Dissipative relativistic magnetohydrodynamics of a multicomponent mixture and its application to neutron stars

Dommes, Vasiliy A.; Gusakov, M. E.; Shternin, P. S.

doi:10.1103/physrevd.101.103020

Cited by 28 publications

(30 citation statements)

References 73 publications

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“…The momentum transfer rates mediated by the electromagnetic interactions can be calculated following the expressions in Refs. [42,73]. They are several orders of magnitude smaller than J ci mediated by the strong interaction, and we do not show them here.…”

Section: Transport Coefficientscontrasting

confidence: 64%

“…For instance, the momentum transfer rates as calculated here constitute the microphysical input for the magnetic field evolution studies, see, e.g., Ref. [41,42]. Large fields, e.g., 10 14 G, may affect the polarization tensor of the plasma making the scattering of the charged particles due to electromagnetic interactions anisotropic.…”

Section: Discussionmentioning

confidence: 97%

“…If the diffusion is caused by the external electromagnetic field, these coefficients enter the generalized Ohm law and determine the electrical conductivity, which is important for studies of the magnetic field evolution of NSs, see, e.g., Refs. [39][40][41][42]. Our results are based on the classical formalism of the kinetic theory of Fermi systems [43] adapted for the NS context, see Refs.…”

Section: Introductionmentioning

confidence: 99%

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Transport Coefficients of Hyperonic Neutron Star Cores

Shternin

Vidaña

2021

Universe

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We consider transport properties of the hypernuclear matter in neutron star cores. In particular, we calculate the thermal conductivity, the shear viscosity, and the momentum transfer rates for npΣ−Λeμ composition of dense matter in β–equilibrium for baryon number densities in the range 0.1–1 fm−3. The calculations are based on baryon interactions treated within the framework of the non-relativistic Brueckner-Hartree-Fock theory. Bare nucleon-nucleon (NN) interactions are described by the Argonne v18 phenomenological potential supplemented with the Urbana IX three-nucleon force. Nucleon-hyperon (NY) and hyperon-hyperon (YY) interactions are based on the NSC97e and NSC97a models of the Nijmegen group. We find that the baryon contribution to transport coefficients is dominated by the neutron one as in the case of neutron star cores containing only nucleons. In particular, we find that neutrons dominate the total thermal conductivity over the whole range of densities explored and that, due to the onset of Σ− which leads to the deleptonization of the neutron star core, they dominate also the shear viscosity in the high density region, in contrast with the pure nucleonic case where the lepton contribution is always the dominant one.

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Section: Transport Coefficientscontrasting

confidence: 64%

Section: Discussionmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

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Transport Coefficients of Hyperonic Neutron Star Cores

Shternin

Vidaña

2021

Universe

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“…The model remains non-singular as long as v n i approaches v s i sufficiently fast as the critical temperature is approached. More detailed discussions of entrainment and finite temperature superfluids can be found in Andersson et al (2013), Gusakov and Andersson (2006), Kantor and Gusakov (2011), Gusakov et al (2009), Gusakov and Haensel (2005), Leinson (2018), Dommes et al (2020) and Rau and Wasserman (2020).…”

Section: Helium: the Original Two-fluid Modelmentioning

confidence: 99%

Relativistic fluid dynamics: physics for many different scales

Andersson

Comer

2021

Living Rev Relativ

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The relativistic fluid is a highly successful model used to describe the dynamics of many-particle systems moving at high velocities and/or in strong gravity. It takes as input physics from microscopic scales and yields as output predictions of bulk, macroscopic motion. By inverting the process—e.g., drawing on astrophysical observations—an understanding of relativistic features can lead to insight into physics on the microscopic scale. Relativistic fluids have been used to model systems as “small” as colliding heavy ions in laboratory experiments, and as large as the Universe itself, with “intermediate” sized objects like neutron stars being considered along the way. The purpose of this review is to discuss the mathematical and theoretical physics underpinnings of the relativistic (multi-) fluid model. We focus on the variational principle approach championed by Brandon Carter and collaborators, in which a crucial element is to distinguish the momenta that are conjugate to the particle number density currents. This approach differs from the “standard” text-book derivation of the equations of motion from the divergence of the stress-energy tensor in that one explicitly obtains the relativistic Euler equation as an “integrability” condition on the relativistic vorticity. We discuss the conservation laws and the equations of motion in detail, and provide a number of (in our opinion) interesting and relevant applications of the general theory. The formalism provides a foundation for complex models, e.g., including electromagnetism, superfluidity and elasticity—all of which are relevant for state of the art neutron-star modelling.

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“…While viscous effects might also be important in black-hole accretion problems [75], the presence of magnetic fields introduces anisotropies in the dissipative sector presently unaccounted for in BDNK theory [38,73]. Although first-order formulations of dissipative MHD have been proposed [76], their extension to general hydrodynamic frames has just started to be investigated [77].…”

Section: Discussionmentioning

confidence: 99%

Conservative finite volume scheme for first-order viscous relativistic hydrodynamics

Pandya,

Most,

Pretorius

2022

Preprint

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We present the first conservative finite volume numerical scheme for the causal, stable relativistic Navier-Stokes equations developed by Bemfica, Disconzi, Noronha, and Kovtun (BDNK). BDNK theory has arisen very recently as a promising means of incorporating entropy-generating effects (viscosity, heat conduction) into relativistic fluid models, appearing as a possible alternative to the so-called Müller-Israel-Stewart (MIS) theory successfully used to model quark-gluon plasma. Both BDNK and MIS-type theories may be understood in terms of a gradient expansion about the perfect (ideal) fluid, wherein BDNK arises at first order and MIS at second order. As such, BDNK has vastly fewer terms and undetermined model coefficients (as is typical for an effective field theory appearing at lower order), allowing for rigorous proofs of stability, causality, and hyperbolicity in full generality which have as yet been impossible for MIS. To capitalize on these advantages, we present the first fully conservative multi-dimensional fluid solver for the BDNK equations suitable for physical applications. The scheme includes a flux-conservative discretization, non-oscillatory reconstruction, and a central-upwind numerical flux, and is designed to smoothly transition to a high-resolution shock-capturing perfect fluid solver in the inviscid limit. We assess the robustness of our new method in a series of flat-spacetime tests for a conformal fluid, and provide a detailed comparison with previous approaches of Pandya & Pretorius (2021) [1].

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Dissipative relativistic magnetohydrodynamics of a multicomponent mixture and its application to neutron stars

Cited by 28 publications

References 73 publications

Transport Coefficients of Hyperonic Neutron Star Cores

Transport Coefficients of Hyperonic Neutron Star Cores

Relativistic fluid dynamics: physics for many different scales

Conservative finite volume scheme for first-order viscous relativistic hydrodynamics

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