论文标题
重新审视Cygnus X-3上的主要和次要耀斑
Major and Minor Flares on Cygnus X-3 Revisited
论文作者
论文摘要
从Cygnus X-3观察到的CM波长的强烈耀斑已有很多年。这种活跃的高质量X射线二进制于重大爆发前还具有淬火时期，并且在几百个MJY的水平上有较小的耀斑。在本文中，我们表明，较小的耀斑的上升时间和持续时间要短得多，表明同步辐射材料的膨胀速度比强耀斑更快。它们也看起来更靠近二进制，而大型耀斑形成了更发达的喷气机。物理条件的计算表明，较小的外部爆炸具有较低的最小功率，但比主要耀斑具有更大的磁场和能量密度。在进行重大耀斑时，可能会发生较小的耀斑，这表明它们之间的间接耦合。次要耀斑的光谱演化可以通过扩展的同步加速器源或冲击模型来解释。探索了SS433中有一个亮区的可能性。
Intense flares at cm-wavelengths reaching levels of tens of Jy have been observed from Cygnus X-3 for many years. This active high mass X-ray binary also has periods of quenching before major outbursts, and has minor flares at levels of a few hundred mJy. In this paper we show that the minor flares have much shorter rise times and durations suggesting more rapid expansion of the synchrotron radiation emitting material than in the strong flares. They also appear closer to the binary, whereas the large flares form a more developed jet. Calculations of physical conditions show that the minor out-bursts have lower minimum power but have larger magnetic fields and energy densities than the major flares. Minor flares can occur while a major flare is in progress, suggesting an indirect coupling between them. The spectral evolution of the minor flares can be explained by either an expanding synchrotron source or a shock model. The possibility that there is a brightening zone as in SS433 is explored.
