Astronomy:CK Carinae
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Carina |
| Right ascension | 10h 24m 25.36s[2] |
| Declination | −60° 11′ 29.0″[2] |
| Apparent magnitude (V) | 7.2 - 8.5[3] |
| Characteristics | |
| Spectral type | M3.5 Iab[4] |
| B−V color index | +2.21[2] |
| Variable type | SRc[4] |
| Astrometry | |
| Radial velocity (Rv) | −3.92[5] km/s |
| Proper motion (μ) | RA: −7.351[5] mas/yr Dec.: 2.995[5] mas/yr |
| Parallax (π) | 0.4286 ± 0.0806[5] mas |
| Distance | 2,920+190 −150[6] pc |
| Absolute magnitude (MV) | −6.31[2] |
| Details | |
| Mass | 15[7] M☉ |
| Radius | 690[7] R☉ |
| Luminosity | 72,000[7] L☉ |
| Surface gravity (log g) | 0[7] cgs |
| Temperature | 3,500[7] K |
| Metallicity [Fe/H] | 0.05[8] dex |
| Other designations | |
| Database references | |
| SIMBAD | data |
CK Carinae (CK Car / HD 90382 / SAO 238038) is a variable star in the constellation Carina, the keel of Argo Navis. It is a member of the star association Carina OB1-D, at a distance of around 2,300 parsecs or 7,500 light years.
In 1921, Ida E. Woods discovered that the star's brightness varied.[9] It was given its variable star designation, CK Carinae, in 1922.[10] Classified as a semiregular variable star, CK Carinae's brightness varies between apparent magnitudes +7.2 and +8.5 with a period of approximately 525 days.[3] It has a Gaia Data Release 2 parallax of 0.4286±0.0806 mas,[5] which implies a distance of around 2,300 pc, and is thought to be a member of the Carina OB1-D stellar association which is at a distance of about 2,200 pc.[2][11] An analysis of the distances of apparently-nearby OB stars implies a distance of 2,920 pc for CK Carinae.[6] It has an MK spectral classification of M3.5 Iab, with the luminosity class indicating an intermediate luminosity supergiant.[4]
CK Carinae is a red supergiant with an effective temperature of 3,500 K.[7] It is 690 times larger than the Sun,[7] which means that if it were in the place of the Sun, its surface would reach beyond the orbit of Mars, with Earth being encompassed within the star. Consequently, CK Carinae is also a luminous star, radiating 72,000 times as much energy as the sun.[7]
References
- ↑ "ASAS All Star Catalogue". The All Sky Automated Survey. http://www.astrouw.edu.pl/asas/?page=aasc.
- ↑ 2.0 2.1 2.2 2.3 2.4 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.
- ↑ 3.0 3.1 Kiss, L. L.; Szabó, Gy. M.; Bedding, T. R. (2006). "Variability in red supergiant stars: Pulsations, long secondary periods and convection noise". Monthly Notices of the Royal Astronomical Society 372 (4): 1721–1734. doi:10.1111/j.1365-2966.2006.10973.x. Bibcode: 2006MNRAS.372.1721K.
- ↑ 4.0 4.1 4.2 Samus, N. N. et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S 1. Bibcode: 2009yCat....102025S.
- ↑ 5.0 5.1 5.2 5.3 5.4 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.
- ↑ 6.0 6.1 Davies, Ben; Beasor, Emma R. (March 2020). "The 'red supergiant problem': the upper luminosity boundary of Type II supernova progenitors" (in en). MNRAS 493 (1): 468–476. doi:10.1093/mnras/staa174. Bibcode: 2020MNRAS.493..468D.
- ↑ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 7.7 González-Torà, G.; Wittkowski, M.; Davies, B.; Plez, B. (2024). "The effect of winds on atmospheric layers of red supergiants II. Modelling VLTI/GRAVITY and MATISSE observations of AH Sco, KW SGR, V602 Car, CK Car, and V460 Car". Astronomy & Astrophysics 683: A19. doi:10.1051/0004-6361/202348047. Bibcode: 2024A&A...683A..19G.
- ↑ 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 & Astrophysics 628: A94. doi:10.1051/0004-6361/201935765. Bibcode: 2019A&A...628A..94A.
- ↑ Cannon, A. J.; Leavitt, H. S.; Bailey, S. I. (1921). "Fifty-One New Variable Stars". Harvard College Observatory Circular 225: 1-3. https://articles.adsabs.harvard.edu/full/1921HarCi.225....1C. Retrieved 11 December 2024.
- ↑ Hartwig, Ernst (February 1922). "Benennung von neu entdeckten veränderlichen Sternen". Astronomische Nachrichten 215 (7): 185-194. doi:10.1002/asna.19212150702. Bibcode: 1922AN....215..185H. https://articles.adsabs.harvard.edu/pdf/1922AN....215..185H. Retrieved 11 December 2024.
- ↑ 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.
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