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Three prominent Wolf-Rayet stars have been detected within the cluster.
Wolf-Rayet stars are extremely hot stars that have lost much or all of their outer layers.
At that time its spectrum was that of a Wolf-Rayet star.
He also made an important contribution in analyzing spectra of Wolf-Rayet stars.
There are no other naked eye Wolf-Rayet stars.
The evolutionary status of the Wolf-Rayet stars suggests that they all formed in a relatively short timespan.
He discovered Wolf-Rayet stars together with Charles Wolf in 1867.
It may be a Wolf-Rayet star.
Her work has had a strong influence in the areas of massive stars and close binaries, especially Wolf-Rayet stars.
In some cases, after becoming supergiants, they can evolve into Wolf-Rayet stars or luminous blue variables.
More than 100 OB and Wolf-Rayet stars have been identified there so far.
The most massive stars can become Wolf-Rayet stars without becoming giants or supergiants at all.
Additionally, there are several confirmed Wolf-Rayet stars.
These stars usually become blue supergiants, although it is possible that some of them evolve directly to Wolf-Rayet stars.
Some Wolf-Rayet stars are surrounded by pinwheel nebulae.
Low-mass stars explode as supernovae before they lose enough mass to become Wolf-Rayet stars.
R136b is a Wolf-Rayet star in the Large Magellanic Cloud.
The nature of the emission bands in the spectra of a Wolf-Rayet star remained a mystery for several decades.
WR 102ea is a Wolf-Rayet star in the Sagittarius constellation.
In 1867 he and Georges Rayet discovered Wolf-Rayet stars.
It is possible for a Wolf-Rayet star to progress to a "collapsar" stage in its death throes if it doesn't lose sufficient mass.
The star is actually quintuple, and the primary component is famous for being the brightest Wolf-Rayet star in the sky.
Rapid mass loss can occur in the case a Wolf-Rayet star, and these massive objects show a spectrum that is lacking in hydrogen.
Wolf-Rayet stars were co-discovered by French astronomer Charles Wolf and not by him.
Observationally, this late thermal pulse phase appears almost identical to a Wolf-Rayet star in the midst of its own planetary nebula.
However, one group of WR stars do show significant hydrogen.
In contrast to the other WR stars, these are not highly evolved stars that have exhausted hydrogen in their cores.
High mass WR stars are young stars only just evolving away from the main sequence, rather than very old stars that have lost all their hydrogen.
There is however one group of WR stars that have strong hydrogen lines in their spectra indicating the existence of a hydrogen atmosphere.
Wolf-Rayet stars (WR stars) are evolved, massive stars (over 20 solar masses initially).
WR stars are not thought to form in low metallicity stars because they do not lose enough mass, instead proceeding directly to pair-instability or photodisintegration supernovae.
The majority of WR stars are now understood as being at a natural state in the evolution of massive stars (not counting the less common planetary nebula central stars).
WNh stars are both initially more massive and have lost relatively little mass compared to other WR stars, hence they are amongst the most luminous stars known.
Wolf-Rayet stars (often referred to as WR stars) are evolved, massive stars (over 20 solar masses initially) which are losing mass rapidly by means of a very strong stellar wind, with speeds up to 2000 km/s.
About 30% of known galactic Wolf-Rayet stars, are located in dense clusters of O stars with intense ultraviolet radiation fields, and the collapsar model suggests that WR stars are likely GRB progenitors.
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