13: Stellar Finale
- Page ID
- 115287
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Introduction
In this chapter we will discuss the end-states of stars. Just as the length of a star's life is dependent on its initial mass, what a star looks like at the end of its life also depends on mass. Almost all stars end in a bang, but the size of the explosion also depends on its initial mass and whether it has one or more companion stars.
- Distinguish the mass range of stars that will become white dwarfs
- Describe the interior of a massive star before a supernova
- Describe the observed features of SN 1987A both before and after the supernova
- Explain the research method that led to the discovery of neutron stars
- Describe the features of a neutron star that allow it to be detected as a pulsar
- List the observational evidence that links pulsars and neutron stars to supernovae
- Describe the kind of binary star system that leads to a nova event
- Describe the type of binary star system that leads to a type Ia supernovae event
- Indicate how type Ia supernovae differ from type II supernovae
Thumbnail: When a massive star exploded in the Large Magellanic Cloud, a satellite galaxy to the Milky Way, it left behind an expanding shell of debris called SNR 0519-69.0. Here, multimillion degree gas is seen in X-rays from Chandra in blue. The outer edge of the explosion in red and stars in the field of view are in visible light from Hubble. (Public Domain; X-ray: NASA/CXC/Rutgers/J.Hughes; Optical: NASA/STScI via Wikimedia Commons)