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It's because a gas cloud has to have a critical mass in order to generate enough temperature to start the nuclear processes that enable the star to radiate heat and light.
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Is juveline star a low mass star or a high mass star?
It may be either. Juvenile means young.
Depending on its mass a star may live from about?
Depending on the mass a star may live 10million to 200billion years!
What is the life expectancy of the cool red dwarf star?
It depends. The lower the mass of the star, the longer the lifespan. It is believed that the lifespan of these stars exceeds the expected 10 billion year lifespan of our Sun by the third or fourth power of the ratio of their masses to the solar mass, which means a red dwarf with 0.1 solar mass may continue burning for 10 trillion years
What is a low-mass star?
A low mass star will burn very slowly for a very long time, maybe hundreds of billions of years at a cool red temperature. It will eventually run out of fuel, nuclear fusion will cease and it will contract to become a hotter White dwarf star, which will eventually become a black dwarf star as it cools.
Is a characteristic of a white dwarf star?
The end state of a star, whether it will explode as a supernova and become a black hole (or neutron star), or if the star simply becomes a white dwarf without undergoing any kind of explosive transformation is determined by its mass. To form a supernova in this way the original star needs to be about 8 times as massive as the Sun.But you should also recognise that white dwarf stars can also become supernova if they orbit another star in a binary system and steal material from their companion. Such a mass stealing white dwarf may undergo several 'nova' explosions as hydrogen fusion starts on their surfaces and, if they accumulate enough mass (above the Chandrasekhar limit of about 1.38 solar masses), they explode as supernovae.
What is the connection between chondro shekhor limit and black hole?
The Chandrasekhar limit describes the maximum stable mass of a highly compressed type of star called a white dwarf - a collapsed remnant of a star towards the end of its life cycle. This mass limit is about 1.44 times the mass of the sun; above this mass, gravitational force is calculated to overcome the outward pressure and thus precipitate further collapse, for example, into a neutron star. If the neutron star is of sufficient mass it may yet again collapse further, into more exotic states including possibly a black hole. Note that the mass limit of a neutron star (the Tollman-Oppenheimer-Volkoff limit) of around 3-4 solar masses is separate and distinct from the Chandrasekhar limit - you might say that the Chandrasekhar limit is just one of the mass limits along the stellar remnant's evolution into a black hole.
Can only giant stars become black holes?
The basic requisite is that enough mass gets together. This can happen with a large star if, after it explodes as a supernova, enough residual mass remains to go beyond the limit of a white dwarf, and of a neutron star. Yet there is also another possibility: a star may end up first as a white dwarf or as a neutron star, but it may eventually receive enough infalling matter to become a black hole.The basic requisite is that enough mass gets together. This can happen with a large star if, after it explodes as a supernova, enough residual mass remains to go beyond the limit of a white dwarf, and of a neutron star. Yet there is also another possibility: a star may end up first as a white dwarf or as a neutron star, but it may eventually receive enough infalling matter to become a black hole.The basic requisite is that enough mass gets together. This can happen with a large star if, after it explodes as a supernova, enough residual mass remains to go beyond the limit of a white dwarf, and of a neutron star. Yet there is also another possibility: a star may end up first as a white dwarf or as a neutron star, but it may eventually receive enough infalling matter to become a black hole.The basic requisite is that enough mass gets together. This can happen with a large star if, after it explodes as a supernova, enough residual mass remains to go beyond the limit of a white dwarf, and of a neutron star. Yet there is also another possibility: a star may end up first as a white dwarf or as a neutron star, but it may eventually receive enough infalling matter to become a black hole.
Is juveline star a low mass star or a high mass star?
It may be either. Juvenile means young.
Depending on its mass a star may live from about?
Depending on the mass a star may live 10million to 200billion years!
What is the life expectancy of the cool red dwarf star?
It depends. The lower the mass of the star, the longer the lifespan. It is believed that the lifespan of these stars exceeds the expected 10 billion year lifespan of our Sun by the third or fourth power of the ratio of their masses to the solar mass, which means a red dwarf with 0.1 solar mass may continue burning for 10 trillion years
What is Chandrasekhar's Limit?
The Chandrasekhar Limit, also called the Chandrasekhar mass, is the point beyond which the "electron degeneracy pressure" within a white dwarf star no longer balances the star's own gravity. It places an upper limit on the possible mass of a white dwarf. If a white dwarf's gravity pulls material away from a neighboring star, adding it to the white dwarf and increasing its mass, the Chandrasekhar mass (roughly 1.4 times the mass of our Sun) can eventually be reached and surpassed. When the balance between electron degeneracy pressure and gravity ends, the force of gravity rapidly collapses the white dwarf, and the resulting pressure and density result in a violent outward explosion that destroys the white dwarf. In Astronomy, this is known as a type Ia supernova. There have been a small number of type Ia supernovae (supernova "2007if" was the second known) which were believed to occur at masses significantly above the Chandrasekhar limit. The prevailing theory is that in these cases, two white dwarves collided, resulting in the limit being abruptly exceeded.
What is a low-mass star?
A low mass star will burn very slowly for a very long time, maybe hundreds of billions of years at a cool red temperature. It will eventually run out of fuel, nuclear fusion will cease and it will contract to become a hotter White dwarf star, which will eventually become a black dwarf star as it cools.
What a star may become after a supernova explosion?
Usually a neutron star, or a black hole, depending on the remaining mass.
What is the life cycle of high mass?
A high-mass star will use up its fuel faster than a low-mass one. Depending on the amount of mass that remains at the end of its life, it may convert to a neutron star, or to a black hole.
Can a neutron star die If so how What happens?
A neutron star may be considered "already dead"; it has stopped producing energy. A neutron star will gradually get dimmer, as it cools down. If it gathers enough mass from its surroundings, it may turn into a black hole.A neutron star may be considered "already dead"; it has stopped producing energy. A neutron star will gradually get dimmer, as it cools down. If it gathers enough mass from its surroundings, it may turn into a black hole.A neutron star may be considered "already dead"; it has stopped producing energy. A neutron star will gradually get dimmer, as it cools down. If it gathers enough mass from its surroundings, it may turn into a black hole.A neutron star may be considered "already dead"; it has stopped producing energy. A neutron star will gradually get dimmer, as it cools down. If it gathers enough mass from its surroundings, it may turn into a black hole.
How do stars more massive than four solar masses evolve into neutron stars?
I've seen that figure of 4 times the Sun's mass, but the usual number given is at least 8 times the Sun's mass. Anyway here's the answer: The general idea is that, depending on how much mass is left once the star runs out of fuel, it may become a white dwarf, a neutron star, or a black hole. A star like the Sun goes through a "red giant" star stage then becomes white dwarf star. Stars that are much more massive than the Sun go through a "supergiant" stage. They finally run out of fuel. The core of the star is now mainly iron. If, after running out of fuel, the amount of mass left in the core is more than a certain limit - the Chandrasekhar limit, currently believed to be about 1.39 times the mass of the Sun - the core's "electron degeneracy" pressure is not enough to resist the gravitational force on the core. In this case, the core of the star collapses into a neutron star or black hole and causes a supernova explosion.
Can a star with very small mass be formed?
Basically, if there is too little mass, the object won't have enough pressure and temperature to start nuclear fusion, so it won't qualify as a star. The limit seems to be about 8% of the Sun's mass - below that, there won't be the "normal" fusion, of hydrogen-1 to helium-4. However, there may still be some fusion, using deuterium (which is easier to fuse than normal hydrogen). Such objects - below about 8% of the Sun's mass - are called brown dwarves.
