Magnetic Compton-induced Pair Cascade Model for Gamma-Ray Pulsars
Magnetic Compton-induced Pair Cascade Model for Gamma-Ray Pulsars
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DOI：
10.1086/175736
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发表时间：
1995-06
期刊：
影响因子：
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通讯作者：
S. Sturner;C. Dermer;F. Michel
中科院分区：
文献类型：
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作者：
S. Sturner;C. Dermer;F. Michel
在脉冲星磁层中加速到相对论能量的电子将康普顿散射表面热发射和非热光学、紫外和软X射线发射到伽马射线能量，从而通过同步辐射和磁对产生启动对级联。这个过程被认为是从六个孤立的恒星中探测到的高能辐射的起源。我们构建了一个孤立脉冲星磁层极冠附近的磁康普顿散射的解析模型，并提出了散射光谱，电子能量损失率和光子光度的近似解析推导。用蒙特卡罗方法模拟了相对论电子通过回旋共振散射光子引起的对级联。为了简单起见，初级电子被假定为单能的，并且省略了非共振发射。假设磁轴和自旋轴之间的夹角φ（sub B）近似等于极冠角θ（sub pc），该模型可以产生双峰和宽单峰脉冲轮廓，并解释了从较老的恒星上观察到的更硬的伽马射线谱的趋势。
Electrons accelerated to relativistic energies in pulsar magnetospheres will Compton scatter surface thermal emission and nonthermal optical, UV, and soft X-ray emission to gamma-ray energies, thereby initiating a pair cascade through synchrotron radiation and magnetic pair production. This process is proposed as the origin of the high-energy radiation that has been detected from six isolated pulsars. We construct an analytic model of magnetic Compton scattering near the polar cap of isolated pulsar magnetospheres and present approximate analytic derivations for scattered spectra, electron energy-loss rates, and photon luminosities. A Monte Carlo simulation is used to model the pair cascade induced by relativistic electrons scattering photons through the cyclotron resonance. For simplicity, the primary electrons are assumed to be monoenergetic and the nonresonant emission is omitted. Assuming that the angle phi(sub B) between the magnetic and spin axes is approximately equal to the polar-cap angle theta(sub pc), this model can produce both double-peaked and broad single-peaked pulse profiles and account for the trend of harder gamma-ray spectra observed from older pulsars.