D-112 Be/X 線連星における中性子星周囲に形成される降着円盤の進化と構造

概要

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We study the accretion onto the neutron star in Be/X-ray binaries, using the 3D SPH code and the data from the simulations by Okazaki et al. (2002) for a coplanar system with a short period (P_<orb>=24.3 days) and moderate eccentricity (e=0.34). We find that a non-steady accretion disk is formed around the neutron star. The disk shrinks after the periastron passage of the Be star and restores its radius afterwards. While the mass-capture rate by the neutron star has a regular, strong dependence on the orbital phase, the orbital modulation in the accretion rate slowly gradually decreases. Our simulations show that the truncated Be disk model for Be/X-ray binaries is consistent with the observed X-ray behavior.
2003-07-28