Exam 13: Stellar Evolution: the Lives and Deaths of Stars

Stable fusion reactions end when builds in a high- mass star's core.

The helium flash converts helium into _.

During the hydrogen shell burning phase

What are two differences observed between Type I and Type II supernovae?

A star system can become a Type I supernova several times.

Our Sun will never become hot enough for carbon nuclei to fuse.

Most of our knowledge of stellar evolution comes from studies of .

Low- mass stars may become hundreds of times more luminous as giants than they were on the main sequence.

The Chandrasekhar limit is

The blue stragglers represent the horizontal branch for globular clusters.

Will our Sun become a supernova? Why?

The helium flash is followed within a few million years by the Type II supernova.

As their name implies, all planetary nebulae feature spherical shells and look like the disks of Uranus or Neptune.

Massive stars form cores of before exploding as Type II supernovae.

The luminosity of the red giant during its second trip to the upper right on the H- R diagram is less than before the helium flash expansion.

Supernova 1987A was the first supernova observed by astronomers since Galileo first turned a telescope to the heavens.

What is the typical age for a globular cluster associated with our Milky Way?

Although mass transfer can occur in binary stars, the small mass change does not impact the evolution of either companion.

When a low- mass star runs out of hydrogen in its core, it gets brighter. Why?

Because they all involve formation of iron in the cores of massive stars, all Type II supernovae are approximately equally luminous.