HXMT研究脉冲星的硬X射线/软γ射线辐射

我们对脉冲星的硬X射线/软伽马射线发射进行理论和观测研究。 与GeV伽马射线脉冲星（200个源）相比，在硬X射线/软伽马射线（> 10keV）处看到的脉冲星数量仍然很少（约15个源）。 随着能带范围的广泛覆盖，HXMT非常适合研究脉冲星的硬X射线/软伽马射线发射，并为脉冲星磁层发生的物理过程提供新的见解。 在提议的项目中，为了HXMT定期收集这些数据我们深入研究了Crab脉冲星和PSR B1509-58的硬X射线/软伽马射线辐射。 我们将模拟X射线/伽玛射线光谱和光线曲线对观察几何形状的依赖关系，并且会讨论这个模型是否可以解释HXMT的观察结果。 我们在拟议项目中的研究可能是未来MeV观测的前期研究

We carry out theoretical and observational studies of the hard X-ray/soft gamma-ray emissions from the pulsar with using the Hard X-ray Telescope Monitor (HXMT). At the hard X-ray/soft gamma-ray bands, theoretical studies expecte that the pulsar emission process rom the curvature radiation process (or inverse-Compton scattering process) in GeV bands to the synchrotron process in the soft X-ray bands. It can be said hat a detail observation of HXMT is crucial to understand the multi-wavelength nature of the high-energy pulsars. In comparison to GeV pulsars (200 sources), however, number of pulsars seen at hard X-ray/soft gamma-ray (>10keV) remains small (~15 sources). Moreover, current data in the X-ray/soft gamma-rays include relatively large uncertainties. The current observations cannot provide enough information of the hard X-ray/soft gamma-ray emission of the pulsars. . With the wide coverage in the energy bands, HXMT perfectly suits for studying the hard X-ray/soft gamma-ray emission of the pulsar, and provide new insight the physical processes occurred in the pulsar magnetosphere. In the proposed project, we carry out a deep study of the hard X-ray/soft gamma-ray emissions from the Crab pulsar and PSR B1509-58, for which HXMT regularly collects the data. Although PSR B1509-58 is a young and energetic pulsar, it shows a dim GeV gamma-ray emission. It also shows a bright hard X-ray emission in comparison to other GeV pulsars. To understand what causes this difference in the spectra, it is important to fill the observational gap between the soft X-ray and the GeV gamma-ray bands. HXMT will enable us to carry out a detail study for the pulse profile and phase-resolved spectrum. The results will be compared with a three-dimensional radiation model. . In the theoretical study, we explore the possibilities that the difference in the spectral properties between the GeV gamma-ray pulsar and PSR B1509-58 is mainly caused by the difference in the viewing geometry. We will simulate the dependency of X-ray/gamma-ray spectra and light curves on the viewing geometry, and we will discuss if this model could explain the observations of HXMT.. About 5 young energetic pulsars show similar spectral behavior to PSR B1509-58, and they probably emit an observable hard X-ray emission with HXMT. In the project, therefore, we propose the observation of these pulsars (so called soft gamma-ray pulsars) with HXMT and we reveal the nature of the non-thermal emissions of the soft gamma-ray pulsars. PSR B1509-58 and other soft gamma-ray pulsars will be a primary target for future MeV telescopes, because they will be one of the brightest MeV sources in the sky. Our study in the proposed project can be a preceding research for the future MeV observations