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BAT99-98
Observation data; Epoch J2000 Equinox J2000
Constellation	Dorado
Right ascension	05h 38m 39.144s
Declination	−69° 06′ 21.30″
Apparent magnitude (V)	13.38
Characteristics
Evolutionary stage	Wolf–Rayet star
Spectral type	WN6
B−V color index	-0.10
Astrometry
Proper motion (μ)	RA: 1.680 mas/yr ; Dec.: 0.512 mas/yr
Parallax (π)	0.0288 ± 0.0159 mas
Distance	165,000 ly ; (50,600 pc)
Absolute magnitude (MV)	-8.11
Absolute bolometric; magnitude (Mbol)	-12.0
Details
Mass	226 (highly uncertain) M☉
Radius	37.5 R☉
Luminosity	5,000,000 L☉
Luminosity (visual, LV)	141,000 L☉
Temperature	45,000 K
Age	7.5 Myr
Other designations
	Brey 79, NGC 2070 MEL J, SSTISAGEMC J053839.14-690621.2, BAT99 98, LMC AB12, Melnick 49, 2MASS J05383914-6906211, UCAC4 105‑014273, Gaia EDR3 4657679654981424640
Database references
SIMBAD	data

BAT99-98 is a Wolf–Rayet star located in the Large Magellanic Cloud, in NGC 2070 near the R136 cluster in the Tarantula Nebula (30 Doradus). At 226 M_☉ and 5,000,000 L_☉ it is the most massive known star, and close to one of the most luminous stars currently known.^[3]

Observations

A 1978 survey carried out by Jorge Melnick covered the 30 Doradus region and found six new Wolf–Rayet (WR) stars, all belonging to the WN sequence. The survey observed stars that were above^{[clarification needed]} apparent magnitude 14 and within 2 arcminutes of the centre of the 30 Doradus nebula, and the star now known as BAT99‑98 was labelled as star J. It was found to have a magnitude of 13.5 and a spectral type of WN5.^[5]

The following year, thirteen new WR stars in the Large Magellanic Cloud were reported, one of which was Mel J. It was numbered 12, and referred to as AB12, or LMC AB12 to distinguish it from the better-known AB stars in the Small Magellanic Cloud.^[6]

Melnick conducted another study of stars in NGC 2070 and gave BAT99-98 the number 49, reclassifying its spectral type as WN7.^[7]

Neither the AB12 nor the Mel J designation is in common use, although "Melnick 49" is sometimes seen. More commonly, LMC Wolf–Rayet stars are referred to by R (Radcliffe Observatory) numbers, Brey (Breysacher catalogue numbers^[8]), or BAT99 numbers.^[9]

Characteristics

BAT99‑98 is located near the R136 cluster and has similar mass–luminosity properties to the massive stars in the cluster itself. It is estimated that the star held 250 M_☉ at its birth and has since lost 20 M_☉.^[3] It sheds a large amount of mass through a stellar wind that moves at 1,600 km/s.^[3] The star has a surface temperature of 45,000 K and a luminosity of 5,000,000 L_☉. Although the star is very luminous due to its high temperature, much of that light is ultraviolet and invisible to humans – making it 141,000 times brighter than the Sun visually. It is now classified as a WN6 star, and models suggest that it is 7.5 million years old.

Fate

The future of BAT99-98 depends on its mass loss. It is thought that stars this massive can never lose enough mass to avoid a catastrophic end. The result is likely to be a supernova, hypernova, gamma-ray burst, or perhaps almost no visible explosion, leaving behind a black hole or neutron star. The exact details depend heavily on the timing and amount of the mass loss, with current models not fully reproducing observed stars, but the majority of massive stars in the Local Group are expected to produce Type Ib or Ic supernovae, sometimes with a gamma-ray burst, and leave behind a black hole.^[10] However, for some stars of exceptionally high mass, the supernova event is triggered by pair instability and leaves behind no remnant at all.^[11]

References

^ ^a ^b ^c ^d ^e Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
^ ^a ^b Doran, E. I.; Crowther, P. A.; de Koter, A.; Evans, C. J.; McEvoy, C.; Walborn, N. R.; Bastian, N.; Bestenlehner, J. M.; Grafener, G.; Herrero, A.; Kohler, K.; Maiz Apellaniz, J.; Najarro, F.; Puls, J.; Sana, H.; Schneider, F. R. N.; Taylor, W. D.; van Loon, J. Th.; Vink, J. S. (2013). "The VLT-FLAMES Tarantula Survey – XI. A census of the hot luminous stars and their feedback in 30 Doradus". Astronomy & Astrophysics. 558: A134. arXiv:1308.3412v1. Bibcode:2013A&A...558A.134D. doi:10.1051/0004-6361/201321824. S2CID 118510909.
^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j ^k Hainich, R.; Rühling, U.; Todt, H.; Oskinova, L. M.; Liermann, A.; Gräfener, G.; Foellmi, C.; Schnurr, O.; Hamann, W. -R. (2014). "The Wolf–Rayet stars in the Large Magellanic Cloud". Astronomy & Astrophysics. 565: A27. arXiv:1401.5474. Bibcode:2014A&A...565A..27H. doi:10.1051/0004-6361/201322696. S2CID 55123954.
^ Selman, F. J.; Melnick, J. (2005). "The IMF of the field population of 30 Doradus". Astronomy and Astrophysics. 443 (3): 851. Bibcode:2005A&A...443..851S. doi:10.1051/0004-6361:20042173. S2CID 120118444.
^ Melnick, J. (1978). "More Wolf–Rayet stars in 30 Doradus". Astronomy and Astrophysics Supplement Series. 34: 383–385. Bibcode:1978A&AS...34..383M.
^ Azzopardi, M.; Breysacher, J. (1979). "New Wolf–Rayet stars in the Large Magellanic Cloud". Astronomy and Astrophysics. 75: 243. Bibcode:1979A&A....75..243A.
^ Melnick, J. (1985). "The 30 Doradus nebula. I – Spectral classification of 69 stars in the central cluster". Astronomy and Astrophysics. 153: 235. Bibcode:1985A&A...153..235M.
^ Breysacher, J. (1981). "Spectral Classification of Wolf–Rayet Stars in the Large Magellanic Cloud". Astronomy and Astrophysics Supplement. 43: 203. Bibcode:1981A&AS...43..203B.
^ Breysacher, J.; Azzopardi, M.; Testor, G. (1999). "The fourth catalogue of Population I Wolf–Rayet stars in the Large Magellanic Cloud". Astronomy and Astrophysics Supplement Series. 137 (1): 117–145. Bibcode:1999A&AS..137..117B. doi:10.1051/aas:1999240.
^ Woosley, S. E.; Heger, A. (2015). "The Deaths of Very Massive Stars". Very Massive Stars in the Local Universe. Astrophysics and Space Science Library. Vol. 412. pp. 199–225. arXiv:1406.5657. Bibcode:2015ASSL..412..199W. doi:10.1007/978-3-319-09596-7_7. ISBN 978-3-319-09595-0. S2CID 119238749.
^ "Lecture 18: Pair Instability Supernovae" (PDF). Archived (PDF) from the original on 2021-12-04.