ASTR 001 Lecture Notes - Lecture 19: Moe Williams, Solar Mass, Star Cluster
15 Jul 2020
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Document Summary
Each stage of burning is progressively shorter. Example: si burning lasts for only a few days. Huge production of neutrinos, which carry away energy (neutrino cooling) The star cannot access the huge amount of energy produced in neutrinos. Photodisintegration, neutrino cooling reduces pressure, collapse accelerates. At these high densities, nuclear forces repel atoms. Core stops, bounces back, driving a shock wave through the star. Shock wave takes a mere few hours to rip through the star. Outer layers blow off in tremendous explosion (type ii supernova) If the star is not too massive, the type ii supernova leaves behind a neutron-degenerate core: neutron star. Mass between 1. 4 and 3 solar mass, radius ~ 10km. Some neutron stars are found in x-ray binaries, and give off strong x-rays. Others are found as pulsars (rapidly rotating neutron stars) Beam of radiation sweeps by earth like a lighthouse beam.
