Astronomy:V Coronae Borealis
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Short description: Mira-type long period variable star in the constellation Corona Borealis
250px V Coronae Borealis in optical light | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Corona Borealis |
| Right ascension | 15h 49m 31.31220s[1] |
| Declination | +39° 34′ 17.8926″[1] |
| Apparent magnitude (V) | 6.9 - 12.6[2] |
| Characteristics | |
| Evolutionary stage | AGB[3] |
| Spectral type | C6,2e(N2e)[4] |
| Variable type | Mira[2] |
| Astrometry | |
| Proper motion (μ) | RA: +5.905[1] mas/yr Dec.: −15.089[1] mas/yr |
| Parallax (π) | 1.1378 ± 0.0238[1] mas |
| Distance | 2,870 ± 60 ly (880 ± 20 pc) |
| Details[5] | |
| Radius | 750[lower-alpha 1] R☉ |
| Luminosity | 5,300 L☉ |
| Temperature | 1,800 K |
| Other designations | |
| Database references | |
| SIMBAD | data |
V Coronae Borealis (V CrB) is a Mira-type long period variable star and carbon star in the constellation Corona Borealis. Its apparent magnitude varies between 6.9 and 12.6 over a period of 357 days.[4]
Based on a period of 357 days, the absolute magnitude of V Coronae Borealis has been calculated to be -4.62.[8] It is estimated to be 880 pc (2,900 ly) from Earth based on parallax, has a luminosity of 5,300 L☉ and a rather cool effective temperature of 1,800 K, these implying a very large radius of about 750 R☉, making V Coronae Borealis one of the largest stars so far discovered.[5] If placed in the center of the Solar System, its size would engulf all rocky planets and reach parts of the asteroid belt.
Notes
- ↑ Applying the Stefan–Boltzmann law with a nominal solar effective temperature of 5,772 K:
References
- ↑ 1.0 1.1 1.2 1.3 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 Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports 61 (1): 80. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S.
- ↑ Hoai, Do Thi; Nhung, Pham Tuyet; Darriulat, Pierre; Tan, Mai Nhat (2025). "Stellar Evolution Along the Asymptotic Giant Branch as Revealed by the Shape of Miras' Visual Light Curves". The Astrophysical Journal 982 (2): 201. doi:10.3847/1538-4357/adb8d9. Bibcode: 2025ApJ...982..201H.
- ↑ 4.0 4.1 VSX (4 January 2010). "V Coronae Borealis". AAVSO Website. American Association of Variable Star Observers. http://www.aavso.org/vsx/index.php?view=detail.top&oid=10604.
- ↑ 5.0 5.1 Danilovich, T.; Teyssier, D.; Justtanont, K.; Olofsson, H.; Cerrigone, L.; Bujarrabal, V.; Alcolea, J.; Cernicharo, J. et al. (2015-09-01). "New observations and models of circumstellar CO line emission of AGB stars in the Herschel SUCCESS programme". Astronomy and Astrophysics 581: A60. doi:10.1051/0004-6361/201526705. ISSN 0004-6361. Bibcode: 2015A&A...581A..60D.
- ↑ "V Coronae Borealis". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V+CrB&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id.
- ↑ "Download Data". AAVSO. https://www.aavso.org/data-download.
- ↑ Guandalini, R.; Cristallo, S. (2013). "Luminosities of carbon-rich asymptotic giant branch stars in the Milky Way". Astronomy & Astrophysics 555: 7. doi:10.1051/0004-6361/201321225. A120. Bibcode: 2013A&A...555A.120G.
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