The upper limit to the mass of a white dwarf (equals 1.4 times the mass of the sun).
theoretical limit below which a low-mass star can evolve into a white dwarf at the end of its life. Its value is 1.4 solar masses.
The theoretical upper limit at which a stellar remnant can form a white dwarf. Beyond this value (~1.4 solar masses) the electron degeneracy pressure is unable to withstand gravitational collapse and the electrons are forced into the nucleus where they combine with protons to form a dense sea of neutrons. The remnant star is then a neutron star.
the maximum mass for which a degenerate gas can support itself against gravity (1.4 solar masses).
The mass below which dying stars form white dwarves. Above this mass a star will become either a neutron star or a black hole. The limit was famously calculated by the Indian physicist Subrahmanyan Chandrasekhar, on the steamer to Liverpool, when he was on the way to take up a place at Cambridge.
The theoretical upper limit on the mass of a white dwarf, 1.4 solar masses. A white dwarf exceeding the Chandrasekhar limit will go supernova.
The mass beyond which a white dwarf must inevitably collapse into a neutron star, about 1.4 solar masses.
The maximum mass of a white dwarf, about 1.4 solar masses. A white dwarf of greater mass can not support itself and will collapse.
Equal to 1.4 solar masses, the maximum mass a dying star may have and still turn into a white dwarf star. Dying stars with masses greater than 1.4 solar masses collapse into neutron stars or black holes. Subrahamanyan Chadrasekhar, at age 19 in 1930, worked out this limiting mass while on a steamship to England, where he planned to present his astrophysical work.
The maximum mass of a white dwarf, 1.4 solar masses. Beyond this mass, the star collapses into a neutron star or black hole depending on the mass of the collapsing core. Subrahamanyan Chadrasekhar, at age 19 in 1930, worked out this limiting mass while on a steamship to England.
The Chandrasekhar limit is the maximum mass which can be supported against gravitational collapse by electron degeneracy pressure. It is commonly given as being about 1.4 or 1.44 solar masses. Computed values for the limit will vary depending on the nuclear composition of the mass and the approximations used.