The endpoint of stellar evolution for stars with intermediate masses, FTP, name these stars that, as their name implies, are often colorless and small.
Radiation from these bodies is uniquely dominated by thermal diffusion due to non-degenerate ionic states in their cores. Objects of this type are prevented from collapse by electron degeneracy pressure and are consequently highly compact. For an astronomical body of this type, a solution for the special relativistic equation for the wave function of the electrons yields a unique mass-radius relation, but this only has a meaningful solution for objects below a certain mass, which is known as the Chandrasekhar limit. The endpoint of stellar evolution for stars with intermediate masses, FTP, name these stars that, as their name implies, are often colorless and small.
Radiation from these bodies is uniquely dominated by thermal diffusion due to non-degenerate ionic states in their cores.
white dwarf stars [or white dwarves]