Speaker
Description
We study rotating hybrid stars, with a particular emphasis on the effect of a deconfinement phase
transition on their properties at high spin. Our analysis is based on a hybrid equation of state with
a phase transition from hypernuclear matter to color-superconducting quark matter, where both
phases are described within a relativistic density functional approach. By varying the vector meson
and diquark couplings in the quark matter phase, we obtain different hybrid star sequences with
varying extensions of the quark matter core, ensuring consistency with astrophysical constraints
from mass, radius, and tidal deformability measurements. We test whether the early deconfinement
phase transition is consistent with the present observational data. We show how the fastest spinning
pulsars and the appearance of the quasi-radial oscillations and non-axisymmetric instabilities constrain the strongly interacting matter equation of state at zero temperature. Our findings reveal that
incorporating the hybrid equation of state into the analysis of pulsars has significant implications
for the constraints on the properties of strongly interacting matter and neutron stars which is of the
high interest for the future SKA observations.
