NEUTRON STARS AND BLACK HOLES form from the stellar cores that remain after
stars have exploded as
Supernovae(explained in the previous blog Part-9). If the remaining core is between
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| Neutron Star |
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| Black Hole |
about one and half and three solar masses, it contracts to form a Neutron star. If the remaining core is greater than about three solar masses(mass of the Sun-1.989 × 1030 kg) it contracts to form a Black hole. Neutron stars are typically only about 10 Kilometers in diameter and consist almost entirely of subatomic particles called Neutrons. Such stars are so dense that a teaspoonful would weigh about a billion tonnes.Neutron stars are observed as Pulsars, so-called because they rotate rapidly and emit two beams of radio waves, which sweep across the sky and are detected as short pulses. Black holes
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| Colliding Neutron Stars |
are characterized by their extremely strong gravity,
which is so powerful that not even light can escape; as a result, black holes are invisible. However, they can be detected if they have a close companion star. The gravity of the black hole pulls gas from the other star, forming an accretion disc that spiral s around the black hole at high speed, heating up and emitting radiation. Eventually, the matter spirals in to cross the
Event Horizon (the boundary of black hole), thereby disappearing from the visible
Universe.
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| Stellar Black Hole |
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| Pulsar(Rotating Neutron Star) |
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