Electrical conductivity tensor of dense plasma in magnetic fields

Harutyunyan, Arus; Sedrakian, Armen

doi:10.22323/1.262.0011

Cited by 3 publications

(4 citation statements)

References 6 publications

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“…The recent detections of gravitational waves by the LIGO-Virgo collaboration, in particular, the multimessenger binary-neutron star (BNS) merger event GW170817 [1], motivate studies of the transport properties of dense nuclear matter at temperatures and densities relevant to BNS mergers [2][3][4][5][6][7]. The mass of the post-merger object typically would exceed the maximum mass of a neutron star and, as a consequence, it would collapse to a black hole on the timescales ranging from tens of milliseconds up to seconds depending on the mass of the post-merger object [8][9][10].…”

Section: Introductionmentioning

confidence: 99%

Bulk Viscous Damping of Density Oscillations in Neutron Star Mergers

2020

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In this paper, we discuss the damping of density oscillations in dense nuclear matter in the temperature range relevant to neutron star mergers. This damping is due to bulk viscosity arising from the weak interaction "Urca" processes of neutron decay and electron capture. The nuclear matter is modelled in the relativistic density functional approach. The bulk viscosity reaches a resonant maximum close to the neutrino trapping temperature, then drops rapidly as temperature rises into the range where neutrinos are trapped in neutron stars. We investigate the bulk viscous dissipation timescales in a post-merger object and identify regimes where these timescales are as short as the characteristic timescale ∼10 ms, and, therefore, might affect the evolution of the post-merger object. Our analysis indicates that bulk viscous damping would be important at not too high temperatures of the order of a few MeV and densities up to a few times saturation density.

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Section: Introductionmentioning

confidence: 99%

Bulk Viscous Damping of Density Oscillations in Neutron Star Mergers

2020

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“…where T and T F are the temperature of the stellar matter and the Fermi temperature of electrons, respectively. While more accurate tables are available [56], the expression above is accurate up to 10%, which exceeds the accuracy required for our qualitative estimates. The rest-mass density dependence of σ is via the Fermi temperature given by T F = 0.511 1 + (Zρ 6 /A) 2/3 − 1 MeV, where ρ 6 := ρ/(10 6 g cm −3 ).…”

Section: Estimating Magnetic Field Decay Timescalementioning

confidence: 67%

“…The conductivity tensor in a magnetic field for applications to neutron star mergers was obtained recently [22,56]. This study provides the conductivity tensor for temperatures extending up to T 10 MeV, rest-mass densities down to ρ 10 6 g cm −3 and for non-quantizing magnetic field B ≤ 10 14 G .…”

Section: Ohmic and Hall Timescalesmentioning

confidence: 85%

Electrical resistivity and Hall effect in binary neutron star mergers

et al. 2018

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We examine the range of rest-mass densities, temperatures and magnetic fields involved in simulations of binary neutron star mergers (BNSM) and identify the conditions under which the ideal magnetohydrodynamics (MHD) breaks down using recently computed conductivities of warm, magnetized plasma created in such systems. While previous dissipative MHD studies of BNSMs assumed that dissipation sets in due to low conduction at low rest-mass densities, we show that this paradigm must be shifted: the ideal MHD is applicable up to the regime where the hydrodynamic description of matter breaks down. We also find that the Hall effect can be important at low densities and low temperatures, where it can induce a non-dissipative rearrangement of the magnetic field. Finally, we mark the region in temperaturedensity plane where the hydrodynamic description breaks down.Keywords: binary neutron star mergers -magnetohydrodynamic simulations -magnetic-field decay -electrical conductivity -Hall effect arXiv:1907.05218v1 [astro-ph.HE]

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“…Applications to neutron stars and relevant transport coefficients were derived, for example, in Refs. [61][62][63]. A comprehensive review of the new developments in this field is given in Ref.…”

Section: Introductionmentioning

confidence: 99%

Phenomenological Relativistic Second-Order Hydrodynamics for Multiflavor Fluids

Harutyunyan

Sedrakian

2023

Symmetry

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In this work, we perform a phenomenological derivation of the first- and second-order relativistic hydrodynamics of dissipative fluids. To set the stage, we start with a review of the ideal relativistic hydrodynamics from energy–momentum and particle number conservation equations. We then go on to discuss the matching conditions to local thermodynamical equilibrium, symmetries of the energy–momentum tensor, decomposition of dissipative processes according to their Lorentz structure, and, finally, the definition of the fluid velocity in the Landau and Eckart frames. With this preparatory work, we first formulate the first-order (Navier–Stokes) relativistic hydrodynamics from the entropy flow equation, keeping only the first-order gradients of thermodynamical forces. A generalized form of diffusion terms is found with a matrix of diffusion coefficients describing the relative diffusion between various flavors. The procedure of finding the dissipative terms is then extended to the second order to obtain the most general form of dissipative function for multiflavor systems up to the second order in dissipative fluxes. The dissipative function now includes in addition to the usual second-order transport coefficients of Israel–Stewart theory also second-order diffusion between different flavors. The relaxation-type equations of second-order hydrodynamics are found from the requirement of positivity of the dissipation function, which features the finite relaxation times of various dissipative processes that guarantee the causality and stability of the fluid dynamics. These equations contain a complete set of nonlinear terms in the thermodynamic gradients and dissipative fluxes arising from the entropy current, which are not present in the conventional Israel–Stewart theory.

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Electrical conductivity tensor of dense plasma in magnetic fields

Cited by 3 publications

References 6 publications

Bulk Viscous Damping of Density Oscillations in Neutron Star Mergers

Bulk Viscous Damping of Density Oscillations in Neutron Star Mergers

Electrical resistivity and Hall effect in binary neutron star mergers

Phenomenological Relativistic Second-Order Hydrodynamics for Multiflavor Fluids

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