IX Carinae

IX Carinae

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]
Distance7,400 ± 400 ly
(2,300 ± 100 pc)
Details
Mass13[6] M☉
Radius603[7] R☉
Luminosity61,660[7] L☉
Temperature3,660±170[8] 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
SIMBADdata

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.[9][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,[10][8] while its bolometric luminosity is between 34,000 L☉[11] and 134,000 L☉.[10] It is one of the largest stars with a radius of approximately 600 R☉ (420,000,000 km; 2.8 au). If placed at the center of the Solar System, it would extend close to the orbit of the outer asteroid belt.[7]

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.[12]

  1. ^ Cite error: The named reference ASASServer was invoked but never defined (see the help page).
  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 Cite error: The named reference gcvs was invoked but never defined (see the help page).
  4. ^ a b c d "IX Carinae". AAVSO. Retrieved 2022-06-16.
  5. ^ Cite error: The named reference gontcharov was invoked but never defined (see the help page).
  6. ^ Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (2022). "Stellar and substellar companions from Gaia EDR3". Astronomy & Astrophysics. 657: A7. arXiv:2109.10912. Bibcode:2022A&A...657A...7K. doi:10.1051/0004-6361/202142146. S2CID 237605138.
  7. ^ a b c 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. ^ a b 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.
  9. ^ 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.
  10. ^ a b 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.
  11. ^ 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.
  12. ^ 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.