On the Spectrum of Electrons Accelerated in Supernova Remnants. (arXiv:1905.07414v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Diesing_R/0/1/0/all/0/1">Rebecca Diesing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caprioli_D/0/1/0/all/0/1">Damiano Caprioli</a>
Using a semi-analytic model of non-linear diffusive shock acceleration, we
model the spectrum of cosmic ray (CR) electrons accelerated by supernova
remnants (SNRs). Because electrons experience synchrotron losses in the
amplified magnetic fields characteristic of SNRs, they exhibit substantially
steeper spectra than protons. In particular, we find that the difference
between the electron and proton spectral index (power law slope) ranges from
0.1 to 0.4. Our findings must be reckoned with theories of Galactic CR
transport, which often assume that electrons and protons are injected with the
same slope, and may especially have implications for the observed “positron
excess.”
Using a semi-analytic model of non-linear diffusive shock acceleration, we
model the spectrum of cosmic ray (CR) electrons accelerated by supernova
remnants (SNRs). Because electrons experience synchrotron losses in the
amplified magnetic fields characteristic of SNRs, they exhibit substantially
steeper spectra than protons. In particular, we find that the difference
between the electron and proton spectral index (power law slope) ranges from
0.1 to 0.4. Our findings must be reckoned with theories of Galactic CR
transport, which often assume that electrons and protons are injected with the
same slope, and may especially have implications for the observed “positron
excess.”
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