Nonthermal emission from the reverse shock of the youngest Galactic supernova remnant G1.9+0.3
Nonthermal emission from the reverse shock of the youngest Galactic supernova remnant G1.9+0.3
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最年轻的银河系超新星遗迹 G1.9 反向激波的非热发射 0.3
DOI：
10.1051/0004-6361/201834430
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发表时间：
2019
影响因子：
6.5
通讯作者：
R. Lin
中科院分区：
文献类型：
--
作者：
R. Brose;I. Sushch;M. Pohl;K. Luken;M. Filipović;R. Lin
上下文最年轻的银河系超新星遗迹G1.9+0.3是下一代伽马射线天文台的一个有趣的目标。到目前为止，残骸只在无线电和X射线波段被探测到，但它的年轻年龄为100年，推断的冲击速度为14000 km s-1，这使它成为一个有效的粒子加速器。
目标。我们的目标是模拟观测到的无线电和X射线光谱以及残骸的形态。同时，我们的目标是估计从源的伽马射线通量，并评估其检测与未来的伽马射线实验的前景。
方法.我们进行了球对称的一维模拟与RATPaC代码，在其中，我们同时解决宇宙射线的输运方程，磁湍流的输运方程，和气体流动的流体动力学方程。分别计算的粒子分布加速在前进和反向冲击，然后被用来计算光谱的同步，逆康普顿，和π衰变辐射的来源。
结果G1.9+0.3的发射可以在测试粒子限值内自洽地解释。我们发现X射线通量主要来自前向激波的辐射，而射电辐射主要来自反向激波附近，这使得G1.9+0.3成为第一个从反向激波中探测到非热辐射的遗迹。来自G1.9+0.3的极高能伽马射线辐射通量预计接近切伦科夫望远镜阵列的灵敏度阈值。由于大尺度湍流的时间有限，粒子的最大能量被限制在100 TeV以下，因此G1.9+0.3不是PeVatron。
Context. The youngest Galactic supernova remnant G1.9+0.3 is an interesting target for next-generation gamma-ray observatories. So far, the remnant is only detected in the radio and the X-ray bands, but its young age of ≈100 yr and inferred shock speed of ≈14 000 km s−1 could make it an efficient particle accelerator.
Aims. We aim to model the observed radio and X-ray spectra together with the morphology of the remnant. At the same time, we aim to estimate the gamma-ray flux from the source and evaluate the prospects of its detection with future gamma-ray experiments.
Methods. We performed spherical symmetric 1D simulations with the RATPaC code, in which we simultaneously solved the transport equation for cosmic rays, the transport equation for magnetic turbulence, and the hydro-dynamical equations for the gas flow. Separately computed distributions of the particles accelerated at the forward and the reverse shock were then used to calculate the spectra of synchrotron, inverse Compton, and pion-decay radiation from the source.
Results. The emission from G1.9+0.3 can be self-consistently explained within the test-particle limit. We find that the X-ray flux is dominated by emission from the forward shock while most of the radio emission originates near the reverse shock, which makes G1.9+0.3 the first remnant with nonthermal radiation detected from the reverse shock. The flux of very-high-energy gamma-ray emission from G1.9+0.3 is expected to be close to the sensitivity threshold of the Cherenkov Telescope Array. The limited time available to grow large-scale turbulence limits the maximum energy of particles to values below 100 TeV, hence G1.9+0.3 is not a PeVatron.
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