MAGNETIZED DISKS AROUND YOUNG STARS

被引：0

作者：

Lizano, S. ^{[1
]}

Shu, F. H. ^{[2
]}

Galli, D. ^{[3
]}

Glassgold, A. ^{[4
]}

机构：

[1] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Apdo Postal 3-72, Morelia 58090, Michoacan, Mexico

[2] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA

[3] Osserv Astrofis Arcetri, I-50125 Florence, Italy

[4] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

来源：

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

关键词：

accretion; accretion disks; ISM: magnetic fields; stars: formation; stars: pre-main sequence; ACCRETION DISKS; FIELD;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We discuss the structure and evolution of a magnetized accretion disks around young stars that have dragged their magnetic field in the process of gravitational collapse. The disk evolves due to two diffusive processes: viscous stresses that redistribute mass and angular momentum, and the resistive diffusion of mass across magnetic field lines due to imperfect conduction. In steady-state there is an analytic model of the structure of these magnetized disks. We discuss the application of this model to disks around low and high mass young stars and recent results of time dependent models.

引用

页码：149 / +

页数：2

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