We quantify the impact of strong magnetic fields (assuming $B=B_0\cdot r_0^3/r^3$ with $B_0\gtrsim 10^{ 16}$ G) on the neutrino transport in core-collapse supernovae (CCSNe). Magnetic fields quantize the momenta of electrons and positrons, resulting in an enhanced absorption cross section for low-energy neutrinos and suppressed chemical potentials for $e^\pm$. We include these changes in the M1 scheme for neutrino transport and perform 1-D CCSNe simulations with \texttt{ GR1D}. The increased low-energy cross sections reduce the $\bar{ \nu}_e$ mean energy $\langle E_{ \bar\nu_e}\rangle$ while elevating the neutrino number luminosities $\mathcal{ L_\nu}$ for both ${ \nu}_e$ and $\bar{ \nu}_e$ due to the lower energy weighted spectra. The reduction of chemical potential enhances the $\bar{ \nu}_e$ emission while suppressing that of $\nu_e$, thereby driving an increase in the electron fraction behind the stalled shock at $\sim30$--$100$ km. This further amplifies $\langle E_{ \nu_e}\rangle$ through an increased electron density. Consequently, magnetic fields amplify $L_{ \nu_e}$ by increasing both $\mathcal{ L}_{ \nu_e}$ and $\langle E_{ \nu_e}\rangle$ whereas for $\bar\nu_e$, the rise in $\mathcal{ L}_{ \bar\nu_e}$ is offset by a decreased $\langle E_{ \bar\nu_e}\rangle$, leading to a minimal change in $L_{ \bar\nu_e}$. A systematic parameter scan of dipole field configurations suggests that, for $r_0 > 30$ km, $\langle E_{ \bar{ \nu}_e} \rangle$ is significantly suppressed and $L_{ \nu_e}$ is enhanced if $B_0 \geq { 2.7} \times 10^{ 16}$ G. These magnetic effects become negligible for $B_0$ below $\sim { 7.4} \times 10^{ 15}$ G.
Categories: astro-ph.HE