Magnetospheric Accretion Models for the Hydrogen Emission Lines of T Tauri Stars
Magnetospheric Accretion Models for the Hydrogen Emission Lines of T Tauri Stars
复制标题
金牛座 T 星氢发射线的磁层吸积模型
DOI：
10.1086/305069
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发表时间：
1998
期刊：
影响因子：
--
通讯作者：
L. Hartmann
中科院分区：
文献类型：
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作者：
J. Muzerolle;N. Calvet;L. Hartmann
利用统计平衡辐射转移处理，我们研究了经典T-Tauri恒星磁层坠落带产生的氢发射线的行为。在计算了巴耳末谱线PAβ和BRγ的自洽谱线轮廓后，我们探索了参数空间，考察了磁层气体温度和大小对谱线通量的影响。我们比较了巴尔默线的模型通量和观测的线通量，发现使用相对较小的参数范围就能很好地匹配。我们还能够匹配观测到的嵌入天体WL16的BRγ谱线轮廓，这支持即使在恒星形成的最早阶段也使用红外线来研究磁层坠落。最后，我们讨论了物理参数的约束以及用发射线作为吸积率指示器的可能性。
Using a statistical equilibrium radiative transfer treatment, we examine the behavior of hydrogen emission lines arising from the magnetospheric infall zones of classical T Tauri stars. Having calculated self-consistent line profiles of the Balmer lines, Paβ and Brγ, we explore parameter space, examining the effects of the magnetospheric gas temperature and size on the line fluxes. We compare model and observed line fluxes for the Balmer lines and find a good match using a relatively small range of parameters. We are also able to match the observed Brγ line profile of the embedded object WL 16, which supports the use of the infrared lines in studying magnetospheric infall even in the earliest stages of star formation. Finally, we discuss constraints on the physical parameters and the possibility of using the emission lines as accretion rate indicators.