探究在伽马射线双星中的脉冲星风的物理现象

In this project, we will carry out a theoretical and observational investigation for multi-wavelength emissions from the gamma-ray binary, which radiate away their most radiation output in the gamma-ray bands, and produce the high-energy emissions that modulate along the orbital phase. There are tyo type of the gamma-ray binaries, that is which compact object (young pulsar or black hole)/ high-mass star (O or B-type star) system and millisecond pulsar/low mass Star (white dwarf or G-type star). The compact object of the high-mass gamma-ray binary has not been known, except for PSR B1259-63/LS2883, for which the compact object is radio pulsar. In this project, therefore, we will establish the binary model that can explain multi-wavelength observations for various high-mass gamma-ray binaries.. One long-standing mystery of the pulsar is the physics of pulsar wind. It has been believed that an energy conversion from the electromagnetic energy to the particle energy in the pulsar wind forms a cold-relativistic pulsar wind before termination shock. However, where and how this energy conversion process takes place is still in debate. The energy and the particle distribution in the cold-relativistic pulsar.are also unknown. The gamma-ray binary will offer a new approach to the physics of the pulsar wind.. In the proposed project, we will explore the possibility that the inverse-Compton scattering process of the cold-relativistic pulsar wind off the stellar photons generate the observable GeV emissions from the gamma-ray binary. It is believed that X-rays and TeV gamma-rays from the gamma-ray binaries are originated from the synchrotron radiation and inverse-Compton scattering process, respectively, of the pulsar wind particles reaccelerated at the shock. But, what mechanism causes the GeV emissions of the gamma-ray binaries is still in debate.. The next generation telescopes will enable us to start new science of the gamma-ray binaries. The Chinese hard X-ray telescope, HXMT, will measure the precise spectrum of the gamma-ray binary in hard X-ray and soft gamma-ray bands,which enables to discriminate our Inverse-Compton scattering model of the GeV emissions from other models. The new generation TeV telescope, CTA, by the international collaboration will discover >100 new gamma-ray binaries and will reveal how the spectrum extends in very high-energy gamma-ray bands. With establishing the theoretical model for multi-wavelength emissions, we will cooperate closely with new observations to advance in understanding for nature of the gamma-ray binary and pulsar wind.

我们将从理论和观察上研究伽马射线双星的多波段辐射，其中伽马射线双星由一个脉冲星和一个大质量星（一般为O或者B型星）或一个小质量星（白矮星或者G型星）组成。脉冲星的星风物理一直是一个长期的谜。人们相信在驻激波之前会由电磁能转换成粒子的能量而形成冷的相对论性的脉冲星星风。但是，这个能量是在哪里怎样转化的一直争论不休。这个冷的相对论性星风的能量和粒子分布也不知道。而伽马射线双星提供一个新的研究途径。在本项目中，我们将探究冷的相对论性星风通过逆康普顿散射伴星光子而产生GeV辐射的过程。人们相信X射线和TeV辐射分别来自激波重新加速的粒子的同步和逆康普顿散射。但是GeV辐射来源还依然存在争论。.下一代望远镜将让我们可以研究伽马射线双星的一些新的科学问题。中国的硬X射线调制望远镜HXMT可以测伽马射线双星从硬X射线到软伽马射线波段。这将用来区分我们的逆康普顿散射模型和其他的模型。

我们将从理论和观察上研究伽马射线双星的多波段辐射，其中伽马射线双星由一个脉冲星 和一个大质量星(一般为O或者B型星)或一个小质量星(白矮星或者G型星)组成。脉冲星的 星风物理一直是一个长期的谜。人们相信在驻激波之前会由电磁能转换成粒子的能量而形成冷 的相对论性的脉冲星星风。但是，这个能量是在哪里怎样转化的一直争论不休。这个冷的相对 论性星风的能量和粒子分布也不知道。而伽马射线双星提供一个新的研究途径。在本项目中， 我们将探究冷的相对论性星风通过逆康普顿散射伴星光子而产生GeV辐射的过程。人们相信X射 线和TeV辐射分别来自激波重新加速的粒子的同步和逆康普顿散射。但是GeV辐射来源还依然存 在争论。.下一代望远镜将让我们可以研究伽马射线双星的一些新的科学问题。中国的硬X射线调制 望远镜HXMT可以测伽马射线双星从硬X射线到软伽马射线波段。这将用来区分我们的逆康普顿 散射模型和其他的模型。