Thermal Conductivity of Superfluid Neutron Stars

Shahzamanian, M. A.; Yavary, H.

doi:10.1142/s0218271805005840

Cited by 2 publications

(3 citation statements)

References 17 publications

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“…In the context of neutron stars, this was not studied in detail (see however Refs. [213,214]). A thorough investigation of the Bogoliubov quasiparticle contribution to transport coefficients remains an open problem, but the key features at low temperatures can be worked out, neglecting all the modifications to the quasiparticle collision integral except the spectrum modification by the gap (for the neutron thermal conductivity this was done by Baiko et al [186]).…”

Section: Effects Of Cooper Pairingmentioning

confidence: 99%

Reaction Rates and Transport in Neutron Stars

Schmitt

Shternin

2018

Astrophysics and Space Science Library

100

122

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Understanding signals from neutron stars requires knowledge about the transport inside the star. We review the transport properties and the underlying reaction rates of dense hadronic and quark matter in the crust and the core of neutron stars and point out open problems and future directions. arXiv:1711.06520v3 [astro-ph.HE] 29 Oct 2018 65 References 66 I. INTRODUCTION A. ContextTransport describes how conserved quantities such as energy, momentum, particle number, or electric charge are transferred from one region to another. Such a transfer occurs if the system is out of equilibrium, for instance through a temperature gradient or a non-uniform chemical composition. Different theoretical methods are used to understand transport, depending on how far the system is away from its equilibrium state. If the system is close to equilibrium locally and perturbations are on large scales in space and time, hydrodynamics is a powerful technique. Further away from equilibrium other techniques are required, for example kinetic theory, which can also be used to provide the transport coefficients needed in the hydrodynamic equations. In any case, transport is determined by interactions on a microscopic level, and it is the resulting transport properties that we are concerned with in this review.Signals from neutron stars are sensitive to equilibrium properties such as the equation of state but also, to a large extent, to transport properties -here, by neutron stars we mean all objects with a radius of about 10 km and a mass of about 1-2 solar masses, including the possibilities of hybrid stars, which have a quark matter core, and pure quark stars. Therefore, understanding transport is crucial to interpret astrophysical observations, and, turning the argument around, we can use astrophysical observations to improve our understanding of transport in dense matter and thus ultimately our understanding of the microscopic interactions.Transport properties are most commonly computed from particle collisions. (Although, in strongly coupled systems, the picture of well-defined particles scattering off each other has to be taken with care.) These can be scattering processes in which energy and momentum is exchanged without changing the chemical composition of the system, or these can be flavor-changing processes from the electroweak interaction. Understanding transport thus amounts to understanding the rates of these processes, as a function of temperature and density. Electroweak processes are well understood, but large uncertainties arise if the strong interaction is involved in a reaction that contributes to transport. Therefore, approximations such as weak-coupling techniques or one-pion exchange for nucleon-nucleon collisions are being used, and efforts in current research aim at improving these approximations.In a neutron star, most of the particles involved in these processes are fermions: electrons, muons, neutrinos, neutrons, protons, hyperons, and quarks. Since the Fermi momenta of these fermions are typically much larger tha...

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Section: Effects Of Cooper Pairingmentioning

confidence: 99%

Reaction Rates and Transport in Neutron Stars

Schmitt

Shternin

2018

Astrophysics and Space Science Library

100

122

View full text Add to dashboard Cite

show abstract

“…At low temperatures, only the binary processes are dominated and other transition probabilities have nearly zero value. [9] In other words, we have W 22 . The potential in Eq.…”

Section: Transition Probabilitiesmentioning

confidence: 99%

“…Transport properties of different superfluids have been studied in various regimes, such as BEC-BCS crossover or Feshbach resonance. [2] In the field of astrophysics, the thermal conductivity of a superfluid neutron stars has been calculated by shahzamanian et al [9] Sawkey et al [10] have presented the first measurements of the thermal conductivity of spin-polarized normal liquid 3 He.…”

Section: Introductionmentioning

confidence: 99%