OSWAGO AST 311 - Astronomy 311 Lecture 2 - Solar System Formation (3 pages)

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Astronomy 311 Lecture 2 - Solar System Formation



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Astronomy 311 Lecture 2 - Solar System Formation

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Pages:
3
School:
State University of New York at Oswego
Course:
Ast 311 - Solar System Astronomy

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Astronomy 311 Lecture 2 Solar System Formation Solar Nebula Theory Cold dense molecular gas cloud starts to contract it satsified the Jeans mass criterion Spins heats up and flattens out Proto Sun at the center Angular momentum transferred from the protoSun to outside through viscous drag Initially temperature rises in the SN but eventually it starts to cool Material starts to condense from gas to solid in dust grains following whether its a refractory or volatile material Less than 5AU ices never condense Greater than 5AU ices do condense These dust grains condense to central plane of the nebula Grow by gentle collisions sticking together by magnetism electrostatic charges etc This is also called coagulation Normal grains in the interstellar medium are maybe between 100 10 10 m to 0 2 10 6 m and consist of carbons and silicates mainly In the SN coagulation results in these grains becoming 0 1 10km in size in a few hundred thousand years This grain growth is a very hot topic today Chondrules are carbon rich materials embedded in silicate rich surroundings seen in meteorites and represent the possible types of grains available for coagulation A planetismal is something about 10km in diameter Only 10km large rocks are generally large enough to attract other grains rocks to it through gravitational attraction That is after a rock reaches 10km in size it grows further through encouraging collisions through gravitational attraction This leads to one large body or planetary embryo forming by swallowing up all the other smaller bodies runaway growth is where one planetisimal grew more than others Larger bodies grew more rapidly than smaller ones while the total mass in smaller bodies declined At 1AU such planetary embryos are about 1 10 mass of the current Earth and takes about 104 105 years to come about In the outer part of the SS planetary embryos could be perhaps an Earth size mass and take about 105 years to form The terrestrial planets formed by collisions between



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