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

脉冲星风与恒星和星际物质相互作用的研究

• 批准号: 05640315
• 负责人: HOSHI Reiun
• 金额: $ 1.34万
• 依托单位: RIKKYO UNIVERSITY
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for General Scientific Research (C)
• 财政年份: 1993
• 资助国家: 日本
• 起止时间: 1993 至 1994
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/en/grant/KAKENHI-PROJECT-05640315/
• 关键词: pulsar wind; jet; supernova remnant; shock wave; particle acceleration; synchrotron radiation

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.

我们开发了模拟程序来研究脉冲星与恒星和星际事务的相互作用。当脉冲星从移动的中子恒星与星际物质碰撞时，预计将在脉冲星和星际大对风平衡的位置形成弓形冲击。当马赫数不那么高时，我们开发的仿真代码可以计算出弓震动的行为。现在，我们正在改进程序，以便即使马赫数很高，也可以稳定地进行模拟。我们研究了喷气机与超新星残留物的相互作用。我们得出了一种分析解决方案，以与射流与残留物发生碰撞后向前和反向冲击的传播。当应用于SS 433/W50系统时，我们发现我们的模型可以相对很好地解释系统的无线电和X射线形态。将我们的模型与SS 433/W 50系统的观察结果进行比较，我们可以确定射流和星际物质的密度以及射流速度为-0.01cm^<-3>，-0.001cm^3>，以及-2x10^9cms^9cms^< -1>，尊重。我们还发现，可以通过在反向冲击下加速的电子发射的同步子发射的X射线来解释。

项目成果

T. Ito: "Special-Purpose Computer HORN-1 for Reconstruction of Virtual Image in Three Dimensions" Comput. Phys. Commun.82. 104-110 (1994)

T. Ito：“用于三维虚拟图像重建的专用计算机 HORN-1”计算。

P. Y. Wang: "Higher Order Formulation of Absorbing Boundary Conditions for Finite-Difference Time-Domain Method" Electronics Letters. 29. 2018-2020 (1993)

P. Y. Wang：“时域有限差分法吸收边界条件的高阶公式”电子快报。

T. Yabe: "Holography Machine HORN-1 for Computer-Aided Retrieval of Virtual Three-Dimensional Image" Jpn. J. Appl. Phys.32. L1359-L1361 (1993)

T. Yabe：“用于计算机辅助检索虚拟三维图像的全息机 HORN-1”Jpn。

N. Shibazaki: "An Internal Friction Model for an Unusually Large Second Derivative of theDulsar Potation Rate" Proceedings of the 17th Texas Symposium on Relativistic Astrophysics. (in press). (1995)

N. Shibazaki：“Dulsar Potation Rate 的异常大二阶导数的内部摩擦模型”第 17 届德克萨斯州相对论天体物理学研讨会论文集。

N.Shibazaki: "An Internal Friciton Model for an Unusually Large Second Derivative of the Pulsar Rotation Rate" in Proceedings of the 17th Texas Symposium on Relativistic Astrophysics. (in press). (1995)

N.Shibazaki：“脉冲星自转速率异常大的二阶导数的内摩擦模型”，第 17 届德克萨斯相对论天体物理学研讨会论文集。