Lecture08

Lecture08 - Previous Lecture Angular momentum and star...

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Previous Lecture Angular momentum and star formation Protostars and their evolution evolutionary tracks on HR diagram Extremes of star formation, mass limits <0.085 M sun brown dwarf >~100 M sun blows itself apart T Tauri stars Herbig-Haro objects Planet formation
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Stellar Structure Key physical relationships: hydrostatic equilibrium: pressure vs. gravity mass/density equation energy source equation (nuclear energy) energy transport: convection or radiation equation of state (ideal gas law) gas opacity Stellar model description of all important physical characteristics as a function of position in the star usually spherical geometry simplifying fact: stellar material is a gas
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Nuclear Energy in Stars Structure of the nucleus size ~ 10 -15 m composed of neutrons (no electrical charge) and protons (positive charge) Two new forces strong nuclear force: overcomes the electrical repulsion of protons, binds nucleus weak nuclear force: mediates radioactive decay both are short range – effective over nuclear size only
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Conditions for nuclear interactions: nuclei must be close together for nuclear force to be effective high density high temperature (high speed)
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This note was uploaded on 01/31/2012 for the course 750 110 taught by Professor Ericgawaiser during the Fall '10 term at Rutgers.

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Lecture08 - Previous Lecture Angular momentum and star...

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