Synchrotron Radiation from Galactic Sources: What We Can Learn About Particle Acceleration

Details Synchrotron Radiation from Galactic Sources: What We Can Learn About Particle Acceleration Synchrotron Radiation from Galactic Sources: What We Can Learn About Particle Acceleration

Oct 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001ssrv...99..177r&link_type=abstract

Space Science Reviews, v. 99, Issue 1/4, p. 177-186 (2001).

Computer Science

6

Scientific paper

I review the observations of galactic synchrotron sources, focusing on shell supernova remnants (SNRs), with particular attention to attributes that constrain the properties of electron acceleration. Radio observations provide information on source fluxes, spectral index, morphology, and polarization. Recent observations give us strong reason to believe that several young SNRs show synchrotron X-ray emission. Even if X-rays are thermal, however, limits can be set on the maximum energy to which electrons can be accelerated without a spectral break, since no galactic SNR is observed to have X-ray emission (due to any source) as bright as the extrapolation from radio frequencies of radio synchrotron emission. If synchrotron X-rays are detected or inferred, their morphology and spectrum provide important information on mechanisms governing acceleration to the highest energies. I describe models of synchrotron emission from SNRs and their comparison with observations. Finally, I describe the tasks ahead for both observers and theoreticians, to make better use of what SNR synchrotron emission tells us about particle acceleration.

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