Model of radio emission from spherically symmetric pulsar wind nebulae
Model of radio emission from spherically symmetric pulsar wind nebulae
复制标题
球对称脉冲星风星云射电发射模型
DOI：
10.1017/s1743921312024696
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发表时间：
2013
期刊：
影响因子：
--
通讯作者：
Shuta J. Tanaka
中科院分区：
文献类型：
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作者：
Ambo E.;Suga T.;Nedate K.;中島沙恵子;中島沙恵子;中島沙恵子;中島沙恵子;中島沙恵子;田中周太;Shuta J. Tanaka
考虑到观测到的空间结构，我们研究了脉冲星风星云（PWNe）的无线电发射。我们假设球对称的PWN，和模型的磁场和粒子的能量分布的演变。我们不考虑粒子的同步辐射冷却，而考虑绝热冷却，因为我们最感兴趣的是PWNe的射电辐射。该模型被应用到蟹状星云，并成功地复制观察到的空间集成频谱无线电与一个单一的幂律注入。相反，在我们以前的工作（一个单区模型）中，蟹状星云的综合光谱是通过粒子的幂律注入而被打破的。然而，无线电的空间结构与观测结果不一致，我们需要一个径向速度分布，这与Kennel & Coroniti的模型非常不同。进一步研究PWNe的空间结构对于理解年轻PWNe射电辐射的起源具有重要意义。
We study radio emission from pulsar wind nebulae (PWNe) considering the observed spatial structure. We assume spherical symmetry of the PWN, and model the evolution of the magnetic field and the particle energy distribution. We do not consider the synchrotron cooling of particles but consider the adiabatic cooling, because we are mostly interested in the radio emission from PWNe. The model is applied to the Crab Nebula and succeeds to reproduce the observed spatially integrated spectrum in radio with a single power-law injection. In our previous work (a one-zone model), in contrast, the integrated spectrum of the Crab Nebula is reproduced by a broken power-law injection of particles. However, the spatial structure in radio is inconsistent with observations and we need a radial velocity profile which is very different from the model by Kennel & Coroniti. Further studies of the spatial structure of PWNe are important to understand the origin of the radio emission from young PWNe.