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 603 [7]   R☉
Luminosity 61,660 [7]   L☉
Temperature 3,660±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
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. [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]

Related Research Articles

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Scutum is a small constellation. Its name is Latin for shield, and it was originally named Scutum Sobiescianum by Johannes Hevelius in 1684. Located just south of the celestial equator, its four brightest stars form a narrow diamond shape. It is one of the 88 IAU designated constellations defined in 1922.

<span class="mw-page-title-main">V520 Carinae</span> Star in the constellation Carina

V520 Carinae is a single star in the southern constellation of Carina. It has the Bayer designation w Carinae, while V520 Carinae is a variable star designation. The star has an orange hue and is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around +4.58. It is located at a distance of approximately 1,140 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +9 km/s. It is a candidate member of the IC 2391 moving group of co-moving stars.

<span class="mw-page-title-main">AG Carinae</span> Luminous variable star in the constellation Carina

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<span class="mw-page-title-main">MY Cephei</span> Star in the constellation Cepheus

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<span class="mw-page-title-main">HR Carinae</span> Star in the constellation Carina

HR Carinae is a luminous blue variable star located in the constellation Carina. It is surrounded by a vast nebula of ejected nuclear-processed material because this star has a multiple shell expanding atmosphere. This star is among the most luminous stars in the Milky Way. It has very broad emission wings on the Balmer lines, reminiscent from the broad lines observed in the spectra of O and Wolf–Rayet stars. A distance of 5 kpc and a bolometric magnitude of −9.4 put HR Car among the most luminous stars of the galaxy.

<span class="mw-page-title-main">V381 Cephei</span> Triple star system in the constellation Cepheus

V381 Cephei is a triple star system in the northern constellation of Cepheus. Its apparent magnitude is slightly variable between 5.5 and 5.7.

<span class="mw-page-title-main">V602 Carinae</span> Star in the constellation Carina

V602 Carinae is a red supergiant and variable star of spectral type M3 in the constellation Carina. It is considered to be one of largest known stars, being around 1,000 times larger than the Sun.

<span class="mw-page-title-main">RT Carinae</span> Star in the constellation Carina

RT Carinae, also known as CD-58 3538, is a red supergiant and a variable star, located 7,000 light years away in the constellation Carina. It is in the Carina Nebula. The average apparent magnitude of +8.55, too faint to be visible to the naked eye.

<span class="mw-page-title-main">TZ Cassiopeiae</span> Star in the constellation Cassiopeia

TZ Cassiopeiae(TZ Cas, HIP 117763, SAO 20912) is a variable star in the constellation Cassiopeia with an apparent magnitude of around +9 to +10. It is approximately 8,400 light-years away from Earth. The star is a red supergiant star with a spectral type of M3 and a temperature around 3,600 K.

145 G. Canis Majoris is a single K giant or supergiant star in the southern constellation of Canis Major. This star is Gould's 145th of Canis Major in his Uranometria Argentina. Kostjuk erroneously lists it as simply "145 CMa". SIMBAD follows this error in its object query result as "* 145 CMa – Star".

<span class="mw-page-title-main">PZ Cassiopeiae</span> Star in the constellation Cassiopeia

PZ Cassiopeiae is a red supergiant star located in the constellation of Cassiopeia, and a semi-regular variable star.

<span class="mw-page-title-main">UY Scuti</span> Star in the constellation Scutum

UY Scuti (BD-12°5055) is a red supergiant star, located 5,900 light-years away in the constellation Scutum. It is also a pulsating variable star, with a maximum brightness of magnitude 8.29 and a minimum of magnitude 10.56, which is too dim for naked-eye visibility. It is considered to be one of the largest known stars, with a radius estimated at 909 solar radii, thus a volume of 750 million times that of the Sun. This estimate implies if it were placed at the center of the Solar System, its photosphere would extend past the orbit of Mars or even the asteroid belt.

<span class="mw-page-title-main">RS Persei</span> Star in the constellation Perseus

RS Persei is a red supergiant variable star located in the Double Cluster in Perseus. The star's apparent magnitude varies from 7.82 to 10.0, meaning it is never visible to the naked eye.

<span class="mw-page-title-main">EV Carinae</span> Red supergiant star in the constellation Carina

EV Carinae is a red supergiant and pulsating variable star of spectral type M4Ia in the constellation Carina. It is a semiregular variable star with its apparent magnitude varying between 7.4 and 9.0 in the visible band, making it only seen by binoculars or a telescope. Various periods have been identified, but the dominant one is around 347 days. It is an MK spectral standard star for the class M4.5Ia.

<span class="mw-page-title-main">BC Cygni</span> Star in the constellation Cygnus

BC Cygni is a red supergiant and pulsating variable star of spectral type M3.5Ia in the constellation Cygnus.

<span class="mw-page-title-main">CK Carinae</span> Red supergiant star in the constellation Carina

CK Carinae 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.

<span class="mw-page-title-main">U Lacertae</span> Binary star in the constellation Lacerta

U Lacertae is a spectroscopic binary star in the constellation Lacerta.

<span class="mw-page-title-main">V528 Carinae</span> Star in the constellation Carina

V528 Carinae is a variable star in the constellation Carina.

<span class="mw-page-title-main">BO Carinae</span> Star in the constellation Carina

BO Carinae, also known as HD 93420, is an irregular variable star in the constellation Carina.

<span class="mw-page-title-main">NR Vulpeculae</span> Star in the constellation Vulpecula

NR Vulpeculae is a red supergiant and irregular variable star in the constellation Vulpecula. It has an apparent magnitude varying between 9.13 and 9.61, which is too faint to be seen to the naked eye.

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. arXiv: 2109.10912 . Bibcode:2022A&A...657A...7K. doi: 10.1051/0004-6361/202142146 . S2CID   237605138.
  7. 1 2 3 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. 1 2 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. 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.
  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.


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