IRAS 05280–6910

In this article, we are going to explore in detail IRAS 05280–6910 and its impact on our society. IRAS 05280–6910 is a widely discussed topic that has generated controversy in different areas. Over the years, IRAS 05280–6910 has played a crucial role in people's lives, influencing culture, politics, economics, and many other areas. Through this comprehensive analysis, we hope to provide a clearer view of IRAS 05280–6910 and its importance in the modern world.

IRAS 05280–6910

The supergiant IRAS 05280–6910 in the open cluster NGC 1984. It is the bright reddened object near the centre
Credit: Université de Strasbourg/CNRS
Observation data
Epoch J2000      Equinox J2000
Constellation Dorado (LMC)
Right ascension 05h 28m 00.28s[1]
Declination −69° 10′ 26.0″[1]
Characteristics
Apparent magnitude (J) 14.45[2]
Apparent magnitude (K) 12.87[2]
Details
Radius1,367[3] - 1,736[4][a] R☉
Luminosity220,000[4] - 225,000[3] L☉
Temperature3,000[4] - 3,400[3] K
Other designations
IRAS 05280–6910, MSX LMC 582, OH 279.6-32.6, LI-LMC 1100, NGC 1984 IR 1
Database references
SIMBADdata

IRAS 05280–6910 is a red supergiant star or OH/IR supergiant star[5] located in the Large Magellanic Cloud. IRAS 05280−6910 was found towards the cluster NGC 1984. It is more than 1,300 times larger than of the Sun, making it one of the largest stars discovered so far. If placed at the center of the Solar System, its photosphere would engulf the orbit of Jupiter. It has an estimated mass loss rate of 5.4×10−4 M☉ per year, one of the highest known for any red supergiant star.[3]

Characteristics

IRAS 05280–6910 is likely an OH supergiant star. It is the most reddened object in the LMC, It also shows the distinct type of maser signal similar to that of VY Canis Majoris.[6] Its exact radius is uncertain. According to one paper, it is 1,367 times the size of the Sun,[3] while another says that it is 1,736 times the size of the Sun. In either case, it is among the largest stars known.[4]

IRAS 05280–6910 likely had a mass of 20 to 25 solar masses when it formed.[6]

Notes

  1. ^ The radius of IRAS 05280-6910 can be calculated using the Stefan–Boltzmann law and the solar effective temperature of 5,772 K:

References

  1. ^ a b Gruendl, R.A.; Chu, Y.-H. (2009). "High- and intermediate-mass young stellar objects in the Large Magellanic Cloud". The Astrophysical Journal Supplement. 184 (1): 172–197. arXiv:0908.0347. Bibcode:2009ApJS..184..172G. doi:10.1088/0067-0049/184/1/172.
  2. ^ a b Van Loon, J.T.; Marshall, J.R.; Zijlstra, A. A. (2005). "Dust-enshrouded giants in clusters in the Magellanic Clouds". Astronomy and Astrophysics. 442 (2): 597–613. arXiv:astro-ph/0507571. Bibcode:2005A&A...442..597V. doi:10.1051/0004-6361:20053528.
  3. ^ a b c d e Steven R. Goldman; Jacco Th. van Loon (2016). "The wind speeds, dust content, and mass-loss rates of evolved AGB and RSG stars at varying metallicity". Monthly Notices of the Royal Astronomical Society. 465 (1): 403–433. arXiv:1610.05761. Bibcode:2017MNRAS.465..403G. doi:10.1093/mnras/stw2708. S2CID 11352637.
  4. ^ a b c d Matsuura, Mikako; Sargent, B.; Swinyard, Bruce; Yates, Jeremy; Royer, P.; Barlow, M. J.; Boyer, Martha; Decin, L.; Khouri, Theo; Meixner, Margaret; Van Loon, Jacco Th., Woods, Paul M (2016). "The mass-loss rates of red supergiants at low metallicity: Detection of rotational CO emission from two red supergiants in the Large Magellanic Cloud". Monthly Notices of the Royal Astronomical Society. 462 (3): 2995–3005. arXiv:1608.01729. Bibcode:2016MNRAS.462.2995M. doi:10.1093/mnras/stw1853. S2CID 53059365.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  5. ^ Wood, P. R.; Whiteoak, J. B.; Hughes, S. M. G.; Bessell, M. S.; Gardner, F. F.; Hyland, A. R. (October 1992). "OH/IR Stars in the Magellanic Clouds". The Astrophysical Journal. 397: 552. Bibcode:1992ApJ...397..552W. doi:10.1086/171812. ISSN 0004-637X.
  6. ^ a b Beasor, Emma R.; Smith, Nathan (May 2022). "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.