What is the meaning of thermal spectral function and thermal decay width in thermal field theory?
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Stellar evolution in brief:
A star begins its life as a shrinking clump of gas and dust called a protostar. It stops shrinking when nuclear fusion reactions start in its core. The first reactions fuse hydrogen to make helium. Later, helium is changed into carbon, oxygen, and—in the biggest stars—iron. Eventually, there is nothing left to burn and the star collapses. For a few massive stars, this results in a supernova explosion. Most of the star’s matter is blown away by the supernova. The star’s collapsed core may survive as a neutron star or a black hole.
Stellar evolution in brief:
A star begins its life as a shrinking clump of gas and dust called a protostar. It stops shrinking when nuclear fusion reactions start in its core. The first reactions fuse hydrogen to make helium. Later, helium is changed into carbon, oxygen, and—in the biggest stars—iron. Eventually, there is nothing left to burn and the star collapses. For a few massive stars, this results in a supernova explosion. Most of the star’s matter is blown away by the supernova. The star’s collapsed core may survive as a neutron star or a black hole.
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