what is the ultimate fate of an isolated white dwarf ?
what is the ultimate fate of an isolated white dwarf？
What is the ultimate fate of an isolated white dwarf? It will cool down and become a cold black dwarf.
Long,What happens to a white dwarf when it accretes enough matter to approach the 1.4 MSun limit?
What happens to a white dwarf when it accretes enough matter to reach the 1.4MSun limit? It explodes. Massive star supernova: Iron core of massive star reaches white dwarf limit and collapses into a neutron star, causing an explosion.
Correspondingly,What is the ultimate fate of a pulsar?
What is the ultimate fate of an isolated pulsar? It will spin ever slower, the magnetic field will weaken, and it will become invisible.
Likewise,What happens when a white dwarf accretes enough mass to reach the 1.4 solar mass white dwarf limit quizlet?
What happens if its mass reaches the 1.4 solar mass limit? A white dwarf can never gain enough mass to reach the limit because a strong stellar wind prevents the accreting material from reaching it in the first place. The white dwarf undergoes a collapse and expels the excess mass in a nova eruption.
Furthermore,What is the reason why there is an upper mass limit for white dwarfs?
This is because the more mass a white dwarf has, the more its electrons must squeeze together to maintain enough outward pressure to support the extra mass. However, there is a limit on the amount of mass a white dwarf can have. Subrahmanyan Chandrasekhar discovered this limit to be 1.4 times the mass of the Sun.
What happens to a white dwarf that reaches its solar mass limit through accretion from a binary companion star quizlet?
A white dwarf in a close binary system will explode as a supernova if it gains enough mass to exceed the "white dwarf limit (1.4 solar masses)". A(n) "accretion disk" consists of hot, swirling gas captured by a white dwarf (or neutron star or black hole) from a binary companion star.
What makes white dwarf Supernovae useful to astronomers?
What makes white dwarf supernovae useful to astronomers? a. They are all thought to have approximately the same luminosity so they can be used measure distances to very distant galaxies.
What happens when a white dwarf hits the 1.4 solar mass limit?
A white dwarf star is in balance between gravity and degeneracy pressure, but if the mass is too large (greater than 1.4 solar masses, called the Chandrasekhar limit), the degeneracy pressure is not adequate to hold up the star, and the star collapses.
When a white dwarf accretes enough material and reaches the 1.4 solar masses limit its temperature becomes hot enough for carbon fusion What happens next?
What happens to a white dwarf when it accretes enough material to reach the 1.4 Msun limit? It explodes. It collapses into a neutron star. It gradually begins fusing carbon in its core.
What happens if a white dwarf reaches the 1.4 MSun limit it explodes as a white dwarf supernova it collapses to become a neutron star it collapses to become a black hole?
- neutron star or black hole left behind. White dwarf supernova: -Carbon fusion suddenly begins as white dwarf in close binary system reaches 1.4 MSun limit, causing a total explosion of the white dwarf. - nothing left of the star!
What does Einstein's general theory of relativity tell us about two white dwarfs orbiting one another very close together quizlet?
Einstein's general theory of relativity tells us that two white dwarfs orbiting especially close together should emit gravitational waves, and these waves carry energy and angular momentum away from the system. The result is that the two white dwarfs gradually spiral inward towards each other.
How could we tell observationally If a supernova is a white dwarf supernova or a massive star supernova?
Observationally, how can we tell the difference between a white-dwarf supernova and a massive-star supernova? The spectrum of a massive-star supernova shows prominent hydrogen lines, while the spectrum of a white-dwarf supernova does not.
What kind of pressure supports a white dwarf quizlet?
White dwarfs are the remaining cores of dead stars. Electron degeneracy pressure supports them against gravity.