R136a2
The central region of the R136 star cluster as seen in near infrared. R136a1 and R136a2 are the two very close bright stars at the center, with R136a2 being the fainter of the two. Credit: ESO | |
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Dorado |
Right ascension | 05h 38m 42.40s[1] |
Declination | −69° 06′ 02.88″[1] |
Apparent magnitude (V) | 12.34[1] |
Characteristics | |
Evolutionary stage | Wolf-Rayet star
|
Spectral type | WN5h[2] |
B−V color index | 0.23[1] |
Absolute magnitude (MV) | -7.80[4] |
Absolute bolometric magnitude (Mbol) | -12.0[5] |
Details Myr | |
BAT99 109, CHH92 2 | |
Database references | |
SIMBAD | data |
R136a2 (RMC 136a2) is a
Discovery
In 1960, a group of astronomers working at the Radcliffe Observatory in Pretoria made systematic measurements of the brightness and spectra of bright stars in the Large Magellanic Cloud. Among the objects cataloged was RMC 136, (Radcliffe Observatory Magellanic Cloud Catalogue, Catalog number 136) the central "star" of 30 Doradus. Subsequent observations showed that R136 was located in the center of a giant H II region that was a center of intense star formation in the immediate vicinity of the observed stars.[8]
In the early 1980s,
Distance
Determining a precise distance to R136a2 is challenging due to many factors. At the immense distance to the LMC, the parallax method is beyond the limits of current technology. Most estimates assume that R136 is at the same distance as the Large Magellanic Cloud. The most accurate distance to the LMC is 49.97 kpc, derived from a comparison of the angular and linear dimensions of
Properties
Like all Wolf-Rayet stars, R136a2 is undergoing severe mass loss by a fast stellar wind. The star loses 4.6×10−5 solar masses per year through a stellar wind with a speed of 2,400 km/s.[5][12] The high mass of the star compresses and heats the core and promotes rapid hydrogen fusion predominantly through the CNO process, leading to a luminosity of 5,129,000 L☉. The fusion rate is so great that in 10 seconds R136a2 produces more energy than the Sun does in a year. It may have been a 221 M☉ star at the time it was born and lost as much as 24 M☉ in the past 1 to 2 million years,[4] but since current theories suggest that no stars can be born above 150 M☉ it may be a merger of two or more stars.[13]
Although the star is one of the
Fate
It is thought that stars this massive can never lose enough mass to avoid a catastrophic end with the collapse of a large iron core. The result will be a