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A nova occurs as a result of thermonuclear runaway in the accreted matter on the surface of a white dwarf in a close binary system. A considerable portion of the accreted matter is ejected at velocities of several thousand km/s. The brightness of the star increases by 6 to 9 magnitudes very rapidly, followed by a decline. Novae emit detectable radiation at almost all wavelengths. In this talk, we focus on the emission mechanisms and detections of novae at high energies using simple calculations and simulations.
BGS Office