2003/12/11 by Arieh Königl, A. Konigl, Konigl, A.
Physics and Astronomy · #Astro and Planetary Science #Astrophysics (astro-ph) #Astrophysics and Star Formation Studies #FOS: Physical sciences #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0312287
8 pages, 2 figures, to appear in Star Formation in the Interstellar Medium, proc. of workshop in honor of David Hollenbach, Chris McKee and Frank Shu, held at Granlibakken, Lake Tahoe, June 29-July 3, 2003 (ASP. Conf. Ser.)
arxiv created 2003/12/11 · openalex publication_date 2003/12/11 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Newly formed stars are often observed to possess circumstellar disks, from which mass continues to be accreted onto the star and fed into outflowing jets, and which eventually may evolve into dusty debris disks and planetary systems. Recent modeling developments have made it possible, for the first time, to study the formation and early evolution of rotationally supported protostellar disks in the context of a realistic scenario of star formation in weakly ionized, magnetic, molecular cloud cores. The derived semianalytic solutions incorporate ambipolar diffusion and magnetic braking and may be extended to include centrifugally driven disk winds; they can be used to examine the full range of expected behaviors of real systems and their dependence on physical parameters.