PROBING THE RADIAL TEMPERATURE STRUCTURE OF PROTOPLANETARY DISKS WITH HERSCHEL/HIFI
PROBING THE RADIAL TEMPERATURE STRUCTURE OF PROTOPLANETARY DISKS WITH HERSCHEL/HIFI
复制标题
用 Herschel/HIFI 探测原行星盘的径向温度结构
DOI：
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发表时间：
2013
期刊：
影响因子：
--
通讯作者：
Mpia
中科院分区：
文献类型：
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作者：
D. Fedele;S. Bruderer;E. V. Dishoeck;M. Hogerheijde;O. Panić;J. Brown;Th. Henning Mpe;L. Observatory;U. Cambridge;Cfa;Mpia
本文给出了HD 100546的Herschel/HIFI光谱观测结果，其中CO J = 10 ~（-9），CO J = 16 ~（-15），[C_（ii）]。我们的目标是解决线的速度分布，以解决发射区的过渡，并直接探测在磁盘中的暖气体的分布。的光谱显示双峰CO线轮廓集中在系统速度，符合磁盘的起源。J = 16-15的谱线轮廓比J = 10-9的谱线轮廓宽，而J = 10-9的谱线轮廓又比低J跃迁的谱线轮廓宽（6-5，3-2，用APEX观察到），因此显示出气体随半径的明显温度梯度。用幂律平盘模型同时拟合了CO谱线和CO转动阶梯，得到温度T_0 = 1100 ± 350 K（r_0 = 13 Au），温度径向梯度指数q = 0.85 ± 0.1。这表明，气体有一个陡峭的径向温度梯度比尘埃（平均qdust <0.5），提供了进一步的证据，气体和尘埃的热去耦的磁盘高度的CO线形成。[C ii]线剖面显示出较强的单峰剖面，与系统速度相比，红移了0.5 km s−1。我们得出结论，大部分[C ii]发射具有非盘起源（例如，残余包层或弥散云）。
Herschel/HIFI spectroscopic observations of CO J = 10–9, CO J = 16–15 and [C ii] toward HD 100546 are presented. The objective is to resolve the velocity profile of the lines to address the emitting region of the transitions and directly probe the distribution of warm gas in the disk. The spectra reveal double-peaked CO line profiles centered on the systemic velocity, consistent with a disk origin. The J = 16–15 line profile is broader than that of the J = 10–9 line, which in turn is broader than those of lower-J transitions (6–5, 3–2, observed with APEX), thus showing a clear temperature gradient of the gas with radius. A power-law flat disk model is used to fit the CO line profiles and the CO rotational ladder simultaneously, yielding a temperature of T0 = 1100 ± 350 K (at r0 = 13 AU) and an index of q = 0.85 ± 0.1 for the temperature radial gradient. This indicates that the gas has a steeper radial temperature gradient than the dust (mean qdust ∼ 0.5), providing further proof of the thermal decoupling of gas and dust at the disk heights where the CO lines form. The [C ii] line profile shows a strong single-peaked profile red-shifted by 0.5 km s−1 compared to the systemic velocity. We conclude that the bulk of the [C ii] emission has a non-disk origin (e.g., remnant envelope or diffuse cloud).
X 射线照射的原行星盘大气。
DOI：
10.1088/0004-637x/699/2/1639
发表时间：
2009
期刊：
The Astrophysical Journal
影响因子：
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作者：
Ercolano B
通讯作者：
Ercolano B