PSR B1259-63 is a gamma-ray binary system hosting a radio pulsar orbiting around a O9.5Ve star, LS 2883, with a period of ~3.4 years. The interaction of the pulsar wind with the LS 2883 outflow leads to unpulsed broad band emission in the radio, X-rays, GeV and TeV domains. While the radio, X-ray and TeV light curves show rather similar behaviour, the GeV light curve appears very different with a huge outburst about a month after a periastron. The energy release during this outburst seems to significantly exceed the spin down luminosity of the pulsar and the GeV light curve and energy release varies from one orbit to the next. In this paper we present for the first time the results of optical observations of the system in 2017, and also reanalyze the available X-ray and GeV data. We present a new model in which the GeV data are explained as a combination of the bremsstrahlung and inverse Compton emission from the unshocked and weakly shocked electrons of the pulsar wind. The X-ray and TeV emission is produced by synchrotron and inverse Compton emission of energetic electrons accelerated on a strong shock arising due to stellar/pulsar winds collision. The brightness of the GeV flare is explained in our model as a beaming effect of the energy released in a cone oriented, during the time of flare, in the direction of the observer.

中文翻译：

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从 2017 年星周通道对双星系统 PSR B1259-63/LS 2883 中 GeV 耀斑起源的新见解

PSR B1259-63 是一个伽马射线双星系统，拥有一颗射电脉冲星，围绕一颗 O9.5Ve 恒星 LS 2883 运行，周期约为 3.4 年。脉冲星风与 LS 2883 外流的相互作用导致无线电、X 射线、GeV 和 TeV 域中的非脉冲宽带发射。虽然射电、X 射线和 TeV 光变曲线表现出相当相似的行为，但 GeV 光变曲线看起来非常不同，在近天体大约一个月后发生了巨大的爆发。这次爆发期间的能量释放似乎大大超过了脉冲星的自旋下降光度，并且 GeV 光变曲线和能量释放从一个轨道到另一个轨道都不同。在本文中，我们首次展示了该系统在 2017 年的光学观测结果，并重新分析了可用的 X 射线和 GeV 数据。我们提出了一个新模型，其中 GeV 数据被解释为来自脉冲星风未受冲击和弱冲击电子的韧致辐射和逆康普顿发射的组合。X 射线和 TeV 发射是由同步加速器和高能电子的逆康普顿发射产生的，这些高能电子在恒星/脉冲星风碰撞引起的强烈冲击下加速。GeV 耀斑的亮度在我们的模型中被解释为在耀斑期间朝向观察者方向的锥体中释放的能量的光束效应。X 射线和 TeV 发射是由同步加速器和高能电子的逆康普顿发射产生的，这些高能电子在恒星/脉冲星风碰撞引起的强烈冲击下加速。GeV 耀斑的亮度在我们的模型中被解释为在耀斑期间朝向观察者方向的锥体中释放的能量的光束效应。X 射线和 TeV 发射是由同步加速器和高能电子的逆康普顿发射产生的，这些高能电子在恒星/脉冲星风碰撞引起的强烈冲击下加速。GeV 耀斑的亮度在我们的模型中被解释为在耀斑期间朝向观察者方向的锥体中释放的能量的光束效应。