Neutron Star Phase Transition as the Origin for the Fast Radio Bursts and Soft Gamma-Ray Repeaters of SGR J1935+2154

Magnetars are believed to be neutron stars (NSs) with strong magnetic fields. X-ray flares and fast radio bursts (FRBs) have been observed from the magnetar (soft gamma-ray repeater, SGR J1935+2154). We propose that the phase transition of the NS can power the FRBs and SGRs. Based on the equation of state provided by the MIT bag model and the mean field approximation, we solve the Tolman-Oppenheimer-Volkoff equations to get the NS structure. With the spin-down of the NS, the hadronic shell gradually transfers to the quark shell. The gravitational potential energy released by one time of the phase transition can be achieved. The released energy, time interval between two successive phase transitions, and glitch are all consistent with the observations of the FRBs and the X-ray flares from SGR J1935 + 2154. We conclude that the phase transition of an NS is a plausible mechanism to power the SGRs as well as the repeating FRBs.

Automated summary

Magnetars, which are neutron stars with strong magnetic fields, have been observed to emit X-ray flares and fast radio bursts (FRBs). This study proposes that the phase transition of neutron stars can generate the energy required for FRBs and SGRs. By solving the Tolman-Oppenheimer-Volkoff equations using the MIT bag model and mean field approximation, the authors find that the phase transition from hadronic to quark matter releases significant gravitational potential energy. The energy released, time interval between phase transitions, and observed glitches align with the behavior of FRBs and X-ray flares from SGR J1935+2154. Therefore, the phase transition of neutron stars is a plausible mechanism to power SGRs and repeating FRBs.