AST 309 Lecture Notes - Lecture 16: Spiral Galaxy, Density Wave Theory, Protoplanetary Disk
Document Summary
Low mass stars with a companion stages (earliest to latest) Most massive high mass stars stages(earliest to latest) Gfdj (if a bit less massive, then you"ll end up as a neutron star) Molecular cloud cores may need a push to get the collapse process started. Supernova (type ii) explosions, winds, outflows, and shock waves in the ism may all be triggers that could initiate the collapse process. New stars triggered by winds and shocks from massive stars. Massive stars sweep up material, they create advancing ionization and shock fronts which can compress the gas. Possible sequence for triggered star formation in hii regions ay all hich. Gas in a molecular cloud is not of uniform density. As ionization front moves into molecular gas, and over denser clumps, those are more likely to collapse. Compresses the molecular gas and continues over dense clumps. Scenario if most lower mass stars are not influenced/ triggered by shocks created by massive stars: s the.
