天鹅座环Shock Wave中的碳、氦和质子动力学温度
Carbon, Helium and Proton Kinetic Temperatures in a Cygnus Loop Shock Wave
摘要：
对SN 1006的观测表明，在快速超新星遗迹激波后面的等离子体中的离子和电子远离平衡，电子温度远低于质子温度，离子温度与离子质量近似成正比。另一方面，在天鹅座环的~360 km/s冲击波中，电子和离子温度大致相等，并且有证据表明氧动力学温度与质子温度相差不远。在本文中，我们报告的观测He II λ 1640线和C IV λ 1550双峰在360公里/秒的冲击在天鹅座圈。虽然最佳拟合动力学温度略高于质子温度，但He和C的温度与质子温度一致，上限为质量比例温度的0.5和0.3倍，这意味着在这种无碰撞冲击中有效的热平衡。氦和氢的平衡影响了从H α线轮廓确定的质子温度与冲击速度之间的转换，并且这里发现的有效平衡将冲击速度估计值和Medina等人（2014）的天鹅座圈的距离估计值降低到约800 pc。
英文摘要：
Observations of SN1006 have shown that ions and electrons in the plasma behind fast supernova remnant shock waves are far from equilibrium, with the electron temperature much lower than the proton temperature and ion temperatures approximately proportional to ion mass. In the ~360 km/s shock waves of the Cygnus Loop, on the other hand, electron and ion temperatures are roughly equal, and there is evidence that the oxygen kinetic temperature is not far from the proton temperature. In this paper we report observations of the He II lambda 1640 line and the C IV lambda 1550 doublet in a 360 km/s shock in the Cygnus Loop. While the best fit kinetic temperatures are somewhat higher than the proton temperature, the temperatures of He and C are consistent with the proton temperature and the upper limits are 0.5 and 0.3 times the mass-proportional temperatures, implying efficient thermal equilibration in this collisionless shock. The equilibration of helium and hydrogen affects the conversion between proton temperatures determined from H alpha line profiles and shock speeds, and that the efficient equilibration found here reduces the shock speed estimates and the distance estimate to the Cygnus Loop of Medina et al. (2014) to about 800 pc.
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