# Properties of jet and surrounding material of GW/GRB~170817A

## TL;DR

This paper models the afterglows of GW/GRB 170817A using a multi-component jet structure, revealing insights into jet composition, beaming, and circum-burst environment based on broad band observations over a year.

## Contribution

It introduces a multi-component jet model with a structured relativistic jet and cocoon, consistent with long-term afterglow observations and previous prompt emission analysis.

## Key findings

- Jet has a core with Lorentz factor ~100 and a mildly relativistic cocoon.
- Afterglow rise linked to low circum-burst density and jet expansion.
- External shocks occurred >110 days post-merger, affecting jet evolution.

## Abstract

We use published data in radio, optical and X-ray bands to analyze and model afterglows of GW/GRB 170817A. Our analysis is based on a phenomenological gamma-ray burst generator model which we previously used to study the prompt gamma-ray emission of this important transient. We find a multi-component model and a few of its variants that are consistent with broad band $\sim 1$ year observations of afterglows, once the contribution of kilonova in optical/IR band is taken into account. Considering beaming and off-axis view, we interpret the components of the model as approximately presenting the profile of a relativistic structured jet with a rapidly declining Lorentz factor from our line of sight, where it had a Lorentz factor of $\mathcal {O}(100)$, to outer boundaries, where it became a mildly relativistic cocoon with a relative velocity to light of $\sim 0.4-0.97$. Properties of the jet core obtained here are consistent with conclusions from analysis of the prompt gamma-ray emission. In particular, our results show that after prompt internal shocks the remnant of the jet retains in some extent its internal collimation and coherence. Slow rise of the afterglows can be associated to low density of circum-burst material and low column density of the jet. The long distance of external shocks from the merger, which could have been in part responsible for extensive thinning of the jet through expansion and energy dissipation before occurrence of external shocks is responsible for the peak of emission being at $\gtrsim 110$~days after the merger. We discuss implications of these observations for properties of circum-burst material around binary neutron stars. This analysis confirms our previous results showing that an outflow with a Lorentz factor of $\sim 2-5$ cannot explain observed afterglows without an additional X-ray source or significant absorption of optical/IR photons.