Signature of strange star as the central engine of GRB 240529A

TL;DR

This paper proposes that the complex emission features of GRB 240529A can be explained by a transition from a supramassive magnetar to a strange star, supported by observational data fitting this physical model.

Contribution

It introduces a novel model linking the prompt and afterglow emissions of GRB 240529A to a magnetar-strange star phase transition, which differs from standard black hole models.

Findings

The prompt emission episodes align with jet activity from a collapsing star and magnetar re-activation.

The third prompt episode matches the phase transition from magnetar to strange star.

The X-ray plateau emissions correspond to cooling and spin-down processes of the strange star.

Abstract

GRB 240529A is a long-duration gamma-ray burst (GRB) whose light curve of prompt emission is composed of a triple-episode structure, separated by quiescent gaps of tens to hundreds of seconds. More interestingly, its X-ray light curve of afterglow exhibits two-plateau emissions, namely, an internal plateau emission that is smoothly connected with a $\sim t^{-0.1}$ segment and followed by a $\sim t^{-2}$ power-law decay. The three episodes in the prompt emission, together with two plateau emissions in X-ray, are unique in the Swift era. They are very difficult to explain with the standard internal/external shock model by invoking a black hole central engine. However, it could be consistent with the prediction of a supramassive magnetar as the central engine, the physical process of phase transition from magnetar to strange star, as well as the cooling and spin-down of the strange star. In this paper, we propose that the first- and second-episode emissions in the prompt $\gamma-$ray of GRB 240529A are from the jet emission of a massive star collapsing into a supramassive magnetar and the re-activity of central engine, respectively. Then, the third-episode emission of prompt is attributed to the phase transition from a magnetar to a strange star. Finally, the first- and second-plateau emissions of the X-ray afterglow are powered by the cooling and spin-down of the strange star, respectively. The observational data of each component of GRB 240529A are roughly coincident with the estimations of the above physical picture.