ANGULAR-MOMENTUM TRANSFER DUE TO GALACTIC WINDS AND COOLING FLOWS

The interaction of a slowly rotating halo with an early galactic super wind is investigated. Two cases of the halo are assumed: a) rich in co ld clouds, b) constituted by diffuse gas. In the first case, the cloud s evaporate due to the shock-wave and their matter is mixed with the w ind to a uniform mixture. In the second case, a cold shell is formed a t large distance from the center. Fragmentation of this shell leads to the appearance of a stellar shell whereas the remaining clouds are fr ee-falling to the center of the system. In both cases a strong redistr ibution of the mass is taking place which leads to angular momentum tr ansfer from the outer to the inner regions. By the same way the mass a nd angular momentum can be redistributed by quasi-stationary cooling f lows with cloud formation. Some applications of the above mechanisms t o the structure of the disk of spiral galaxies are discussed.