Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001jkas...34..309t&link_type=abstract
Journal of the Korean Astronomical Society, vol. 34, no. 4, pp. 309-311
Astronomy and Astrophysics
Astronomy
1
Magnetohydrodynamics: Magnetic Reconnection: Galaxy
Scientific paper
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 B_local 30 micro Gauss 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 _obs 3 micro Gauss 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 reconnection triggered by a supernova shock (fig.1). We assume that the magnetic field is B_x=30 tanh(y/20 pc) micro Gauss, B_y=B_z=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 reconnection, and the gas is heatd to >7 keV. The magnetic reconnection heats the interstellar gas to 7 keV in the Galactic plane, if it occurs in the locally strong magnetic fields of B_local 30 micro Gauss. The heated plasma is confined by the magnetic field for 1E+5.5 yr. The required interval of the magnetic reconnections (triggered by anything) is 1-10 yr. The magnetic reconnection will explain the origin of X-rays from the Galactic ridge, furthermore the Galactic halo, and clusters of galaxies.
Kudoh Takahiro
Shibata Kazunari
Tanuma Syuniti
Yokoyama Takaaki
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