Mixing processes in the interstellar medium

A fine account of the structure and content of galaxies is given in Mihalas and Binney (1981) and excellent introductions to many questions in GCE are to be found in Truran and Cameron (1971) and Tinsley (1980). A good modern account of the kinematics and abundance distribution of the Galaxy is given by Gilmore, Wyse and Kuijken (1989). 

The question of upper mass limits to stars which explode as SN II and leave neutron-star remnants is discussed by Maeder (1992,1993) and by Brown, Bruenn and Wheeler (1992) it is highly controversial. (Note that Koppen and Arimoto (1991) when referring to the Scalo IMF use the version with b T) = 1, as I have done, whereas Maeder (1993) uses the version with b (T) = 0.48, corresponding to yields that are 3 times higher ) 

Interesting variants on the simplest star formation laws include stochastic self-propagating star formation (Gerola Seiden 1978 Dopita 1985), self-regulating star formation (Arimoto 1989 Hensler Burkert 1990), stochastic star-formation bursts (Matteucci Tosi 1985), separate laws for the halo and disk, the latter including terms that account for cloud collisions and induced star formation from interactions between massive stars and clouds (Ferrini et al. 1992, 1994), and the existence of a threshold surface gas density for star formation (Kennicutt 1989 Chamcham, Pitts Tayler 1993). 

Galactic chemical evolution basic concepts and issues 

Use the IMFs in Table 7.8 to calculate the relative numbers of stars more massive than 0.1 M born with less and more mass than 1M . 

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