论文标题
偏心率在碰撞脉冲星的演变中的主要作用
The major role of eccentricity in the evolution of colliding pulsar-stellar winds
论文作者
论文摘要
拥有大量恒星和非精神脉冲星的二进制系统可能是强大的非热发射器。相对论的脉冲星风和非偏见的恒星流出沿轨道相互作用，从而产生从无线电到伽马射线辐射的超层压颗粒。为了正确地表征这些来源的物理，并且更好地了解它们对环境的排放和影响，需要对流出相互作用进行仔细的建模，跨越广泛的空间和时间尺度。完整的三维方法在计算上非常昂贵，但更简单的近似方法，虽然在半定量级别仍然是现实的。我们在这里介绍了使用准3维方案进行的计算结果，以计算跨越大小的区域中相互作用流的演变，最高为二进制的大小的一千倍。特别是，我们首次分析了不同偏心率在冲击流的大规模演变中的作用。我们发现，偏心率越高，流动的表现越近，它的表现就越像一个侧面流出，这对于偏心值$ \ gtrsim 0.75 $变得相当准确。这些模拟还公布了脉冲星和恒星风在网格中完全混合到低偏心系统的网格中，在大尺度上比在高度偏心的系统中表现出更大的随机行为。
Binary systems that host a massive star and a non-accreting pulsar can be powerful non-thermal emitters. The relativistic pulsar wind and the non-relativistic stellar outflows interact along the orbit, producing ultrarelativistic particles that radiate from radio to gamma rays. To properly characterize the physics of these sources, and better understand their emission and impact on the environment, careful modelling of the outflow interactions, spanning a broad range of spatial and temporal scales, is needed. Full 3-dimensional approaches are very computationally expensive, but simpler approximate approaches, while still realistic at the semi-quantitative level, are available. We present here the results of calculations done with a quasi 3-dimensional scheme to compute the evolution of the interacting flows in a region spanning in size up to a thousand times the size of the binary. In particular, we analyze for the first time the role of different eccentricities in the large scale evolution of the shocked flows. We find that the higher the eccentricity, the closer the flows behave like a one-side outflow, which becomes rather collimated for eccentricity values $\gtrsim 0.75$. The simulations also unveil that the pulsar and the stellar winds become fully mixed within the grid for low eccentricity systems, presenting a more stochastic behavior at large scales than in the highly eccentric systems.
