arXiv 0710.35262007-10-18astro-ph

大质量恒星系统中非热粒子谱的聚束效应

Clumping effects on non-thermal particle spectra in massive star systems

A. Reimer

备注：: 3 pages, 3 figures, to appear in the workshop proceedings "Clumping in Hot Star Winds", eds. W.-R. Hamann, A. Feldmeier and L. Oskinova

摘要：

观测证据表明，大质量恒星的恒星风是聚集在一起的。许多大质量恒星系统被称为非热粒子产生场所，正如它们在无线电波段的同步辐射所表明的那样。因此，它们也被认为是非热高能光子产生高达伽马射线能量的候选地点。目前的工作认为，预计在碰撞风系统的发射相对论粒子谱风结块的影响，建立了从热风粒子池通过扩散粒子加速，并考虑逆康普顿和同步加速器的损失。与均匀风相比，团簇风在团簇进入风碰撞区时，会引起发射粒子谱的通量变化。结果发现，与这种变化相关的光谱特征移动时间从低到高的能量带与任何两个光谱带之间的时间偏移依赖于团块大小，填充因子，和粒子能量的增益和损失的能量依赖性。

英文摘要：

Observational evidence exists that winds of massive stars are clumped. Many massive star systems are known as non-thermal particle production sites, as indicated by their synchrotron emission in the radio band. As a consequence they are also considered as candidate sites for non-thermal high-energy photon production up to gamma-ray energies. The present work considers the effects of wind clumpiness expected on the emitting relativistic particle spectrum in colliding wind systems, built up from the pool of thermal wind particles through diffusive particle acceleration, and taking into account inverse Compton and synchrotron losses. In comparison to a homogeneous wind, a clumpy wind causes flux variations of the emitting particle spectrum when the clump enters the wind collision region. It is found that the spectral features associated with this variability moves temporally from low to high energy bands with the time shift between any two spectral bands being dependent on clump size, filling factor, and the energy-dependence of particle energy gains and losses.

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英文摘要：

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