Szczegóły seminarium
Data: 09.01.2024
Pawel Szewczyk (PhD candidate, OAUW)
Are hypermassive neutron stars dynamically stable?
Streszczenie:
Neutron stars (NS) formed by collapse of a massive stellar core or in
binary NS mergers are known to begin their lives with a strongly
differential rotation. Even though the rotation becomes uniform on
long timescales, the differential rotation may play an important role
in the initial phase of the NS life. In particular, differentially
rotating NS can be much more massive than rigidly rotating NS. NS with
such large masses are called hypermassive.
However, these objects are not always dynamically stable. Some of them
may undergo a prompt collapse to a black hole. By performing a series
of numerical simulations, we inspect the limit of stability against
quasi-radial perturbations for a wide range of parameters of
differentially rotating NS. We also study the stability against
non-axisymmetrical perturbations for selected models.
I will present the results of our study of NS stability and discuss
their impact on observational prospects of core-collapse supernovae
and binary NS mergers.