WOH G64

WOH G64

VLTI image of the dusty torus around the star.
Credit: ESO
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Dorado (LMC)
Right ascension 04h 55m 10.5252s[1]
Declination −68° 20′ 29.998″[1]
Apparent magnitude (V) 17.7 - 18.8[2]
Characteristics
Evolutionary stage OH/IR red supergiant
Spectral type M5 I[3] – M7.5e[4][5]
Apparent magnitude (K) 6.849[6]
Apparent magnitude (R) 15.69[7]
Apparent magnitude (G) 15.0971[1]
Apparent magnitude (I) 12.795[8]
Apparent magnitude (J) 9.252[6]
Apparent magnitude (H) 7.745[6]
Variable type Carbon-rich LPV (Mira?)[8]
Astrometry
Radial velocity (Rv)294±2[3] km/s
Proper motion (μ) RA: 1.108[1] mas/yr
Dec.: −1.348[1] mas/yr
Parallax (π)−0.2280 ± 0.0625 mas[1]
Distance160,000 ly
(50,000[3] pc)
Absolute magnitude (MV)−6.00[3]
Details
Mass25±5 (initial mass)[3] M☉
Radius1,540±77[3][9][10] R☉
Luminosity282,000+34,400
−30,700[3] L☉
Surface gravity (log g)+0.0[11]–−0.5[3] cgs
Temperature3,400±25[3] K
Age≤5[12] Myr
Other designations
WOH G064, 2MASS J04551048-6820298, IRAS 04553-6825, MSX LMC 1182
Database references
SIMBADdata

WOH G64 (IRAS 04553-6825) is an unusual[3] red supergiant (RSG) star in the Large Magellanic Cloud (LMC) satellite galaxy in the southern constellation of Dorado. It is the largest known star with a well-defined radius.[3][13] It is also one of the most luminous and massive red supergiants, with a radius calculated to be around 1,540 times that of the Sun (R☉) and a luminosity around 282,000 times the solar luminosity (L☉). If placed at the center of the Solar System, the star's photosphere would engulf the orbit of Jupiter.

WOH G64 is surrounded by an optically thick dust envelope of roughly a light year in diameter containing 3 to 9 times the Sun's mass of expelled material that was created by the strong stellar wind.[14]

  1. ^ a b c d e f Cite error: The named reference dr2 was invoked but never defined (see the help page).
  2. ^ Bhardwaj, Anupam; Kanbur, Shashi; He, Shiyuan; Rejkuba, Marina; Matsunaga, Noriyuki; De Grijs, Richard; Sharma, Kaushal; Singh, Harinder P.; Baug, Tapas; Ngeow, Chow-Choong; Ou, Jia-Yu (2019). "Multiwavelength Period-Luminosity and Period-Luminosity-Color Relations at Maximum Light for Mira Variables in the Magellanic Clouds". The Astrophysical Journal. 884 (1): 20. arXiv:1908.01795. Bibcode:2019ApJ...884...20B. doi:10.3847/1538-4357/ab38c2. S2CID 199452754.
  3. ^ a b c d e f g h i j k Levesque, E. M.; Massey, P.; Plez, B.; Olsen, K. A. G. (2009). "The Physical Properties of the Red Supergiant WOH G64: The Largest Star Known?". The Astronomical Journal. 137 (6): 4744. arXiv:0903.2260. Bibcode:2009AJ....137.4744L. doi:10.1088/0004-6256/137/6/4744. S2CID 18074349.
  4. ^ Cite error: The named reference vanloon was invoked but never defined (see the help page).
  5. ^ Cite error: The named reference elias was invoked but never defined (see the help page).
  6. ^ a b c Cite error: The named reference 2mass was invoked but never defined (see the help page).
  7. ^ Cite error: The named reference macho was invoked but never defined (see the help page).
  8. ^ a b Cite error: The named reference ogle was invoked but never defined (see the help page).
  9. ^ Levesque, E. M. (June 2010). The Physical Properties of Red Supergiants. Hot and Cool: Bridging Gaps in Massive Star Evolution ASP Conference Series. Vol. 425. p. 103. arXiv:0911.4720. Bibcode:2010ASPC..425..103L. S2CID 8921166.
  10. ^ Beasor, Emma R.; Smith, Nathan (2022-05-01). "The Extreme Scarcity of Dust-enshrouded Red Supergiants: Consequences for Producing Stripped Stars via Winds". The Astrophysical Journal. 933 (1): 41. arXiv:2205.02207. Bibcode:2022ApJ...933...41B. doi:10.3847/1538-4357/ac6dcf. S2CID 248512934.
  11. ^ Groenewegen, Martin A. T.; Sloan, Greg C. (2018). "Luminosities and mass-loss rates of Local Group AGB stars and Red Supergiants". Astronomy & Astrophysics. 609: A114. arXiv:1711.07803. Bibcode:2018A&A...609A.114G. doi:10.1051/0004-6361/201731089. ISSN 0004-6361. S2CID 59327105.
  12. ^ Davies, Ben; Crowther, Paul A.; Beasor, Emma R. (2018). "The luminosities of cool supergiants in the Magellanic Clouds, and the Humphreys–Davidson limit revisited". Monthly Notices of the Royal Astronomical Society. 478 (3): 3138–3148. arXiv:1804.06417. Bibcode:2018MNRAS.478.3138D. doi:10.1093/mnras/sty1302. S2CID 59459492.
  13. ^ Jones, Olivia; Woods, Paul; Kemper, Franziska; Kraemer, Elena; Sloan, G.; Srinivasan, Sivakrishnan; Oliveira, Joana; van Loon, Jacco; Boyer, Martha; Sargent, Benjamin; Mc Donald, I.; Meixner, Margaret; Zijlstra, A.; Ruffel, Paul; Lagadec, Eric; Pauly, Tyler (May 7, 2017). "The SAGE-Spec Spitzer Legacy program: the life-cycle of dust and gas in the Large Magellanic Cloud. Point source classification – III". Monthly Notices of the Royal Astronomical Society. 470 (3): 3250–3282. arXiv:1705.02709. doi:10.1093/mnras/stx1101. Retrieved 23 June 2022.
  14. ^ Ohnaka, K.; Driebe, T.; Hofmann, K. H.; Weigelt, G.; Wittkowski, M. (2009). "Resolving the dusty torus and the mystery surrounding LMC red supergiant WOH G64". Proceedings of the International Astronomical Union. 4: 454–458. Bibcode:2009IAUS..256..454O. doi:10.1017/S1743921308028858.