期刊
ASTROPHYSICAL JOURNAL
卷 632, 期 2, 页码 L135-L138出版社
UNIV CHICAGO PRESS
DOI: 10.1086/498066
关键词
accretion, accretion disks; MHD; stars : magnetic fields; stars : pre-main-sequence; stars : rotation; stars : winds, outflows
We compare the angular momentum extracted by a wind from a pre-main-sequence star to the torques arising from the interaction between the star and its Keplerian accretion disk. We find that the wind alone can counteract the spin-up torque from mass accretion, solving the mystery of why accreting pre-main-sequence stars are observed to spin at less than 10% of breakup speed, provided that the mass outflow rate in the stellar winds is similar to 10% of the accretion rate. We suggest that such massive winds will be driven by some fraction epsilon of the accretion power. For observationally constrained typical parameters of classical T Tauri stars, epsilon needs to be between a few and a few tens of percent. In this scenario, efficient braking of the star will terminate simultaneously with accretion, as is usually assumed to explain the rotation velocities of stars in young clusters.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据