ASTRON C10 Lecture Notes - Lecture 21: Type Ia Supernova, Nucleosynthesis, Spiral Galaxy

• School: Berkeley
• Department: Astronomy
• Course: ASTRON C10
• Professor: Alexei Filippenko

Document Summary

Single stars evolve in a simple manner: lifetime of main sequence mainly dependent on. On main sequence, they don"t matter much. As larger star goes into red giant, then massive star fills its roche lobe and can start to flow out of roche lobe. Partner star starts to grow up faster with larger mass. Matter can flow back from the smaller star as it evolves off its main sequence and spill back into the other star. An old star with a new lease on life. White dwarf is given material from the the partner star. Star brightens by a factor of 102-106 in a small period of time and fad over time. Matter from disk suddenly falls onto wd >star brightens (x100) Material can gradually rain down onto surface of wd. Nuclear reactions spontaneously occur on surface uncontrolled. Previously normal star suddenly brightens and becomes much more luminous. (up to. Can rival in brightness an entire galaxy in brightness.