In the Hertzsprung-Russell diagram, an instability strip characterized by GW Vir stars contains stars which later evolve into this class of stars. Variable-luminosity stars of this type include DBV and DAV, or ZZ Ceti, stars. These stars which are composed of electron-degenerate matter occupy a strip across the bottom-left of the Hertzsprung-Russell diagram, and one of these stars may collapse into a neutron star if it exceeds 1.4 solar masses, known as the Chandrasekhar limit. For 10 points, na
In the Hertzsprung-Russell diagram, an instability strip characterized by GW Vir stars contains stars which later evolve into this class of stars. Variable-luminosity stars of this type include DBV and DAV, or ZZ Ceti, stars. These stars which are composed of electron-degenerate matter occupy a strip across the bottom-left of the Hertzsprung-Russell diagram, and one of these stars may collapse into a neutron star if it exceeds 1.4 solar masses, known as the Chandrasekhar limit. For 10 points, name this class of dwarf stars.
In the Hertzsprung-Russell diagram, an instability strip characterized by GW Vir stars contains stars which later evolve into this class of stars.
White Dwarf [prompt on Dwarf]