MAGNETIC BRAKING AND FIELD DISSIPATION IN THE PROTOSTELLAR ACCRETION PHASE

被引：0

作者：

Galli, D. ^{[1
]}

Cai, M. ^{[2
]}

Lizano, S. ^{[3
]}

Shu, F. H. ^{[4
]}

机构：

[1] Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy

[2] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan

[3] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico

[4] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA

来源：

MAGNETIC FIELDS IN THE UNIVERSE II: FROM LABORATORY AND STARS TO THE PRIMORDIAL UNIVERSE | 2009年 / 36卷

关键词：

ISM: clouds; ISM: magnetic fields; MHD; planetary systems: protoplanetary disks; stars: formation; MOLECULAR CLOUD CORES; SINGULAR ISOTHERMAL TOROIDS; SELF-SIMILAR COLLAPSE; TIME-DEPENDENT SOLUTION; STAR-FORMATION; GRAVITATIONAL COLLAPSE; DARK CLOUDS; DENSE CORES; FLUX; MAGNETOHYDRODYNAMICS;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We summarize recent theoretical work addressing the role of magnetic fields in the process of star formation. First, we concentrate on the efficiency of magnetic braking during cloud collapse and its consequences on the formation of centrifugally supported disks around young stars. Then, we relate this issue to the well-known magnetic flux problem of star formation, and we show that the introduction of non-ideal MHD effects is a necessary step toward the development of self-consistent models for the collapse of molecular clouds and the formation and evolution of accretion disks around young stars.

引用

页码：143 / +

页数：2

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