Planar H2O masers in star-forming regions
Planar H2O masers in star-forming regions
复制标题
恒星形成区域的平面 H2O 脉泽
DOI：
10.1086/171574
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发表时间：
1992
期刊：
影响因子：
--
通讯作者：
C. McKee
中科院分区：
文献类型：
--
作者：
M. Elitzur;D. Hollenbach;C. McKee
本文探讨了平面几何的冲击材料，这是关键属性，使高亮度温度的H2O脉泽在恒星形成区。的亮度温度，光束的角度，和脉泽光斑的大小被确定为薄的，饱和的平面脉泽的假设下，由于有序运动的速度变化是小的热或微湍流线宽相比。对于给定的一组物理参数，亮温度基本上完全由沿着视线的冲击平面中速度相干区域的长度决定。有效的长宽比（约5-50），发现与先前从观测到的亮度温度推断的值一致。
The paper examines the planar geometry of shocked material, which is the key property in enabling the high brightness temperatures of H2O masers in star-forming regions. The brightness temperature, beaming angle, and the maser spot size are determined for thin, saturated planar masers under the assumption that the velocity change across the maser due to ordered motions is small compared with the thermal or microturbulent line width. For a given set of physical parameters, the brightness temperature is essentially fully determined by the length of the velocity-coherent region in the shocked plane along the line of sight. Effective aspect ratios (about 5-50) are found that are in agreement with values previously inferred from observed brightness temperatures.