Upper critical field and (non)-superconductivity of magnetars
TLDR
In this article, the authors construct equilibrium models of compact stars using a realistic equation of state and obtain the density range occupied by the proton superconductor in strong B-fields.Abstract:
We construct equilibrium models of compact stars using a realistic equation of state and obtain the density range occupied by the proton superconductor in strong B-fields. We do so by combining the density profiles of our models with microscopic calculations of proton pairing gaps and the critical unpairing field H
c2 above which the proton type-II superconductivity is destroyed. We find that magnetars with interior homogeneous field within the range 0.1 ≤ B
16 ≤ 2, where B
16 = B/1016 G, are partially superconducting, whereas those with B
16 > 2 are void of superconductivity. We briefly discuss the neutrino emissivity and superfluid dynamics of magnetars in the light of their (non)-superconductivity.read more
Citations
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Axion star collisions with neutron stars and fast radio bursts
TL;DR: In this article, the authors argue that collisions of dilute axion stars with neutron stars, of the type known as "magnetars," may be the origin of most of the observed fast radio bursts.
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Equation of State of Strongly Magnetized Matter with Hyperons and Δ-Resonances
TL;DR: In this article, a new equation of state for the baryonic matter under an intense magnetic field was constructed within the framework of covariant density functional theory, where the composition of matter includes hyperons as well as Δ-resonances.
Journal ArticleDOI
Equation of state of strongly magnetized matter with hyperons and $\Delta$-resonances
TL;DR: In this article, a new equation of state for the baryonic matter under an intense magnetic field was constructed within the framework of covariant density functional theory, which includes hyperons as well as $ \Delta$-resonances.
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Rapid rotational crust-core relaxation in magnetars
TL;DR: In this article, it was shown that the rapid crust-core coupling is incompatible with oscillation models of magnetars that completely decouple the core superfluid from the crust and that magnetar precession is damped by the coupling of normal fluids to the superfluid core and, if observed, needs to be forced or continuously excited by seismic activity.
References
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Poloidal magnetic fields in superconducting neutron stars
K. T. Henriksson,Ira Wasserman +1 more
TL;DR: In this article, the authors developed a formalism for computing the magnetic field within an axisymmetric neutron star with a strong Type II superconductor core surrounded by a normal conductor.
Journal ArticleDOI
Direct URCA process in neutron stars with strong magnetic fields
L.B. Leinson,Armando Pérez +1 more
TL;DR: In this article, the emissivity of the direct URCA process in strongly magnetized, degenerate matter in neutron stars, under β-equilibrium conditions, was analyzed.
Journal ArticleDOI
Vertex renormalization of weak interactions in compact stars: Beyond leading order
TL;DR: In this paper, the neutrino emission rate from baryonic matter in neutron stars via weak neutral vector interaction is computed up to order O(v_F^6), where v_F is the Fermi velocity in units of speed of light.
Posted Content
Rotating neutron star models with magnetic field
TL;DR: In this paper, the first numerical solutions of the coupled Einstein-Maxwell equations describing rapidly rotating neutron stars endowed with a magnetic field were presented, which are fully relativistic and self-consistent, all the effects of the electromagnetic field on the star's equilibrium (Lorentz force, spacetime curvature generated by the electromagnetic stress energy) being taken into account.
Journal ArticleDOI
Damping of differential rotation in neutron stars
TL;DR: In this article, the authors derived the transport relaxation times for quasiparticle-vortex scattering processes via nuclear force, relevant for the damping of the differential rotation of superfluids in the quantum liquid core of a neutron star.
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