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A stellar black hole (or stellar-mass black hole) is a black hole formed by the gravitational collapse of a star. [1] They have masses ranging from about 5 to several tens of solar masses. [2] They are the remnants of supernova explosions, which may be observed as a type of gamma ray burst. These black holes are also referred to as collapsars.
For most stars, this will result in the formation of a very dense and compact stellar remnant, also known as a compact star. Compact objects have no internal energy production, but will—with the exception of black holes—usually radiate for millions of years with excess heat left from the collapse itself. [3]
A stellar black hole of 1 M ☉ has a Hawking temperature of 62 nanokelvins. [142] This is far less than the 2.7 K temperature of the cosmic microwave background radiation. Stellar-mass or larger black holes receive more mass from the cosmic microwave background than they emit through Hawking radiation and thus will grow instead of shrinking. [143]
OJ 287 core black holes — a BL Lac object with a candidate binary supermassive black hole core system [23] PG 1302-102 – the first binary-cored quasar — a pair of supermassive black holes at the core of this quasar [24] [25] SDSS J120136.02+300305.5 core black holes — a pair of supermassive black holes at the centre of this galaxy [26]
Stellar black holes observed across the Milky Way galaxy are about 10 times as massive as the sun on average. Until the discovery of Gaia BH3, the largest known stellar black hole in our galaxy ...
Stellar black holes have much greater average densities than supermassive black holes. If one accumulates matter at nuclear density (the density of the nucleus of an atom, about 10 18 kg/m 3; neutron stars also reach this density), such an accumulation would fall within its own Schwarzschild radius at about 3 M ☉ and thus would be a stellar ...
The average mass of known black holes of stellar origin in our galaxy is around 10 times the mass of our Sun. Until now, the weight record was held by a black hole in an X-ray binary in the Cygnus ...
The first [1] is given by = where M BH is the mass of the black hole, σ is the stellar velocity dispersion of the host bulge, and G is the gravitational constant. The second definition [ 2 ] is the radius at which the enclosed mass in stars equals twice M BH , i.e. M ⋆ ( r < r h ) = 2 M BH . {\displaystyle M_{\star }(r<r_{h})=2M_{\text{BH}}.}