Maximum energies of shock-accelerated electrons in supernova remnants in the large magellanic cloud

Details Maximum energies of shock-accelerated electrons in supernova remnants in the large magellanic cloud Maximum energies of shock-accelerated electrons in supernova remnants in the large magellanic cloud

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aipc..565..387h&link_type=abstract

YOUNG SUPERNOVA REMNANTS: Eleventh Astrophysics Conference. AIP Conference Proceedings, Volume 565, pp. 387-390 (2001).

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Supernova Remnants, Magellanic Clouds And Other Irregular Galaxies, Cosmic Rays

Scientific paper

Some supernova-remnant X-ray spectra show evidence for synchrotron emission from the extension of the electron spectrum producing radio synchrotron emission. For any remnant, if the extrapolated radio flux exceeds the observed X-ray flux (thermal or nonthermal), a rolloff of the relativistic-electron energy distribution must occur below X-ray emitting energies. We have studied the X-ray emission from a sample of 11 remnants in the Large Magellanic Cloud to constrain this rolloff energy. We assume that the electron distribution is a power law with an exponential cutoff at some Emax and radiates in a uniform magnetic field. If the radio flux and spectral index are known, this simple model for the synchrotron contribution depends on only one parameter which relates directly to Emax. Here we have modeled the X-ray spectra by adding a component for thermal radiation of a Sedov blast wave to the synchrotron model. For all 11 supernova remnants in this sample, the limits for Emax range between 10 and 70 TeV (for a mean magnetic field of 10 μG). We interpret Emax in the context of shock acceleration theories. .

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