Strong thermal X-ray emission, called Galactic Ridge X-ray Emission, is observed along the Galactic plane (Koyama et al. 1986). The origin of hot (~7 keV) component of GRXE is not known, while cool (~0.8 keV) one is associated with supernovae (Kaneda et al. 1997, Sugizaki et al. 2001). We propose a possible mechanism to explain the origin; locally strong magnetic fields of Blocal ~30 μG heat interstellar gas to ~7 keV via magnetic reconnection (Tanuma et al. 1999). There will be the small-scale (< 10 pc) strong magnetic fields, which can be observed as (B)obs ~3 μG by integration of Faraday Rotation Measure, if it is localized by a volume filling factor of f ~ 0.1. In order to examine this model, we solved three-dimensional (3D) resistive magnetohydrodynamic (MHD) equations numerically to examine the magnetic reconnect ion triggered by a supernova shock (fig.l). We assume that the magnetic field is Bx = 30tanh(y/20pc) μG, By = Bz = 0, and the temperature is uniform, at the initial condition. We put a supernova explosion outside the current sheet. The supernova-shock, as a result, triggers the magnetic reconnect ion, and the gas is heatd to > 7 keV. The magnetic reconnect ion heats the interstellar gas to ~7 keV in the Galactic plane, if it occurs in the locally strong magnetic fields of Blocal ~30 μG. The heated plasma is confined by the magnetic field for ~10 5.5 yr. The required interval of the magnetic reconnect ions (triggered by anything) is ~1 - 10 yr. The magnetic reconnect ion will explain the origin of X-rays from the Galactic ridge, furthermore the Galactic halo, and clusters of galaxies.

• SYUNITI TANUMA(Solar-Terrestrial Environment Laboratory, Nagoya University)
• TAKAAKI YOKOYAMA(Nobeyama Radio Observatory)
• TAKAHIRO KUDOH(National Astronomical Observatory of Japan)
• KAZUNARI SHIBATA(Kwazan Observatory, Kyoto University)