Polarization of gamma-ray burst afterglows in the synchrotron self-Compton process from a highly relativistic jet

TL;DR

This paper models the polarization of gamma-ray burst afterglows considering synchrotron self-Compton processes in a relativistic jet with mixed magnetic fields, explaining observed polarization limits and potential angle changes over time.

Contribution

It introduces a calculation of polarization properties in GRB afterglows with mixed magnetic fields, extending understanding of polarization behavior in relativistic jets.

Findings

Polarization in afterglows is generally below 10%.

Random magnetic fields limit polarization to about 10%.

Polarization angle may shift by 90° if magnetic components decay differently.

Abstract

Linear polarization have been observed in both the prompt phase and afterglow of some bright gamma-ray bursts (GRBs). Polarization in the prompt phase spans a wide range, and may be as high as $\gtrsim 50\%$. In the afterglow phase, however, it is usually below $10\%$. According to the standard fireball model, GRBs are produced by synchrotron radiation and Compton scattering process in a highly relativistic jet ejected from the central engine. It is widely accepted that prompt emissions occur in the internal shock when shells with different velocities collide with each other, and the magnetic field advected by the jet from the central engine can be ordered in large scale. On the other hand, afterglows are often assumed to occur in the external shock when the jet collides with interstellar medium, and the magnetic field produced by the shock through, e.g. Weibel instability, is possibly random. In this paper, we calculate the polarization properties of the synchrotron self-Compton process from a highly relativistic jet, in which the magnetic field is randomly distributed in the shock plane. We also consider the generalized situation where a uniform magnetic component perpendicular to the shock plane is superposed on the random magnetic component. We show that, the polarization is hardly to be larger than $10\%$ if the seed electrons are isotropic in the jet frame. This may account for the observed upper limit of polarization in the afterglow phase of GRBs. In addition, if the random and uniform magnetic components decay with time in different speeds, then the polarization angle may change $90^{\circ}$ duration the temporal evolution.