Shock Acceleration Efficiency in Kepler's Supernova Remnant

Details Shock Acceleration Efficiency in Kepler's Supernova Remnant Shock Acceleration Efficiency in Kepler's Supernova Remnant

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21923920r&link_type=abstract

American Astronomical Society, AAS Meeting #219, #239.20

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Scientific paper

Fast shock waves like those in young supernova remnants put some fraction of their energy into fast particles, and another fraction into magnetic field. These fractions are not well determined typically, because synchrotron emission from relativistic electrons depends on roughly the product of the two, while the shock energy density depends on gas density and shock speed. Shock speeds can be difficult to determine from thermal X-ray spectra, as electrons and ions may have different temperatures, and significant energy may be lost to the fast particles. Most importantly, accurate thermal-gas densities are often unknown, or only roughly known from X-ray emission measures. All these quantities may vary at different locations in a supernova remnant. We present new determinations of gas densities at various points around the periphery of Kepler's supernova remnant, from modeling Spitzer IRS spectra from shock-heated dust. In combination with shock velocities from proper motions, radio brightnesses, and magnetic-field determinations from X-ray synchrotron morphology, we can then estimate the fractions of shock energy in relativistic electrons and in magnetic field, at different points around the remnant periphery. Furthermore, X-ray synchrotron emission visible around much of the periphery allows the determination of maximum electron energies. We present spatially resolved estimates of these quantities and discuss their significance for theoretical models of shock acceleration.

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