NK
А как делать как Евгений?
Я в латексе от слова вообще не шарю
Я в латексе от слова вообще не шарю
Ухты, спасибо большое.
А можно конспектировать как @EvgeniyZh?
Size: a a a
2017 June 16
EZ
ID:200200555
можно)
EZ
ID:200200555
А как делать как Евгений?
Я в латексе от слова вообще не шарю
Я в латексе от слова вообще не шарю
латех*
NK
латех*
А в какой программе ты пилишь?
EZ
ID:200200555
А в какой программе ты пилишь?
Tex studio + Tex Live
NK
Tex studio + Tex Live
Спасибо
NK
Пойду планировать часы изучения
t
мир дому вашему
NK
мир дому вашему
И Вам здарова
MK
А в чем принципиальная разница между чд и нз в данном случае? Ну прост как я вижу, в случае с чд гравитационные волны намного проще обнаружить - кроме большей массы они могут еще и вращаться до упора, а нейтронные звезды резлетятся на самом интересном месте
В остальном смысл тот же, разница количественная (2 оч массивных объекта, которые оч быстро вращаются друг вокруг друга, что само по себе должно создавать гравитационные волны)
В остальном смысл тот же, разница количественная (2 оч массивных объекта, которые оч быстро вращаются друг вокруг друга, что само по себе должно создавать гравитационные волны)
Да нет разницы в этом случае
MK
Вот еще интересная вещь:
MK
A gravity wave requires a quadrupolar deformation of space time. Not linear, not circular, but quadrupolar.
A single object just sitting there, or moving with a constant velocity (which is equivalent to stationary via Galilean invariance) does not produce a quadrupolar deformation. So a solitary black hole can never emit gravity waves.
This is why you have to have two orbiting black holes (like in a black hole merger) to emit gravity waves.
Technically speaking, it’s because the graviton is a spin=2 particle, and spin 2 corresponds to the quadrupolar mode in a spherical harmonic expansion.
Finally, let me point out that the two protons colliding won’t necessarily produce a black hole. The Schwarzschild radius of such a black hole would be way smaller than the Planck length, so we don’t have a theory that would describe this.
A single object just sitting there, or moving with a constant velocity (which is equivalent to stationary via Galilean invariance) does not produce a quadrupolar deformation. So a solitary black hole can never emit gravity waves.
This is why you have to have two orbiting black holes (like in a black hole merger) to emit gravity waves.
Technically speaking, it’s because the graviton is a spin=2 particle, and spin 2 corresponds to the quadrupolar mode in a spherical harmonic expansion.
Finally, let me point out that the two protons colliding won’t necessarily produce a black hole. The Schwarzschild radius of such a black hole would be way smaller than the Planck length, so we don’t have a theory that would describe this.
MK
QM suggests that whatever form of matter turns into a black hole or gets added to a black hole would be sorted into layers corresponding to the wavelengths of various particles, with a background of photons of a continuous distribution of wavelengths.
These particles would have to be nearly all bosons, in order to be in the same quantum state together, as a Bose-Einstein condensate. Fermions all have to be in different quantum states. They can support quite large pressures, but there are limits. In white dwarf stars electron degeneracy pressure holds up to the Chandrasekhar limit of 1.44 solar masses. At that point, or even a little below it, electrons and protons combine to form neutrons.
In neutron stars neutron degeneracy pressure holds up to the Tolman-Oppenheimer-Volkhov limit, which is not known to the same precision, but is only a few solar masses. At that point the neutrons must turn into bosons, but we have no knowledge of which ones those might be.
No other fermions that we know of could hold up under any greater pressure. Bosons can be in the same quantum state in a Bose-Einstein condensate in any quantity, up to billions of solar masses, as far as we know.
We do not know what particular bosons might form in a collapsing neutron star, and there is much more that we do not know about conditions inside a black hole, but these are fundamental principles that no proposed theory of quantum gravity provides any exceptions for. Another thing that we do know is that matter can quantum tunnel from the core of a black hole out to any distance. Nearly all of it will materialize within the event horizon and fall straight back, but some can materialize outside the event horizon and escape as Hawking radiation.
