Modeling feedback process

Stellar feedback is important because it is found in earlier modelings that given min(dMcool/dt, dMinfall/dt) and n(M,z) and integrate forward, all the cold gas would be depleted by now for reasonable b choices. But the accuracy of the feedback modeling is still quite uncertain.

Consider a simple model of feedback by Supernovae. Given the IMF, suppose the number of SNe expected per unit mass of star formation is , energy input per SNe is ESN, then the amount of cold gas lost during t is

Mreheat= ESN t/Vc2,

where Vc is the virial circular velocity, contains efficiency of the SNe energy for reheating and is taken as a free parameter.

Since they affect each other the star-forming and feedback processes can be modeled in a single equation. See for example Cole et al. (1994).

References page
Introduction page

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Fan Fang       Last update: 26-July-99