A theoretical study to construct a unified model for high mass binaries with very high energy Gamma-ray emissions.

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A goal of this study is to construct a unified model for an emission mechanism of high mass binaries emitting very high energy Gamma-rays. For high mass binaries including pulsar and Be type star, we research on interactions between pulsar wind and stellar wind/decretion disk using a numerical simulation (1) and an analytical approach (2).In the case of (1), for the high density disk a cavity is made in the disk by pulsar wind. Thus, we show that intense Gamma-rays are emitted from the cavity because of high pressure in the cavity and large emission area. In the case of (2), for the strongly driven pulsar it goes into more inside the disk. Thus, we show that a double-peak light curve of Gamma-rays in the observation is explained.