Chandrasekhar limit

In such a case, the total mass would not be constrained by the Chandrasekhar limit.

Stars with masses above the Chandrasekhar limit, on the other hand, have a big problem when they come to the end of their fuel.

The key to the similarity is the relationship between the Chandrasekhar limit and the supernova process.

The limiting mass is now called the Chandrasekhar limit.

If the accretion continues long enough, the white dwarf may eventually approach the Chandrasekhar limit.

The infalling matter pushes the white dwarf over the Chandrasekhar limit.

Obviously, that means that the white dwarf must approach the Chandrasekhar limit from below.

A dwarf that's already near its Chandrasekhar limit.

Chandrasekhar limit: The maximum possible mass of a stable cold star, above which it must collapse into a black hole.

The Chandrasekhar limit is named after him.

The Chandrasekhar limit is surpassed from the infalling matter.

This number is called the Chandrasekhar limit.

Here I am talking about the Chandrasekhar limit for Neutron stars.

Chandrasekhar's most notable work was the astrophysical Chandrasekhar limit.

Mass transfer in a binary system may cause an initially stable white dwarf to surpass the Chandrasekhar limit.

Eventually, the white dwarf could explode as a type Ia supernova if it approaches the Chandrasekhar limit.

The white dwarf strips gas from its companion's envelope until it has gathered enough to reach the Chandrasekhar limit, after which it explodes.

Electron degeneracy pressure will halt the gravitational collapse of a star if its mass is below the Chandrasekhar limit (1.44 solar masses).

The mass of an isolated, nonrotating white dwarf cannot exceed the Chandrasekhar limit of 1.4 solar masses.

When they finally merge, if their combined mass approaches or exceeds the Chandrasekhar limit, carbon fusion is ignited, raising the temperature.

This iron core is pushed towards the Chandrasekhar limit till it surpasses it and therefore collapses.

There is a limit to how massive a white dwarf can be: the Chandrasekhar limit, which is about 1.4 times the mass of the Sun.

When the core's mass exceeds the Chandrasekhar limit of about 1.4 solar masses, degeneracy pressure can no longer support it, and catastrophic collapse ensues.

As another example of its many applications, the virial theorem has been used to derive the Chandrasekhar limit for the stability of white dwarf stars.

This happens when a stellar core above 1.44 solar masses, the Chandrasekhar limit, collapses and is not halted by the degenerate electrons.