Sep 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978ispv.rept.....w&link_type=abstract
Presented at the Intern. School of Phys., Varenna, Italy, 26 Jun. - 7 Jul. 1978
Physics
Mathematical Models, Stellar Evolution, Stellar Models, Implosions, Interstellar Gas, Spiral Galaxies
Scientific paper
Theoretical models of star formation are discussed beginning with the earliest stages and ending in the formations of rotating, self-gravitating disks or rings. A model of the implosion of very diffuse gas clouds is presented which relies upon a shock at the edge of a galactic spiral arm to drive the implosion. Models are presented for the formation of a second generation of massive stars in such a cloud once a first generation has formed. These models rely on the ionizing radiation from massive stars or on the supernova shocks produced when these stars explode. Calculations of the gravitational collapse of rotating clouds are discussed with special focus on the question of whether rotating disks or rings are the result of such a collapse.
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