2024A&A...684A..16D

The linear polarization of the optical continuum of type II supernovae (SNe), together with its temporal evolution is a promising source of information about the large-scale geometry of their ejecta. To help access this information, we undertook 2D polarized radiative transfer calculations to map the possible landscape of type II SN continuum polarization (P_cont) from 20 to 300 days after explosion. Our simulations were based on crafted 2D axisymmetric ejecta constructed from 1D nonlocal thermodynamic equilibrium time-dependent radiative transfer calculations for the explosion of a red supergiant star. Following the approach used in our previous work on SN 2012aw, we considered a variety of bipolar explosions in which spherical symmetry is broken by material within ∼30° of the poles that has a higher kinetic energy (up to a factor of two) and higher ⁵⁶Ni abundance (up to a factor of about five, allowing for ⁵⁶Ni at high velocity). Our set of eight 2D ejecta configurations produced considerable diversity in P_cont (λ ∼ 7000 Å), although its maximum of 1-4% systematically occurs around the transition to the nebular phase. Before and after this transition, P_cont may be null, constant, rising, or decreasing, which is caused by the complex geometry of the depth-dependent density and ionization and also by optical depth effects. Our modest angle-dependent explosion energy can yield a P_cont of 0.5-1% at early times. Residual optical-depth effects can yield an angle-dependent SN brightness and constant polarization at nebular times. The observed values of P_cont tend to be lower than obtained here. This suggests that more complicated geometries with competing large-scale structures cancel the polarization. Extreme asymmetries seem to be excluded.