Radio Emission from Supernova Remnants: Implications for Post-Shock Magnetic Field Amplification and the Magnetic Fields of Galaxies

Abstract

Using observations from the literature, we show that the non-thermal radio luminosity (L) of supernova remnants (SNRs) is a strong function of the average gas surface density (Sigma) of the galaxy in which the remnants reside, from normal spirals to luminous starbursts. We combine a simple theory for electron cooling in SNRs with the observed radio luminosities to estimate the remnant magnetic field strength (B_SNR): the correlation between L and Sigma implies that B_SNR also increases with Sigma. We explore two interpretations of this correlation: (1) B_SNR is generated by post-shock magnetic field amplification, with B_SNR^2 proportional to Sigma and (2) B_SNR results from shock-compression of the ambient ISM magnetic field (B_ISM), with B_ISM being larger in denser galaxies. We find that shock compression is, on average, sufficient to produce the observed radio emission from SNRs in the densest starbursts; amplification of post-shock magnetic fields is not required. By contrast, in normal spirals post-shock field amplification (by a factor of a few - 10) is consistent with the data; we find tentative evidence that both the Alfven speed and the ratio of B_SNR^2 to the post-shock pressure ("epsilon_B") are constant in SNRs from galaxy to galaxy. We discuss observational tests that can be used to distinguish between these two interpretations of the radio luminosities of SNRs. Regardless of which is correct, the radio emission from SNRs provides an upper limit to B_ISM that is independent of the minimum energy assumption. For the densest starbursts, the ISM magnetic energy density is below that required for hydrostatic equilibrium; thus magnetic fields are not dynamically important on the largest scales in starbursts, in contrast with spiral galaxies like our own. This dichotomy may have implications for galactic dynamo theory.