NR Vulpeculae

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NR Vulpeculae
NRVulLightCurve.png
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]
Distance 8,844+711
−538  ly
(2,713+218
−165  pc) [5]
Details
Mass 23 [4] [lower-alpha 1]   M☉
Radius 923+62
−50 [6]   R☉
Luminosity 197,000 [7]   L☉
Surface gravity (log g)−0.20 [4]   cgs
Temperature 3,986 [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
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.

Contents

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.

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References

  1. ↑ "ASAS-SN Variable Stars Database". ASAS-SN Variable Stars Database. ASAS-SN. Retrieved 6 January 2022.
  2. 1 2 3 4 5 6 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. 1 2 3 4 5 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. 1 2 3 4 5 6 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. 1 2 Ryan Norris. "Student Science at NMT: Learning Optical Interferometry Through Projects on Evolved Stars" (PDF). CHARA.
  7. 1 2 3 4 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.
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