Abstract
The star formation era is a period during which rotational effects are of crucial importance in determining the evolution of the star. Also, during this period, significant redistribution of angular momentum must occur in the star, as indicated by the substantial discrepancy between deduced angular momenta in star formation sites in the cores of molecular clouds and in the youngest optically visible stars. A major problem is the short time scale, comparable to a few initial free-fall times of the cloud core, in which this redistribution must take place. The following questions will be considered in this paper: (1) What is the origin of the angular momentum of stars? (2) What is the observational evidence for the existence of angular momentum at the earliest stages of star formation? (3) How serious is the so-called angular momentum problem? (4) For the solution of the angular momentum problem, what kinds of angular momentum transport processes are available and at what stages of star formation do they probably operate? (5) What recent theoretical information is available regarding the evolution of rotating protostars? (6) To what extent can the angular momentum problem be solved by the formation of binary or multiple systems and disks? (7) Given that the T Tauri stars, even near the birthline, are rotating slowly, what is a possible sequence of events in the evolution of the angular momentum distribution that could bring them to this state?
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