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首页> 外文期刊>The Astrophysical journal >DUST EMISSION FROM PROTOSTARS: THE DISK AND ENVELOPE OF HH 24 MMS
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DUST EMISSION FROM PROTOSTARS: THE DISK AND ENVELOPE OF HH 24 MMS

机译：原恒星产生的粉尘：HH 24 MMS的磁盘和外壳

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摘要

High-resolution imaging of the protostar HH 24 MMS at wavelengths of 7 mm and 3.4 mm shows the dust emission to originate from two components: an unresolved disk and an extended envelope. The envelope is an order of magnitude more massive than the disk, suggesting that HH 24 MMS is very young, since the fraction of circumstellar material in an extended component probably decreases with the age of the forming star. For the disk, the frequency dependence of the dust mass opacity coefficient, β, is 0.68 ± 0.12, significantly lower than the interstellar medium value of 2. In the envelope β is less well constrained but must lie in the range 0 to 1.9. Emission from the disk dominates at wavelengths longer than 3 mm, but the far-infrared emission is relatively weak. This suggests that the envelope is optically thick at wavelengths as short as 60 μm and obscures the disk.
机译：Protostar HH 24 MMS在7毫米和3.4毫米波长处的高分辨率成像显示，粉尘排放源于两个组件：未分辨的磁盘和扩展的外壳。包层比盘的质量大一个数量级，这表明HH 24 MMS非常年轻，因为扩展分量中的恒星物质比例可能会随着形成恒星的年龄而减少。对于圆盘，尘埃质量不透明度系数β的频率依赖性为0.68±0.12，远低于星际介质值2。在包络中，β的约束性较弱，但必须在0到1.9的范围内。从磁盘发出的光在大于3 mm的波长处占主导地位，但远红外线的发出相对较弱。这表明包膜在短至60μm的波长处光学上很厚，并掩盖了光盘。

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