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IX Carinae

This article will address IX Carinae, a topic of great relevance and interest today. IX Carinae is an issue that has generated debate and controversy in different areas, awakening the interest of experts, academics and the general public. Over the years, IX Carinae has gained increasing importance due to its impact on society and people's daily lives. In this context, it is pertinent to analyze IX Carinae in detail, exploring its different facets, implications and possible solutions. Likewise, we will seek to offer an objective and enriching perspective on IX Carinae, in order to promote a constructive dialogue and foster greater understanding of this topic.

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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.

In 1948, Daniel Joseph Kelly O'Connell announced that the star is a variable star.[9] 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.[10][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,[11][8] while its bolometric luminosity is between 34,000 L☉[12] and 134,000 L☉.[11] 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.[13]

References

  1. ^ "ASAS All Star Catalogue". The All Sky Automated Survey. Retrieved 8 December 2021.
  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 "GCVS Query=IX Car". General Catalogue of Variable Stars @ Sternberg Astronomical Institute, Moscow, Russia. Retrieved 2018-01-14.
  4. ^ a b c d "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. 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. ^ O'Connell, D (February 1948). "New Variable Stars (Fourth List)". Publications of the Riverview College Observatory. 2: 68. Bibcode:1948PRCO....2...68O. Retrieved 13 December 2024.
  10. ^ 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.
  11. ^ 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.
  12. ^ 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.
  13. ^ 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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