D.2. Stellar Evolution

a) Gravitational contraction

b) Nuclear fission

c) Nuclear fusion

d) Chemical reactions

a) The star collapses into a black hole.

b) The star explodes in a supernova.

c) The star expands into a red giant.

d) The star remains stable and its temperature decreases.

a) Its age

b) Its mass

c) Its composition

d) Its temperature

a) Oppenheimer-Volkoff limit

b) Chandrasekhar limit

c) Stellar mass limit

d) Fusion limit

a) It is formed from the collapse of a star's core exceeding the Chandrasekhar limit.

b) It is primarily composed of hydrogen and helium.

c) It is the final stage of all stars.

d) It is supported by the pressure of tightly packed neutrons.

a) Both temperature and pressure decrease.

b) Both temperature and pressure increase.

c) Temperature increases, pressure decreases.

d) Temperature decreases, pressure increases.

a) Hydrogen fusion in the core

b) Shell burning of hydrogen around a helium core

c) Helium fusion in the core

d) Gravitational collapse

a) It will explode in a supernova.

b) It will continue to cool down and eventually become a black hole.

c) It will continue to cool down indefinitely.

d) It will reignite nuclear fusion in its core.

a) Neutron stars are denser than white dwarfs.

b) Neutron stars have a stronger magnetic field.

c) Neutrons experience a stronger degeneracy pressure than electrons.

d) Neutron stars are remnants of stars with lower initial mass.