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首页> 外文期刊>Astronomy and astrophysics >A young supernova remnant illuminating nearby molecular clouds with cosmic rays
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A young supernova remnant illuminating nearby molecular clouds with cosmic rays

机译：一颗年轻的超新星残余物用宇宙射线照亮了附近的分子云

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The supernova remnant (SNR) HESS J1731-347 displays strong nonthermal TeV γ -ray and X-ray emission, thus the object is presently accelerating particles to very high energies. A distinctive feature of this young SNR is the nearby ( ~30 pc in projection) extended source HESS J1729-345, which is currently unidentified but is in spatial projection coinciding with known molecular clouds (MC). We model the SNR evolution to explore whether the TeV emission from HESS J1729-345 can be explained as emission from runaway hadronic cosmic rays (CRs) that are illuminating these MCs. The observational data of HESS J1729-345 and HESS J1731-347 can be reproduced using core-collapse SN models for HESS J1731-347. Starting with different progenitor stars and their presupernova environment, we model potential SNR evolution histories along with the CR acceleration in the SNR and the diffusion of the CRs. A simplified three-dimensional structure of the MCs is introduced based on data of that region, adopting a distance of 3.2 kpc to the source. A Monte Carlo based diffusion model for the escaping CRs is developed to deal with the inhomogeneous environment. The fast SNR forward shock speed, as implied from the X-ray data, can easily be explained when employing scenarios with progenitor star masses between 20 M _(⊙) and 25 M _(⊙) , where the SNR shock is still expanding inside the main-sequence (MS) bubble at present time. The TeV spectrum of HESS J1729-345 is satisfactorily fitted by the emission from the highest energy CRs that have escaped the SNR, using a standard Galactic CR diffusion coefficient in the interclump medium. The TeV image of HESS J1729-345 can be explained with a reasonable three-dimensional structure of MCs. The TeV emission from the SNR itself is dominated by leptonic emission in this model. We also explore scenarios where the shock is starting to encounter the dense MS progenitor wind bubble shell. The escaping hadronic CR hypothesis for the γ -ray emission of HESS J1729-345 can still hold,but even in this case our model cannot easily account for the TeV emission from HESS J1731-347 in a hadronic scenario.
机译：超新星残留物（HESS J1731-347）表现出很强的非热TeVγ射线和X射线发射，因此该物体目前正在将粒子加速到非常高的能量。这种年轻的SNR的一个显着特征是附近（投影时约为30 pc）扩展源HESS J1729-345，目前尚不清楚，但其空间投影与已知的分子云（MC）一致。我们对SNR演化进行建模，以探讨HESS J1729-345的TeV发射是否可以解释为照亮这些MC的失控强子宇宙射线（CR）的发射。 HESS J1729-345和HESS J1731-347的观测数据可以使用HESS J1731-347的核心塌陷SN模型再现。从不同的祖先恒星及其超新星前环境开始，我们对潜在的SNR演化历史以及SNR中的CR加速和CR的扩散进行建模。根据该区域的数据介绍了MC的简化三维结构，其到源的距离为3.2 kpc。针对逃逸的CR，开发了基于蒙特卡罗的扩散模型。 X射线数据所暗示的快速SNR前向震荡速度，在采用祖星质量在20 M _（⊙）和25 M _（⊙）之间且SNR震荡仍在内部扩展的场景时，很容易解释。当前的主序列（MS）气泡。 HESS J1729-345的TeV光谱可以通过杂散介质中的标准银河CR扩散系数，通过逃脱SNR的最高能量CR的发射来令人满意地拟合。 HESS J1729-345的TeV图像可以用合理的MC三维结构来解释。在此模型中，SNR本身的TeV发射主要是轻子发射。我们还探讨了震动开始遇到密集的MS祖先风壳的情况。 HESS J1729-345的γ射线发射的逃逸强子CR假设仍然成立，但是即使在这种情况下，我们的模型也无法轻松地解释强子情形下HESS J1731-347的TeV发射。

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