Photon Dispersion in a Supernova Core
Abstract
While the photon forward-scattering amplitude on free magnetic dipoles (e.g. free neutrons) vanishes, the nucleon magnetic moments still contribute significantly to the photon dispersion relation in a supernova (SN) core where the nucleon spins are not free due to their interaction. We study the frequency dependence of the relevant spin susceptibility in a toy model with only neutrons which interact by one-pion exchange. Our approach amounts to calculating the photon absorption rate from the inverse bremsstrahlung process gamma n n --> n n, and then deriving the refractive index nrefr with the help of the Kramers-Kronig relation. In the static limit (omega --> 0) the dispersion relation is governed by the Pauli susceptibility chiPauli so that (nrefr)2-1 approx chiPauli > 0. For omega somewhat above the neutron spin-relaxation rate Gammasigma we find (nrefr)2-1< 0, and for omega >> Gammasigma the photon dispersion relation acquires the form omega2-k2=(mgamma)2. An exact expression for the "transverse photon mass" mgamma is given in terms of the f-sum of the neutron spin autocorrelation function; an estimate is (mgamma)2 approx chiPauli T Gammasigma. The dominant contribution to nrefr$ in a SN core remains the electron plasma frequency so that the Cherenkov processes gamma nu <--> nu remain forbidden for all photon frequencies.
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