Polarization Predictions in the GRB Prompt Phase with the Internal Shock Model

TL;DR

This paper investigates polarization predictions during the GRB prompt phase within the magnetized internal shock model, highlighting how energy-dependent polarization can differentiate it from other models like magnetic reconnection.

Contribution

It provides detailed polarization predictions for the magnetized internal shock model, emphasizing the energy dependence of polarization degree as a key discriminant from other models.

Findings

Energy-dependent polarization degree increases at high energies for the magnetized IS model.

Polarization profiles are similar for time-integrated and time-resolved measurements.

Energy dependence of polarization degree can distinguish between the magnetized IS and dissipative photosphere models.

Abstract

As the standard gamma-ray burst (GRB) prompt-emission model, the internal shock (IS) model can reproduce the fast-rise and slow-decay features of the pulses in the GRB light curve. The time- and energy-dependent polarization can deliver important physical information on the emission region and can be used to test models. Polarization predictions for the GRB prompt phase with the magnetized IS model should be investigated carefully. The magnetic field of the magnetized IS model is very likely to be mixed and decays with radius. The synchrotron emission in the presence of such a decaying magnetic field can recover the Band-like spectrum of the GRB prompt phase. We investigate the dependence of the polarization of GRB prompt emission on both time and energy in the framework of the magnetized IS model. Due to the large range of parameters, it is hard to distinguish the magnetized IS model and the magnetic-reconnection model through polarization degree (PD) curves. The energy-dependent PD could increase toward the high-energy band for the magnetized IS model, while it decreases to zero above the megaelectronvolt band for the dissipative photosphere model. Therefore, we conclude that the energy dependence of PD can be used to distinguish these two models for the GRB prompt emission. Finally, we find that, independent of the observational energy band, the profiles of the $\xi_B-PD$ curve for the time-integrated and time-resolved PDs are very similar, where $\xi_B$ is the magnetic field strength ratio of the ordered component to the random component.