it builds up a core of inert helium.
not very long because its about to supernova,,,,,,,,, i think again
Objects above this mass fuse hydrogen too rapidly and cannot stay together.
No. A star's class on the main sequence is ultimately predetermined by its mass, so a star cannot change its position on the main sequence. Epsilon Eridani is about 82% the mass of the sun, which limits it to a lower rate of fusion and thus a lower temperature and luminosity than a G-type star like the sun. Epsilon Eridani's only change in class will come when it leaves the main sequence to become a red giant.
In some binary systems, the less-massive star has become a giant, while the more-massive star is still on the main sequence. If higher-mass stars evolve faster than lower-mass stars, how do the lower-mass stars in such binaries manage to leave the main sequence first? This is called the Algol paradox, after the binary system Algol.
The greater the mass, the greater the brightness.
Main sequence.
Polaris - the current North star is a multiple star system., consisting of the main star and smaller companions. The main star Alpha Ursae Minoris is a bright star, a 6 solar mass supergiant and it is a main sequence star. Orbiting very close to this main star is a white dwarf of roughly 1.5 solar masses. This is not a main sequence star. Orbiting further out is the third companion, a 1.39 solar mass star. This is a main sequence star. There are also two more distant components (α UMi C and α UMi D) - Polaris is thought to be part of an open cluster - I do not know if these later two stars are main sequence or not.
not very long because its about to supernova,,,,,,,,, i think again
Sirius consists of two stars.Sirius A is a main-sequence star with about two solar masses.Sirius B is a white dwarf with about one solar mass. During its main-sequence, it's estimated to have been around five solar masses.
Objects above this mass fuse hydrogen too rapidly and cannot stay together.
No. A star's class on the main sequence is ultimately predetermined by its mass, so a star cannot change its position on the main sequence. Epsilon Eridani is about 82% the mass of the sun, which limits it to a lower rate of fusion and thus a lower temperature and luminosity than a G-type star like the sun. Epsilon Eridani's only change in class will come when it leaves the main sequence to become a red giant.
In some binary systems, the less-massive star has become a giant, while the more-massive star is still on the main sequence. If higher-mass stars evolve faster than lower-mass stars, how do the lower-mass stars in such binaries manage to leave the main sequence first? This is called the Algol paradox, after the binary system Algol.
The greater the mass, the greater the brightness.
A 16.0 solar mass star would spend about 11.7 million years on the main sequence (depending on the metallicity). After approximately 13.0 million years it would become a 1.5 solar mass (approx.) neutron star. This was calculated using metallicity z=0.02 (solar)
A star that was 150 solar masses would spend the main part of its life as a main sequence star before collapsing into a white dwarf. A stars mass determines the life expectancy as well as its probable cause of death.
Main Sequence Stars
The Sun is a medium mass star in main sequence.