Phase transitions in rotating neutron stars cores: back bending, stability, corequakes, and pulsar timing

@article{Zdunik2006PhaseTI,
  title={Phase transitions in rotating neutron stars cores: back bending, stability, corequakes, and pulsar timing},
  author={Julian Leszek Zdunik and Michał Bejger and Paweł Haensel and E. Gourgoulhon},
  journal={Astronomy and Astrophysics},
  year={2006},
  volume={450},
  pages={747-758}
}
Aims. We analyze potentially observable phenomena during spin evolution of isolated pulsars, such as back bending and corequakes resulting from instabilities, which could result from phase transitions in neutron star cores. Methods. We study these aspects of spin evolution of isolated compact stars by means of analytical models of equations of state, for both constant-pressure phase transitions and the transitions through the mixed-phase region. We use high-precision 2-D multi-domain spectral… 
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References

SHOWING 1-10 OF 24 REFERENCES
Phase Transitions in Rotating Neutron Stars: Effects of Stellar Crusts
As a rapidly rotating neutron star spins down due to the loss of its angular momentum, its central density increases and the nuclear matter in its core converts to quark matter, which leads to a
Phase transitions in rotating neutron stars
As rotating neutron stars slow down, the pressure and the density in the core region increase due to the decreasing centrifugal forces and phase transitions may occur in the center. We extract the
Hyperon softening of the EOS of dense matter and the spin evolution of isolated neutron stars
The effect of the hyperon softening of the equation of state (EOS) of dense matter on the spin evolution of isolated neutron stars is studied for a broad set of hyperonic EOSs. We use a multidomain
Spin-down of relativistic stars with phase transitions and PSR J0537-6910
Using a highly accurate numerical code, we study the spin down of rotating relativistic stars undergoing a quark deconfinement phase transition. Such phase transitions have been suggested to yield an
Mixed-phase induced core-quakes and the changes in neutron-star parameters
We present approximate formulae describing the changes in neutron-star parameters caused by the first-order phase transition to an exotic state (pion or kaon condensate, quark matter) resulting in
Signal of Quark Deconfinement in the Timing Structure of Pulsar Spin-Down
(May, 12, 1997)The conversion of nuclear matter to quark matter in thecore of a rotating neutron star alters its moment of inertia.Hence the epoch over which conversion takes place will be sig-naled
First-order phase transitions with more than one conserved charge: Consequences for neutron stars.
  • Glendenning
  • Physics
    Physical review. D, Particles and fields
  • 1992
TLDR
It is pointed out that the general results pertain to relativistic nuclear collisions in the so-called stopping or baryon-rich domain where there are three conserved charges (baryon, electric, and strangeness), and impact the expected phase transition from confined hadronic matter to quark matter as regards signals that are supposedly driven by pressure.
Construction of highly accurate models of rotating neutron stars: Comparison of three different numerical schemes
TLDR
The codes can be used for theruction of highly accurate initial data congurations for polytropes of index N> 0 :5 (which typically correspond to realistic neutron stars), when the domain of integra- tion includes all space and for realistic equations with no phase transitions.
An Effective equation of state for dense matter with strangeness
...
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