IX Carinae

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IX Carinae
IXCarLightCurve.png
A visual band light curve for IX Carinae, plotted from ASAS data [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Carina
Right ascension 10h 50m 26.300s [2]
Declination 59° 58′ 56.57″ [2]
Apparent magnitude  (V)7.2 - 8.5 [3] or 6.87 - 7.9 [4]
Characteristics
Spectral type M2Iab [3]
Variable type SRc [3] [4]
Astrometry
Radial velocity (Rv)0.90±1.8 [5]  km/s
Proper motion (μ)RA: –6.466 [2]   mas/yr
Dec.: 2.322 [2]   mas/yr
Parallax (π)0.4436 ± 0.0220  mas [2]
Distance 7,400 ± 400  ly
(2,300 ± 100  pc)
Details
Mass 13 [6]   M☉
Radius 566 [7]   R☉
Luminosity 52,000 [7]   L☉
Temperature 3,660±170 [7]   K
Other designations
IX Car, CD-59°3368, CPD-59°2775, GSC 08626-01670, HD 94096, HIP 52991, IRAS 10484-5943, 2MASS J10502630-5958563, PPM 339497, SAO 238523, TYC 8626-1670-1
Database references
SIMBAD data

IX Carinae (IX Car) is a red supergiant and pulsating variable star of spectral type M2Iab in the constellation Carina. It is a member of the Carina OB1 association along the Carina Nebula.

IX Carinae is a semiregular variable star, but its properties are poorly-defined. Different sources give its brightness range as magnitude 7.2 to 8.5. [3] or 6.87 to 7.9. [4] The International Variable Star Index finds a period of approximately 384 days from ASAS-3 and visual observations, but also gives a possible period of 108 days. [4] Another analysis finds a primary period of 408±50  d and a longer secondary period of 4,400±2,000 d. [8] [3]

The physical characteristics of IX Carinae are also only known approximately, partly because of an uncertain distance. The effective temperature is around 3,600  K , [9] [7] while its bolometric luminosity is between 34,000  L☉ [10] and 134,000 L☉. [9] It is one of the largest stars with a radius of approximately 566  R☉ (394,000,000  km ; 2.63  au ). [7] If placed at the center of the Solar System, it would extend close to the orbit of the outer Asteroid Belt Jupiter.

IX Carinae has been listed as a candidate supernova close enough to Earth that pre-collapse neutrinos could be detected, allowing for observations of the star to be made from before the supernova explosion. [11]

Related Research Articles

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References

  1. ↑ "ASAS All Star Catalogue". The All Sky Automated Survey. Retrieved 8 December 2021.
  2. 1 2 3 4 5 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 "GCVS Query=IX Car". General Catalogue of Variable Stars @ Sternberg Astronomical Institute, Moscow, Russia . Retrieved 2018-01-14.
  4. 1 2 3 4 "IX Carinae". AAVSO . Retrieved 2022-06-16.
  5. ↑ Gontcharov, G. A.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Josselin, Eric; Maeder, Andre; Meynet, Georges (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID   119231169.
  6. ↑ Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (2022). "Stellar and substellar companions from Gaia EDR3". Astronomy & Astrophysics. 657: A7. Bibcode:2022A&A...657A...7K. doi: 10.1051/0004-6361/202142146 . S2CID   237605138.
  7. 1 2 3 4 5 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. arXiv: 1905.03744 . Bibcode:2019AJ....158...20M. doi: 10.3847/1538-3881/ab1cbd . S2CID   148571616.
  8. ↑ Percy, John R.; Sato, Hiromitsu (2009). "Long Secondary Periods in Pulsating Red Supergiant Stars". Journal of the Royal Astronomical Society of Canada. 103 (1): 11. Bibcode:2009JRASC.103...11P.
  9. 1 2 Dorn-Wallenstein, Trevor Z.; Levesque, Emily M.; Neugent, Kathryn F.; Davenport, James R. A.; Morris, Brett M.; Gootkin, Keyan (2020). "Short Term Variability of Evolved Massive Stars with TESS II: A New Class of Cool, Pulsating Supergiants". The Astrophysical Journal. 902 (1): 24. arXiv: 2008.11723 . Bibcode:2020ApJ...902...24D. doi: 10.3847/1538-4357/abb318 . S2CID   221340538.
  10. ↑ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR .
  11. ↑ Nakamura, Ko; Horiuchi, Shunsaku; Tanaka, Masaomi; Hayama, Kazuhiro; Takiwaki, Tomoya; Kotake, Kei (2016). "Multimessenger signals of long-term core-collapse supernova simulations: Synergetic observation strategies". Monthly Notices of the Royal Astronomical Society. 461 (3): 3296. arXiv: 1602.03028 . Bibcode:2016MNRAS.461.3296N. doi:10.1093/mnras/stw1453.


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