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Models of Stellar Structure
•Divide star into thin shells,calculate how following vary from shell to
shell
(i.e. as function of radius r)
(i.e. as function of radius r)
–P (Pressure)
–T (Temperature)
–r (Density)
•To do
this also need to find:
–M (Mass) contained within any r
–L (Luminosity) generated within any r
•P example:
From our text: Horizons, by Sees