与伽马射线超新星遗迹RCW 103相关的分子气体和原子气体
Molecular and Atomic Gas Associated with the Gamma Ray Supernova Remnant RCW 103
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中文总结 AI 辅助
本研究利用多种射电望远镜数据，分析伽马射线超新星遗迹RCW 103的气体分布，发现其CO气体云膨胀速度约7.5 km s$^{-1}$，估算的宇宙射线质子能量偏低，或因激波能量转化为热能导致加速效率降低。
中文摘要 AI 辅助
本研究利用莫普拉望远镜的$^{12}$CO($J$=1-0)、阿塔卡马大型毫米/亚毫米波阵列的$^{13}$CO($J$=1-0)，以及澳大利亚望远镜致密阵列与帕克斯望远镜的HI数据，对与伽马射线超新星遗迹（SNR）RCW 103相关的星际分子气体和原子气体展开研究。我们发现，速度范围在-58.7至-43.5 km s$^{-1}$的CO气体云与RCW 103的X射线壳层存在清晰的空间对应关系，尤其从西北区域延伸至东南区域。CO发射的位置-速度图揭示了气体的膨胀运动，膨胀速度约为$\triangle V \backsim 7.5$ km s$^{-1}$，该运动可能由前身系统产生的激波和/或恒星风所引发。我们采用约810 cm$^{-3}$的星际质子总密度，估算得到宇宙射线质子总能量约为$3.0^{+1.1}_{-0.6} \times 10^{47}$ erg，该数值比其他年龄相当的伽马射线发射超新星遗迹的推断值低一个数量级以上。鉴于RCW 103内部仍存在大量致密气体，且该区域以热X射线发射为主，我们的结果可能表明，激波能量的很大一部分已通过气体加热转化为热能，从而降低了宇宙射线加速的效率。
英文摘要
We present a study of the interstellar molecular and atomic gas associated with the gamma-ray supernova remnant (SNR) RCW 103 using the Mopra $^{12}$CO($J$ = 1-0), Atacama Large Millimeter/submillimeter Array $^{13}$CO($J$ = 1-0), and the Australia Telescope Compact Array & Parkes HI data. We find that CO clouds in the velocity range from $-58.7$ to $-43.5$ km s$^{-1}$ show a clear spatial correspondence with the X-ray shell of RCW 103, particularly extending from the northwestern to the southeastern regions. The position-velocity diagram of the CO emission reveals an expanding gas motion with an expansion velocity of $ΔV \sim$$7.5$ km s$^{-1}$, which may have been produced by shock waves and/or stellar winds from the progenitor system. We estimate the total cosmic-ray proton energy to be $\sim$$3.0^{+1.1}_{-0.6} \times 10^{47}$ erg, adopting a total interstellar proton density of $\sim$$810$ cm$^{-3}$. This value is more than an order of magnitude lower than those inferred for other gamma-ray emitting SNRs of comparable age. Given that a substantial amount of dense gas remains within the interior of RCW 103, where thermal X-ray emission is dominant, our results possibly suggest that a significant fraction of the shock energy may have been converted into thermal energy via gas heating, thereby reducing the efficiency of cosmic-ray acceleration.
