Modeling of the spatially resolved nonthermal emission from the Vela Jr. supernova remnant
Modeling of the spatially resolved nonthermal emission from the Vela Jr. supernova remnant
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Vela Jr. 超新星遗迹的空间分辨非热辐射建模
DOI：
10.1051/0004-6361/201832879
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发表时间：
2018
影响因子：
6.5
通讯作者：
M. Pohl
中科院分区：
文献类型：
--
作者：
I. Sushch;R. Brose;M. Pohl
小贝拉(RX J0852.0−4622）是少数已知的超新星遗迹（SNRs）之一，其壳层在从射电到极高能（>100 GeV; VHE）伽马射线的整个电磁波谱中都有解析。它的接近和大尺寸允许对源进行详细的空间分辨观测，使Vela Jr.用于研究SNR中粒子加速和发射机制的主要来源之一。高分辨率的X射线观测揭示了向残骸内部的光谱变陡。在这项研究中，我们的目标是一个自洽的Vela Jr辐射模型。这同时可以解释光源的宽带发射及其强度分布。我们结合高分辨率一维（1D）流体动力学模拟（使用冥王星代码）求解完整的粒子输运方程，然后计算来自残骸的辐射。在测试粒子状态下求解方程。我们测试两个模型的冲击下游的磁场分布：阻尼磁场，占强磁湍流下游的阻尼，和运输磁场。这两种情况都无法完全解释球对称下观察到的X射线光谱的径向依赖性。然而，我们表明，软化的光谱和X射线强度分布可以解释的假设下，发射增强内的圆锥。
Vela Jr. (RX J0852.0−4622) is one of just a few known supernova remnants (SNRs) with a resolved shell across the whole electromagnetic spectrum from radio to very-high-energy (>100 GeV; VHE) gamma-rays. Its proximity and large size allow for detailed spatially resolved observations of the source, making Vela Jr. one of the primary sources used for the study of particle acceleration and emission mechanisms in SNRs. High-resolution X-ray observations reveal a steepening of the spectrum toward the interior of the remnant. In this study we aim for a self-consistent radiation model of Vela Jr. which at the same time would explain the broadband emission from the source and its intensity distribution. We solve the full particle transport equation combined with the high-resolution one-dimensional (1D) hydrodynamic simulations (using Pluto code) and subsequently calculate the radiation from the remnant. The equations are solved in the test particle regime. We test two models for the magnetic field profile downstream of the shock: damped magnetic field, which accounts for the damping of strong magnetic turbulence downstream, and transported magnetic field. Neither of these scenarios can fully explain the observed radial dependence of the X-ray spectrum under spherical symmetry. We show, however, that the softening of the spectrum and the X-ray intensity profile can be explained under the assumption that the emission is enhanced within a cone.
DOI：
10.1111/j.1365-2966.2005.09227.x
发表时间：
2005-05
影响因子：
4.8
作者：
S. Gabici;P. Blasi;Giulia Vannoni
通讯作者：
S. Gabici;P. Blasi;Giulia Vannoni
DOI：
10.1086/588499
发表时间：
2008-03
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
S. Katsuda;H. Tsunemi;K. Mori
通讯作者：
S. Katsuda;H. Tsunemi;K. Mori
钱德拉对银河系超新星遗迹 Vela Jr. 的观测：发射同步加速器 X 射线的细丝的新样本
DOI：
--
发表时间：
2005
期刊：
Astrophysical Journal 632
影响因子：
--
作者：
Bamba;A.;YamazaKi;R.;Hiraga;J.
通讯作者：
J.