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What kind of pressure supports a white dwarf?
electron degeneracy pressure
What is fermi pressure?
This is a guess, but I suspect the person means the electron degeneracy pressure.
How is degeneracy pressure related to white dwarfs and neutron stars?
White dwarfs are prevented from collapsing further by electron degeneracy pressure. If the mass of a stellar remnant exceeds the Chandrasekhar limit, about 1.4 solar masses, gravity will overcome this pressure and form a much smaller and denser neutron star. Further collapse in a neutron star is prevented by neutron degeneracy pressure up until the Tolman-Oppenheimer-Volkoff limit of about 3 solar masses, at which point gravity causes a complete collapse, forming a black hole.
What happens when the gravity of a massive star overcomes neutron degeneracy pressure?
The core contracts and becomes a black hole.
What prevents neutron stars from contracting to a smaller size?
Neutron degeneracy pressure, in which the neutrons themselves prevents further collapse.
Is this true or false brown dwarfs white dwarfs and neutron stars are all kept from collapsing by degeneracy pressure?
True.
How come all stars don't form into black holes?
A black hole forms only when the star is large enough that the gravitational pressure exceeds the quantum degeneracy pressure.
What prevents a white dwarf from completely collapsing upon itself?
Further collapse of a white dwarf is prevented by electron degeneracy pressure.
How does temperature differ from a thermal change?
Temperatures, as provided by thermometers, measure and quantify the extent of thermal changes.
How is thermal energy different from temperature How are they similar?
temperatures differ from thermal energy because differ because thermal energy is the total energy of all particles in an object and temperature is a measure of the average energy of random motion of particles of matter.
What keeps white dwarf from collapsing under its own weight?
A white dwarf star, as well as any other stable variety of star,is held together by the pressure popularly known as "gravity".In the opposite direction, white dwarf stars are kept from collapsing completely by degeneracy pressure. Specifically, for white dwarf stars, it's electron degeneracy pressure, which arises from the fact that electrons are fermions and cannot all occupy the same energy state. For higher mass stars, the force of gravity is able to overcome this and push all the electrons into the ground state, and the star is supported by a different kind of degeneracy ... neutron degeneracy, which is the same thing but with neutrons ... and you get a neutron star. At even higher masses, even that isn't sufficient and the star collapses all the way into a black hole.
How do neutron stars form?
When a medium-size star runs out of fuel (hydrogen to fuse into helium), it will collapse on itself. It has a large enough mass that it can push past the resistance from electron degeneracy pressure. When it collapses more, it will get stopped by neutron degeneracy pressure. It will settle at a star that is about 20 kilometers in diameter. The star fuses protons with electrons, and these form neutrons to make a kind of "neutron soup".
