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R136a1 is expected to lose almost all its spin long before core collapse so a GRB is unlikely. [37] The remnant from a type Ic core collapse supernova is either a neutron star or black hole, depending on the mass of the progenitor core. For a star as massive as R136a1, the remnant will very likely be a black hole instead of a neutron star. [38]
UY Scuti (BD-12°5055) is a red supergiant star, located 5,900 light-years away in the constellation Scutum. It is also a pulsating variable star , with a maximum brightness of magnitude 8.29 and a minimum of magnitude 10.56, which is too dim for naked-eye visibility.
The Sun, the orbit of Earth, Jupiter, and Neptune, compared to four stars (Pistol Star, Rho Cassiopeiae, Betelgeuse, and VY Canis Majoris) Overview Although red supergiants are often considered the largest stars, some other star types have been found to temporarily increase significantly in radius, such as during LBV eruptions or luminous red ...
The central R136 concentration of the cluster is about 2 parsecs across, although the whole NGC 2070 cluster is much larger. [8] R136 is thought to be less than 2 million years old. [8] [9] None of the member stars are significantly evolved, and none are thought to have exploded as supernova. Because of this, the cluster contains no red ...
If this object were 10 parsecs away from Earth it would appear nearly as bright in the sky as the Sun (apparent magnitude −26.744). This quasar's luminosity is, therefore, about 2 trillion (10 12) times that of the Sun, or about 100 times that of the total light of average large galaxies like our Milky Way. (Note that quasars often vary ...
Beta Scuti is the second brightest at magnitude 4.22, followed by Delta Scuti at magnitude 4.72. It is also known as 6 Aquilae. [7] Beta Scuti is a binary system, [8] [9] with the primary with a spectral type similar to the Sun, although it is 1,270 times brighter. Delta Scuti is a bluish white giant star, which is now coming at the direction ...
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.
The mass is equally uncertain, thought to have been up to 200 times the Sun when initially formed but now considerably less due to extreme mass loss although likely still over 100 times the Sun. [10] Modelling the star itself to match its spectrum gives a mass of 27.5 M ☉, [7] while matching its current properties to an evolutionary model ...