847/1538-3881/abd806. ISSN 0004-6256. Data about this star can be seen here.
  6. ^ a b Ryan Norris. "Student Science at NMT: Learning Optical Interferometry Through Projects on Evolved Stars" (PDF). CHARA.
  7. ^ a b c d 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.
  8. ^ Anders, F.; Khalatyan, A.; Chiappini, C.; Queiroz, A. B.; Santiago, B. X.; Jordi, C.; Girardi, L.; Brown, A. G. A.; Matijevič, G.; Monari, G.; Cantat-Gaudin, T.; Weiler, M.; Khan, S.; Miglio, A.; Carrillo, I.; Romero-Gómez, M.; Minchev, I.; De Jong, R. S.; Antoja, T.; Ramos, P.; Steinmetz, M.; Enke, H. (2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy and Astrophysics. 628: A94. arXiv:1904.11302. Bibcode:2019A&A...628A..94A. doi:10.1051/0004-6361/201935765. S2CID 131780028.
  9. ^ "The Colour of Stars". Australia National Telescope Facility. Retrieved 2024-05-27.