论文标题
3D相对论的MHD模拟
3D Relativistic MHD simulations of the gamma-ray binaries
论文作者
论文摘要
在伽马射线中，二进制二进制中心星是绕着产生强烈风的同伴。我们证明了“恒星风” - “脉冲风”相互作用的观察到的特性既取决于总风力推力比以及更微妙的几何因素：脉冲星的旋转的相对方向，轨道的平面，运动方向和瞬时视线。使用完全3D相对论的磁性水力学模拟，我们发现所得的内在形态可能显着轨道相依赖性：给定的系统可能会从尾部开放到向后闭合的形状变化。结果，未落下的脉冲星区域可以在四分之一的轨道上改变数量级。我们考虑了$γ-γ$的吸收，计算同步加速器（X射线）和反孔发射（GEV-TEV）的辐射图和合成光曲线。我们的建模光曲线与LS5039的相位依赖性观察到的光曲线一致。
In gamma-ray binaries neutron star is orbiting a companion that produces a strong stellar wind. We demonstrate that observed properties of "stellar wind"-"pulsar wind" interaction depend both on the overall wind thrust ratio, as well as more subtle geometrical factors: the relative direction of the pulsar's spin, the plane of the orbit, the direction of motion, and the instantaneous line of sight. Using fully 3D relativistic magnetohydrodynamical simulations we find that the resulting intrinsic morphologies can be significantly orbital phase-dependent: a given system may change from tailward-open to tailward-closed shapes. As a result, the region of unshocked pulsar wind can change by an order of magnitude over a quarter of the orbit. We calculate radiation maps and synthetic light curves for synchrotron (X-ray) and Inverse-Compton emission (GeV-TeV), taking into account $γ-γ$ absorption. Our modeled light curves are in agreement with the phase-dependent observed light curves of LS5039.
