Evolution of the magnetic field in neutron stars

Gusakov, M. E.; Kantor, E. M.; Ofengeim, D. D.

doi:10.1103/physrevd.96.103012

Cited by 48 publications

(84 citation statements)

References 50 publications

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“…Flavorchanging reactions also contribute to the bulk viscosity of the matter (e.g., [8]) that can be important in the evolution of the NS oscillations. Finally, these reactions are important in regulating the magnetic field evolution in the NSs where some degree of the compositional asymmetry induced by the magnetic field can be expected, e.g., [39].…”

Section: Discussionmentioning

confidence: 99%

In-medium enhancement of the modified Urca neutrino reaction rates

2018

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We calculate modified Urca neutrino emission rates in the dense nuclear matter in neutron star cores. We find that these rates are strongly enhanced in the beta-stable matter in regions of the core close to the direct Urca process threshold. This enhancement can be tracked to the use of the in-medium nucleon spectrum in the virtual nucleon propagator. We describe the in-medium nucleon scattering in the non-relativistic Bruckner-Hartree-Fock framework taking into account two-body as well as the effective threebody forces, although the proposed enhancement does not rely on a particular way of the nucleon interaction treatment. Finally we suggest a simple approximate expression for the emissivity of the neutron branch of the modified Urca process that can be used in the neutron stars cooling simulations with any nucleon equation of state of dense matter.

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Section: Discussionmentioning

confidence: 99%

In-medium enhancement of the modified Urca neutrino reaction rates

2018

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“…However, the MF evolution of the core is much more complex and uncertain because of the possible presence of several particle species, the effect of weak interactions (βequilibrium) and particle diffusion, the possible existence of superfluidity/superconductivity, etc. (see a thorough list of references in Gusakov et al (2017)). Additionally, it is still under debate to what extent magneto-hydrodynamic equilibrium in NSs are arbitrary for given EOSs, with or without axisymmetry (Glampedakis & Lasky 2016;Gusakov et al 2017).…”

Section: Introductionmentioning

confidence: 99%

“…(see a thorough list of references in Gusakov et al (2017)). Additionally, it is still under debate to what extent magneto-hydrodynamic equilibrium in NSs are arbitrary for given EOSs, with or without axisymmetry (Glampedakis & Lasky 2016;Gusakov et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Magnetized hybrid stars: effects of slow and rapid phase transitions at the quark–hadron interface

Mariani

Orsaria

Ranea‐Sandoval

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We study the influence of strong magnetic fields in hybrid stars, composed by hadrons and a pure quark matter core, and analyse their structure and stability as well as some possible evolution channels due to the magnetic field decay. Using an ad-hoc parametrisation of the magnetic field strength and taking into account Landau-quantization effects in matter, we calculate hybrid magnetised equations of state and some associated quantities, such as particle abundances and matter magnetisation, for different sets of parameters and different magnetic field strengths. Moreover, we compute the magnetised stable stellar configurations, the mass versus radius and the gravitational mass versus central energy density relationships, the gravitational mass versus baryon mass diagram, and the tidal deformability. Our results are in agreement with both, the ∼ 2M pulsars and the data obtained from GW170817. In addition, we study the stability of stellar configurations assuming that slow and rapid phase transitions occur at the sharp hadron-quark interface. We find that, unlike in the rapid transition scenario, where ∂ M/∂ c < 0 is a sufficient condition for instability, in the slow transition scenario there exists a connected extended stable branch beyond the maximum mass star, for which ∂ M/∂ c < 0. Finally, analysing the gravitational mass versus baryon mass relationship, we have calculated the energy released in transitions between stable stellar configurations. We find that the inclusion of the magnetic field and the existence of new stable branches allows the possibility of new channels of transitions that fulfil the energy requirements to explain Gamma Ray Bursts. From a model-theoretical point of view, magnetars are magnetised NSs (M ∼ 2 M , R ∼ 15 km (Glendenning 1997)) with an external solid crust and an internal extremely dense

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“…In the core, however, the situation is less clear and there is increasing evidence that ambipolar diffusion and/or fluid motions are key to describe the magnetic field evolution. Several recent papers have started to address this problem with numerical simulations or novel theoretical ideas [29,30,31,32,33,34,35,36].…”

Section: Introductionmentioning

confidence: 99%

A Simflowny-based high-performance 3D code for the generalized induction equation

Viganò

Martínez‐Gómez

Pons

et al. 2019

Computer Physics Communications

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In the interior of neutron stars, the induction equation regulates the long-term evolution of the magnetic fields by means of resistivity, Hall dynamics and ambipolar diffusion. Despite the apparent simplicity and compactness of the equation, the dynamics it describes is not trivial and its understanding relies on accurate numerical simulations. While a few works in 2D have reached a mature stage and a consensus on the general dynamics at least for some simple initial data, only few attempts have been performed in 3D, due to the computational costs and the need for a proper numerical treatment of the intrinsic non-linearity of the equation.Here, we carefully analyze the general induction equation, studying its characteristic structure, and we present a new Cartesian 3D code, generated by the user-friendly, publicly available Simflowny platform. The code uses high-order numerical schemes for the time and spatial discretization, and relies on the highly-scalable SAMRAI architecture for the adaptive mesh refinement. We present the application of the code to several benchmark tests, showing the high order of convergence and accuracy achieved and the capabilities in terms of magnetic shock resolution and three-dimensionality. This paper paves the way for the applications to a realistic, 3D long-term evolution of neutron stars interior and, possibly, of other astrophysical sources.

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Evolution of the magnetic field in neutron stars

Cited by 48 publications

References 50 publications

In-medium enhancement of the modified Urca neutrino reaction rates

In-medium enhancement of the modified Urca neutrino reaction rates

Magnetized hybrid stars: effects of slow and rapid phase transitions at the quark–hadron interface

A Simflowny-based high-performance 3D code for the generalized induction equation

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