how do neutron stars, pulsars, and black holes evolve differently than average stars?

Answer 1

It's all about the mass baby! (sorry, had to say that!)

Ordinary stars such as our sun tend to wind up as white dwarf stars. This is because they fall under the Chandrasekgar limit of 1.4 solar masses or so. As long as the final mass of the star falls within this limit, it is a white dwarf. The more massive the star, the different the composition of the dwarf. Our sun for example will become a simple carbon-oxygen dwarf, while Betelgeuse will become a neon-oxygen dwarf. Red dwarfs become helium dwarfs.

If the final mass of the star is more massive than the 1.4 limit, things will get more explosive. If more mass falls on a white dwarf (due to mass transfers in binaries) a Type Ia supernova results from carbon detonation.

If the star is yet more massive (at least 8 times more massive than the sun while still in the main sequence phase) it cannot lose enough mass to become a white dwarf, and will become either a neutron star or black hole. Scientists are still not certain of the final outcomes of these stars, as the process of stellar evolution is poorly understood.

Note...Pulsars are rapidly spinning neutron stars. Once they stop spinning (and generating the light "pulse" in the process) they become plain neutron stars.

Answer 2

For stars of below 4 image voltaic lots, hydrogen burn-up on the middle triggers strengthen to the pink vast area. From observations of diverse different stars which seem reminiscent of our solar, it really is envisioned that the solar will eventually flow upward and to the right of its present day position on the major sequence and enter a pink vast area. the most suitable degree of our solar is envisioned to be as a white dwarf. a million teaspoon of a white dwarf ought to weigh 5 much. A white dwarf with image voltaic mass should be about the length of the Earth. For a sufficiently tremendous celeb, an iron center is formed and nonetheless the gravitational crumple has sufficient ability to warmth it as a lot as a extreme sufficient temperature to both fuse or fission iron. both in the aftermath of a supernova or in only a collapsing tremendous celeb, the flexibility receives extreme sufficient to break down the iron into alpha debris and different smaller instruments, and nonetheless the rigidity maintains to construct. even as it reaches the verge of crumple of ability mandatory to rigidity the combining of electrons and protons to variety neutrons, the electron degeneracy decrease has been surpassed and the crumple maintains till it really is stopped with assistance from neutron degeneracy. At this aspect apparently that the crumple will end for stars with mass below 2 or 3 image voltaic lots, and the resultant number of neutrons is termed a neutron celeb. The periodic emitters called pulsars are considered neutron stars. If the mass exceeds about 3 image voltaic lots, then even neutron degeneracy gained't end the crumple, and the middle shrinks in the route of the black hollow situation. This neutron degeneracy RADIUS is about 20 km for a image voltaic mass, compared to about EARTH length for a image voltaic mass white dwarf. The density is quoted as about one billion much in step with teaspoonful compared to 5 much in step with teaspoonful for the white dwarf.

Answer 3

Hi. All are the result of a supernova.