http://arxiv.org/abs/2301.05401
Millisecond magnetars produced in the center of dying massive stars are one prominent model to power gamma-ray bursts (GRBs). Their detailed nature, however, remains unsolved. To explore the effects of the initial mass, rotation, mass loss, and metallicity of the progenitor stars of $10-30~M_\odot$ on the formation and properties of the protomagnetars, we evolve over 150 single star models from the pre-main-sequence to core collapse by using the stellar evolution code MESA. We find that all of the fast-rotating stars become Wolf-Rayet stars. The final stellar, helium and carbon-oxygen core masses roughly increase with increasing initial mass, and decrease moderately with increasing initial rotation rate. We illustrate the effects of these intrinsic signatures on the hydrogen and helium envelopes and the metallicity. We then discuss the progenitors of the different types of supernovae. Furthermore, we find that the compactness parameter remains a nonmonotonic function of the initial mass and initial velocity when the effects of different metallicity and wind mass loss are considered. More importantly, we present the estimated period, magnetic field strength, and masses of protomagnetars in all cases. The typical rotational energy of these millisecond magnetars is sufficient to power long-duration GRBs.
C. Song and T. Liu
Mon, 16 Jan 23
50/50
Comments: 27 pages, 11 figures in main text, 1 table in appendix
You must be logged in to post a comment.