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首页> 外文期刊>The Astrophysical journal >NONTHERMAL EMISSION FROM A SUPERNOVA REMNANT IN A MOLECULAR CLOUD
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NONTHERMAL EMISSION FROM A SUPERNOVA REMNANT IN A MOLECULAR CLOUD

机译：分子云中超新星遗留物的非热辐射

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摘要

In evolved supernova remnants (SNRs) interacting with molecular clouds, a highly inhomogeneous structure consisting of a forward shock of moderate Mach number, a cooling layer, a dense radiative shell, and an interior region filled with hot tenuous plasma is expected. We present a model of non-thermal electron injection, acceleration, and propagation in that environment and find that these SNRs are efficient electron accelerators and sources of hard X-ray and γ-ray emission. A forward shock of velocity v_s approx> 100 km s~(-1) with an ionized precursor propagating into the molecular cloud accompanied by magnetohydrodynamic turbulence provides a spatially inhomogeneous distribution of nonthermal electrons. The energy spectrum of the nonthermal electrons is shaped by the joint action of first- and second-order Fermi acceleration in a turbulent plasma with substantial Coulomb losses. Bremsstrahlung, synchrotron, and inverse Compton radiation of the nonthermal electrons produce multiwavelength photon spectra in quantitative agreement with the radio and hard emission from IC 443 observed by ASCA and EGRET. We distinguish interclump shock wave emission from molecular clump shock wave emission; particles reach higher energies in the interclump shock, and that is the likely source of γ-ray emission and radio synchrotron emission. Spatially resolved X-ray and γ-ray spectra from the SNRs IC 443, W44, and 3C 391 as might be observed with BeppoSAX, Chandra XRO, XMM, International Gamma-Ray Astrophysical Laboratory, and Gamma-Ray Large Area Space Telescope would distinguish the contribution of the energetic lepton component to the γ-rays observed by EGRET, constraining the cosmic-ray nuclear component spectra in these SNRs. These data would provide a valuable tool for studying the complex structure of molecular clouds where SNR radiative shocks interact with dense molecular clumps.
机译：在与分子云相互作用的演化超新星残迹（SNR）中，期望一种高度不均匀的结构，该结构由中等马赫数的正向激波，冷却层，致密的辐射壳以及充满热微弱等离子体的内部区域组成。我们提出了在该环境中非热电子注入，加速和传播的模型，并发现这些SNR是有效的电子加速器和硬X射线和γ射线的发射源。速度v_s约> 100 km s〜（-1）的前向冲击，伴随着磁流体动力学湍流的电离前体传播进入分子云，提供了非热电子在空间上的不均匀分布。非热电子的能谱是通过湍流等离子体中一阶和二阶费米加速度的联合作用而成形的，该等离子体具有明显的库仑损耗。非热电子的致辐射，同步加速器和康普顿逆辐射产生多波长光子光谱，与ASCA和EGRET观测到的IC 443的无线电和硬发射在数量上一致。我们将分子团簇冲击波发射与分子团簇冲击波发射区分开;粒子在丛集激波中达到更高的能量，这可能是γ射线发射和无线电同步加速器发射的来源。 BeppoSAX，Chandra XRO，XMM，国际伽玛射线天体物理学实验室和伽玛射线大面积空间望远镜可能会观察到SNRs IC 443，W44和3C 391产生的空间分辨X射线和γ射线光谱高能轻子成分对EGRET观测到的γ射线的贡献，从而限制了这些SNR中的宇宙射线核成分光谱。这些数据将为研究SNR辐射冲击与密集分子团簇相互作用的分子云的复杂结构提供有价值的工具。

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