Constraining the magnetic field structure in collisionless relativistic shocks with a radio afterglow polarization upper limit in GW170817

Abstract

Gamma-ray burst afterglows arise from relativistic collisionless shocks in which the postshock tangled magnetic field $\vec{B}$ is produced by the two-stream and/or Weibel instabilities on plasma skin-depth scales $(c/ω_p)$. The field is expected to be oriented predominantly within the shock plane ($B_{\perp}$; transverse to the shock normal, $\hat{n}_{\rm{sh}}$), and is often approximated to be completely within it ($B_\parallel\equiv\hat{n}_{\rm{sh}}\,\cdot\,\vec{B}=0$). Current 2D/3D particle-in-cell simulations are limited to short timescales and box sizes $\lesssim10^4(c/ω_p)\ll R/Γ_{\rm{sh}}$ much smaller than the shocked region's comoving width, and cannot probe the asymptotic downstream $\vec{B}$ structure. We constrain the latter using the linear polarization upper limit, $|Π|<12\%$, on the radio afterglow of GW170817/GRB170817A. Afterglow polarization depends on the jet's angular structure, our viewing angle, and the $\vec{B}$ structure. In GW170817/GRB170817A the latter can be tightly constrained since the former two are constrained from observations. We model $\vec{B}$ as an isotropic field in 3D that is stretched along $\hat{n}_{\rm{sh}}$ by a factor $ξ\equiv{}B_{\parallel}/B_{\perp}$, whose initial value $ξ_f\equiv{}B_{\parallel,f}/B_{\perp,f}$ describes the field that survives downstream on plasma scales $\ll{}R/Γ_{\rm{sh}}$. We calculate $Π(ξ_f)$ by integrating over the shocked volume for core-dominated structured jets, with a local Blandford-McKee self-similar radial profile. We find that independent of the exact jet structure, $\vec{B}$ has a finite, but initially sub-dominant, parallel component: $0.57\lesssimξ_f\lesssim0.89$, making it less anisotropic. While this motivates numerical studies of the asymptotic $\vec{B}$ structure in relativistic collisionless shocks, it may be consistent with turbulence amplified magnetic field.