Studies on the Interaction of a Pulsar Wind with Stellar and Interstellar Matters

我们已经开发了模拟程序来研究脉冲星风与恒星和星际物质的相互作用。当从运动的中子星喷出的脉冲星风与星际物质碰撞时，弓形激波预计将在脉冲星和星际物质风的冲压平衡的地方形成。我们开发的模拟程序可以在马赫数不是很高的情况下稳定地计算弓激波的行为。我们现在正在改进程序，以便即使在马赫数相当高的情况下也能稳定地进行模拟。我们已经研究了喷流与超新星遗迹的相互作用。我们推导了喷流与残留物碰撞后正向激波和反向激波传播的解析解。当应用于SS433/W50系统时，我们发现我们的模型能较好地解释该系统的射电和X射线形态。将我们的模型与SS433/W50系统的观测结果相比较，我们可以确定喷流密度和星际物质密度，喷流速度分别为-0.01 cm^-3；-0.001 cm^-3&gt；和-2×10^9 cm^-1&gt；我们还发现，从波瓣发出的X射线可以用反向激波加速的电子的同步辐射来解释。

We have developed simulation programs to study the interaction of a pulsar wind with stellar and interstellar matters. When the pulsar wind ejected from a moving neutron star collides with the interstellar matter, the bow shock is expected to be formed at the place where the ram pressures of pulsar and interstellar matter winds balance. Our simulation code developed can calculate the behavior of the bow shock stably when the Mach number is not so high. We are now improving the programs so as to conduct simulations stably even when the Mach number is cosiderably high.We have studied the interaction of a jet with a supernova remnant. We derived an analytical solution to the propagation of forward and reverse shocks after the jet collides with the remnant. When applied to the SS 433/W50 system, we found that our model can explain the radio and X-ray morphology of the system relatively well. Comparing our model with the observations of the SS 433/W 50 system, we could determine the densities of jet and interstellar matters and a jet velocity to be - 0.01cm^<-3>, - 0.001cm^<-3>, and - 2x10^9cms^<-1>, respectivery. We also found that X-rays from the lobes can be explained in terms of synchrotron emission by electrons accelerated at the reverse shock.