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Well, I want you to know that it's okay to have questions about things we don't fully understand yet. Even though I may not have an answer for you right now, I want you to find joy in the journey of exploring and learning more about this phenomenon. Let's keep painting those happy little question marks and keep searching for the beauty of knowledge together.
What else can I help you with?
What kind of pressure supports a white dwarf?
A white dwarf is supported by electron degeneracy pressure, which is the repulsion between closely-packed electrons that prevents further gravitational collapse. This pressure is a result of the Pauli exclusion principle, which states that no two electrons can occupy the same quantum state.
Is white drawf bigger than a nertron star?
Simply, neutron star is a big nuclear - of 10km radius and solar mass (mass density about  1017- 1018 kg/m3). The material in a white dwarf is supported by electron degeneracy pressure. The physics of degeneracy yields a maximum mass for a non-rotating white dwarf, the Chandrasekhar limit-approximately 1.4 solar masses-beyond which it cannot be supported by electron degeneracy pressure. The density of white dwarf is - 109 kg/m3. So its radius is much bigger 10km, but the mass can be less, as well as bigger of solar mass.
What factors will cause the degeneracy pressure within an object to increase?
Oh, that's a fantastic question, my friend. When the electrons in an object get really close together, like in a tightly packed group at a party, they start to push against each other more and more, creating strong degeneracy pressure. This can happen when the object gets denser, like when you add more guests to that party, causing the pressure to increase and keep everything in balance.Nature truly is a wonderful thing, don't you think?
What prevents a white dwarf from completely collapsing upon itself?
Electron degeneracy pressure, a quantum mechanical effect, supports the white dwarf against gravitational collapse. According to the Pauli exclusion principle, no two electrons can occupy the same quantum state, leading to pressure that counteracts gravitational forces. This pressure prevents further collapse and maintains the equilibrium of a white dwarf.
What happens when the gravity of a massive star overcomes neutron degeneracy pressure?
When the gravity of a massive star overcomes neutron degeneracy pressure, the core collapses under its own gravity, leading to the formation of a black hole or a neutron star, depending on the initial mass of the star. This process releases a tremendous amount of energy in the form of a supernova explosion.
What kind of pressure supports a white dwarf?
A white dwarf is supported by electron degeneracy pressure, which is the repulsion between closely-packed electrons that prevents further gravitational collapse. This pressure is a result of the Pauli exclusion principle, which states that no two electrons can occupy the same quantum state.
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 is fermi pressure?
This is a guess, but I suspect the person means the electron degeneracy pressure.
How does degeneracy pressure differ from thermal pressure in terms of their effects on the stability and behavior of a stellar object?
Degeneracy pressure and thermal pressure are two forces that support stellar objects against gravitational collapse. Degeneracy pressure arises from the quantum mechanical properties of particles, while thermal pressure comes from the temperature of the object. Degeneracy pressure is independent of temperature and increases as the object's mass increases, leading to stability in massive stars. Thermal pressure, on the other hand, depends on temperature and tends to decrease as the object cools, potentially leading to instability. In summary, degeneracy pressure is more important for the stability of massive stars, while thermal pressure is more significant for lower-mass stars.
Is white drawf bigger than a nertron star?
Simply, neutron star is a big nuclear - of 10km radius and solar mass (mass density about  1017- 1018 kg/m3). The material in a white dwarf is supported by electron degeneracy pressure. The physics of degeneracy yields a maximum mass for a non-rotating white dwarf, the Chandrasekhar limit-approximately 1.4 solar masses-beyond which it cannot be supported by electron degeneracy pressure. The density of white dwarf is - 109 kg/m3. So its radius is much bigger 10km, but the mass can be less, as well as bigger of solar mass.
Is this true or false brown dwarfs white dwarfs and neutron stars are all kept from collapsing by degeneracy pressure?
True. Brown dwarfs, white dwarfs, and neutron stars are all supported against collapse by degeneracy pressure, which is a quantum mechanical effect that arises when particles are packed densely together and cannot occupy the same quantum state. This pressure prevents further gravitational collapse and supports the star against its own gravity.
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.
What factors will cause the degeneracy pressure within an object to increase?
Oh, that's a fantastic question, my friend. When the electrons in an object get really close together, like in a tightly packed group at a party, they start to push against each other more and more, creating strong degeneracy pressure. This can happen when the object gets denser, like when you add more guests to that party, causing the pressure to increase and keep everything in balance.Nature truly is a wonderful thing, don't you think?
What happens when the gravity of a massive star is ablle to overcome neutron degeneration?
When the gravity of a massive star overcomes neutron degeneracy pressure, it can result in the star collapsing further to form a black hole. This occurs when the mass of the star is above a certain threshold known as the Tolman–Oppenheimer–Volkoff limit, causing the neutron degeneracy pressure to be insufficient to support the star against gravity.
What prevents neutron stars from contracting to a smaller size?
Neutron degeneracy pressure, in which the neutrons themselves prevents further collapse.
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.
Is ower sun big enough to make a black hole?
No. The only mechanism by which black holes are known to form is the gravitational collapse of a star with a mass at least 20 times that of our Sun. All objects require some outward force to balance gravity. In main sequence stars, the outward flow of energy from the nuclear reactions in the core creates an outward pressure to balance gravity. Once the fuel is exhausted and the core collapses, there are two more forms of pressure which can halt collapse. First, electron degeneracy pressure, which can be thought of as a repulsion between electrons. Electron degeneracy pressure can support a body of up to approximately 1.4 times the mass of the Sun, and stars that end their life in this state are known as white dwarves. Second, neutron degeneracy pressure; repulsion between neutrons. We are less certain about the extent to which neutron degeneracy pressure can support a body against gravitational collapse, but we understand the limit to be somewhere around 2.5 times the mass of the Sun. Stars that end in this state become neutron stars. An object experiencing gravitational collapse which has a mass greater than can be supported by neutron degeneracy pressure will collapse into a black hole. Note, that it is not the entire star that collapses, merely the core. The outer envelope of the star is ejected as a planetary nebula in the case of lower mass stars, and in a supernova in the case of higher mass stars.