These particles would have to be nearly all bosons, in order to be in the same quantum state together, as a Bose-Einstein condensate. Fermions all have to be in different quantum states. They can support quite large pressures, but there are limits. In white dwarf stars electron degeneracy pressure holds up to the Chandrasekhar limit of 1.44 solar masses. At that point, or even a little below it, electrons and protons combine to form neutrons.
In neutron stars neutron degeneracy pressure holds up to the Tolman-Oppenheimer-Volkhov limit, which is not known to the same precision, but is only a few solar masses. At that point the neutrons must turn into bosons, but we have no knowledge of which ones those might be.
No other fermions that we know of could hold up under any greater pressure. Bosons can be in the same quantum state in a Bose-Einstein condensate in any quantity, up to billions of solar masses, as far as we know.
We do not know what particular bosons might form in a collapsing neutron star, and there is much more that we do not know about conditions inside a black hole, but these are fundamental principles that no proposed theory of quantum gravity provides any exceptions for. Another thing that we do know is that matter can quantum tunnel from the core of a black hole out to any distance. Nearly all of it will materialize within the event horizon and fall straight back, but some can materialize outside the event horizon and escape as Hawking radiation.
EZ
QM suggests that whatever form of matter turns into a black hole or gets added to a black hole would be sorted into layers corresponding to the wavelengths of various particles, with a background of photons of a continuous distribution of wavelengths.
These particles would have to be nearly all bosons, in order to be in the same quantum state together, as a Bose-Einstein condensate. Fermions all have to be in different quantum states. They can support quite large pressures, but there are limits. In white dwarf stars electron degeneracy pressure holds up to the Chandrasekhar limit of 1.44 solar masses. At that point, or even a little below it, electrons and protons combine to form neutrons.
In neutron stars neutron degeneracy pressure holds up to the Tolman-Oppenheimer-Volkhov limit, which is not known to the same precision, but is only a few solar masses. At that point the neutrons must turn into bosons, but we have no knowledge of which ones those might be.
No other fermions that we know of could hold up under any greater pressure. Bosons can be in the same quantum state in a Bose-Einstein condensate in any quantity, up to billions of solar masses, as far as we know.
We do not know what particular bosons might form in a collapsing neutron star, and there is much more that we do not know about conditions inside a black hole, but these are fundamental principles that no proposed theory of quantum gravity provides any exceptions for. Another thing that we do know is that matter can quantum tunnel from the core of a black hole out to any distance. Nearly all of it will materialize within the event horizon and fall straight back, but some can materialize outside the event horizon and escape as Hawking radiation.
These particles would have to be nearly all bosons, in order to be in the same quantum state together, as a Bose-Einstein condensate. Fermions all have to be in different quantum states. They can support quite large pressures, but there are limits. In white dwarf stars electron degeneracy pressure holds up to the Chandrasekhar limit of 1.44 solar masses. At that point, or even a little below it, electrons and protons combine to form neutrons.
In neutron stars neutron degeneracy pressure holds up to the Tolman-Oppenheimer-Volkhov limit, which is not known to the same precision, but is only a few solar masses. At that point the neutrons must turn into bosons, but we have no knowledge of which ones those might be.
No other fermions that we know of could hold up under any greater pressure. Bosons can be in the same quantum state in a Bose-Einstein condensate in any quantity, up to billions of solar masses, as far as we know.
We do not know what particular bosons might form in a collapsing neutron star, and there is much more that we do not know about conditions inside a black hole, but these are fundamental principles that no proposed theory of quantum gravity provides any exceptions for. Another thing that we do know is that matter can quantum tunnel from the core of a black hole out to any distance. Nearly all of it will materialize within the event horizon and fall straight back, but some can materialize outside the event horizon and escape as Hawking radiation.
дал бы ссылку уже вместо таких простыней
MK
дал бы ссылку уже вместо таких простыней
Если тебе интересно, то загуглишь
EZ
Если тебе интересно, то загуглишь
дело не в том, интересен ли мне источник, а вто, что сообщения на 5 экранов - это неудобно
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