# Observational signature of a wind bubble environment for double neutron star mergers

## TL;DR

This paper investigates how wind bubbles created by electromagnetic radiation from double neutron star binaries affect short gamma-ray burst afterglows, revealing observable signatures that can inform about the binary environment and electromagnetic power.

## Contribution

It introduces a model linking wind bubble environments to observable afterglow features, enabling constraints on binary electromagnetic radiation through combined electromagnetic and gravitational wave observations.

## Key findings

- Abrupt jumps in afterglow light curves can occur due to wind bubble interactions.
- The timing of the light curve jump depends on the viewing angle.
- The method allows constraining the wind bubble radius and electromagnetic power.

## Abstract

During the in-spiral stage of a compact binary, a wind bubble could be blown into interstellar medium, if the electromagnetic radiation due to the binary orbital motion is strong enough. Therefore, short gamma-ray bursts (SGRBs) due to double neutron star mergers would in principle happen in a wind bubble environment, which can influence the propagation of the SGRB jet and the consequent afterglow emission. By calculating the dynamics and synchrotron radiation of the jet-driven external shock, we reveal that an abrupt jump could appear in the afterglow light curves of SGRBs and the observational time of the jump is dependent on the viewing angle. This light curve jump provides an observational signature to constrain the radius of the wind bubble and then the power of the binary electromagnetic radiation, by combining with gravitational wave detection.