The newly born magnetars powering gamma-ray burst internal-plateau emission: are there strange stars?

TL;DR

This paper explores whether strange stars, rather than neutron stars, can better explain the long-lasting, rapidly spinning magnetars powering gamma-ray burst internal-plateau emissions, by analyzing their spin stability.

Contribution

It proposes using GRB observations to test the strange star hypothesis based on the different spin stability properties of neutron stars and strange stars.

Findings

Strange stars can maintain rapid spins longer than neutron stars due to suppressed r-modes.

GRB data can potentially distinguish between neutron star and strange star models.

Rapid spin durations in GRBs may indicate the presence of strange stars.

Abstract

The internal-plateau X-ray emission of gamma-ray bursts (GRBs) indicates that a newly born magnetar could be the central object of some GRBs. The observed luminosity and duration of the plateaus suggest that, for such a magnetar, a rapid spin with a sub- or millisecond period is sometimes able to last thousands of seconds. In this case, the conventional neutron star (NS) model for the magnetar may be challenged, since the rapid spin of nascent NSs would be remarkably decelerated within hundreds of seconds due to r-mode instability. In contrast, the r-modes can be effectively suppressed in nascent strange stars (SSs). In other words, to a certain extent, only SSs can keep nearly-constant extremely-rapid spin for a long period of time during the early ages of the stars. We thus propose that the sample of the GRB rapidly-spinning magnetars can be used to test the SS hypothesis based on the distinct spin limits of NSs and SSs.