Three-dimensional magnetohydrodynamic studies of the non-thermal X-ray morphologies of SN 1006
Three-dimensional magnetohydrodynamic studies of the non-thermal X-ray morphologies of SN 1006
复制标题
SN 1006非热X射线形貌的三维磁流体动力学研究
DOI：
10.1051/0004-6361/201424857
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发表时间：
2015-07
影响因子：
6.5
通讯作者：
Zhang Li
中科院分区：
文献类型：
--
作者：
Yu Huan;Fang Jun;Zhang Peng Fei;Zhang Li
上下文。对超新星遗迹SN 1006的同步辐射观测表明，该遗迹具有双侧形态，其主要特征是沿遗迹边界有两个相对的明亮分支，具有节和丝状结构。形貌不是严格的圆形，在残体边缘有扰动和凸起。例如，根据无线电和x射线观测到的形态，一个大的凸起位于东北（东北）翼，几个相对较小的凸起位于西南（西南）翼。目标。通过三维磁流体力学模拟研究了SN 1006非热x射线的非对称形貌的产生。此外，可以通过将所得同步加速器形态与检测到的硬x射线发射图像进行比较来研究周围物质的密度分布。方法。首先，这个残余物被模拟成在湍流等离子体中演化的超新星爆炸，湍流的振幅相对较小。在该模型中，使用了几个密度低于背景等离子体的球形空腔来重现在明亮的分支处检测到的凸起。其次，采用较低的绝热指数研究了有效宇宙射线加速对残余物形貌的影响。结果。如果假设激波时电子在扩散激波加速过程中的注入效率遵循准平行情景，则在非修饰情景下，利用背景介质中的空腔一般可以再现SN 1006在明亮的NE和SW区域具有凸起的硬x射线形态。此外，在均匀介质中形成的残余的较低绝热指数为1.2的修正情况下，在信噪比边界上可以产生相对较小的扩展，这是由流体动力不稳定性导致的，而这反过来又超过了正向激波。结论。在较小振幅的湍流介质中传播的信噪比比在均匀环境中进化的信噪比能更好地再现残余的结状和丝状形态；此外，东北翼上的大碰撞可以解释为一个密度较低的区域的结果，该区域的半径约为2.5%，密度约为一般环境介质的0.4倍，被激波锋面扫过，而西南翼上其他较小的突起既可以在激波扫过的较小密度区域中再现，也可以解释为不稳定指有效超过正向激波时宇宙射线有效加速情景中的突起。
Context. The observations of the synchrotron emission from the supernova remnant (SNR) SN 1006 indicate a bilateral morphology, which is mainly characterized by two opposite bright limbs with knots and filaments along the boundary of the remnant. The morphology is not strictly circular with disturbances and bumps at the rim of the remnant. For instance, one big bump is located on the northeastern (NE) limb and several relatively small ones on the southwestern (SW) limb on the detected morphologies from the observations in the radio and X-rays. Aims. The generation of the asymmetric morphology of non-thermal X-rays for SN 1006 is investigated through three-dimensional (3D) magnetohydrodynamic simulations. Moreover, the density distribution of the ambient material can be investigated by comparing the resulting synchrotron morphology with the detected images of the hard X-ray emission. Methods. First, the remnant was simulated as a supernova explosion evolved in a turbulent plasma with a relatively small amplitude for the turbulence. In the model, several spherical cavities with lower densities compared with the background plasma were employed to reproduce the detected bumps at the bright limbs. Second, the effect of the modification on the morphology of the remnant due to efficient cosmic ray acceleration was investigated by adopting a lower adiabatic index. Results. If we assume that the injection efficiency of electrons into the diffusive shock acceleration process at the shock follows the quasi-parallel scenario, the hard X-ray morphology of SN 1006 with bumps in the bright NE and SW regions can be generally reproduced by employing cavities in the background medium in the non-modification scenario. Furthermore, in the modification case with a lower adiabatic index of 1.2 for the remnant evolved in a uniform medium, bubbles can be produced with relatively small extensions on the SNR boundary that result from the hydrodynamical instabilities that in turn overtake the forward shock. Conclusions. The SNR propagating in the turbulent medium with a relatively small amplitude can reproduce the knotty and filamentary morphology of the remnant better than what evolved in the uniform environment; moreover, the big bump on the NE limb can be explained as the result of a lower-density region, which has a radius of about 2.5 pc and a density of about 0.4 times of the general ambient medium, swept by the shock front, and the other smaller ones on the SW limb can either be reproduced with smaller regions with lower densities swept by the shock or be explained as the protrusions in the scenario of the efficient cosmic ray acceleration when the instability fingers effectively overtake the forward shock.
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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：
10.1111/j.1365-2966.2010.17125.x
发表时间：
2010-06
影响因子：
4.8
作者：
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通讯作者：
E. Schneiter;P. Vel'azquez;E. Reynoso;F. Colle
DOI：
10.1086/116748
发表时间：
1993-10
期刊：
The Astronomical Journal
影响因子：
--
作者：
D. Moffett;W. Goss;S. Reynolds
通讯作者：
D. Moffett;W. Goss;S. Reynolds
影响因子：
6.5
作者：
R. Rothenflug;J. Ballet;G. Dubner;E. Giacani;A. Decourchelle;P. Ferrando
通讯作者：
R. Rothenflug;J. Ballet;G. Dubner;E. Giacani;A. Decourchelle;P. Ferrando
DOI：
10.1088/2041-8205/735/1/l21
发表时间：
2011-04
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
C. Rakowski;J. Laming;U. Hwang;K. Eriksen;P. Ghavamian;J. Hughes
通讯作者：
C. Rakowski;J. Laming;U. Hwang;K. Eriksen;P. Ghavamian;J. Hughes