M. Bejger (N. Copernicus Astronomical Center, Warsaw, Poland): Observational implications of dense matter phase transitions for the rotational evolution of neutron stars
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Europe/Budapest
Tanácsterem
Tanácsterem
Description
I will discuss the implications of a strong first-order
phase transition region in the dense matter equation of state in the
interiors of rotating neutron stars, and the resulting creation of two
disjoint families of neutron-stars' configurations (the so-called
high-mass twins). Rotating, axisymmetric and stationary stellar
configurations are obtained numerically in the framework of general
relativity, and their global parameters and stability are studied. The
equation of state-induced instability divides stable neutron star
configurations into two disjoint families: neutron stars (second
family) and hybrid stars (third family), with an overlapping region in
mass, the high-mass twin star region. These two regions are divided by
an instability strip. Its existence has interesting astrophysical
consequences for rotating neutron stars. It provides a "natural"
explanation for the rotational frequency cutoff in the observed
distribution of neutron stars spins, and for the apparent lack of
back-bending in pulsar timing. It also straightforwardly enables a
substantial energy release in a mini-collapse to another neutron-star
configuration (core quake), or to a black hole.
Based on arXiv:1608.07049
