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Transport coefficients of two-flavor superconducting quark matter

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abstract

Background: The two-flavor color superconducting (2SC) phase of quark matter is a possible constituent of the core of neutron stars. To assess its impact on the observable behavior of the star one must analyze transport properties, which in 2SC matter are controlled by the scattering of gapless fermionic modes by each other and possibly also by color-magnetic flux tubes. Purpose: We determine the electrical and thermal conductivities and the shear viscosity of 2SC matter. Methods: We use a variational formulation of transport theory, treating the strong and electromagnetic interactions via a weak coupling expansion. Results: We provide the leading order scaling of the transport coefficients with temperature and chemical potential as well as accurate fits to our numerical results. We also find that the scattering of fermions by color-magnetic flux tubes is insignificant for thermal conductivity, but may contribute to the electrical conductivity and shear viscosity in the limit of very low temperature or high magnetic field. We also estimate the transport coefficients in unpaired quark matter. Conclusions: Our calculation has set the stage for exploration of possible signatures of the presence of 2SC quark matter in neutron stars.

fields

astro-ph.HE 1

years

2026 1

verdicts

UNVERDICTED 1

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Modelling Dissipative Dynamics of r-mode Instability in Hybrid Stars

astro-ph.HE · 2026-06-25 · unverdicted · novelty 4.0

Bayesian inference on observational data yields shear viscosity timescale τ_s=(4.99^{+0.49}_{-0.52})×10^8 T^{5/3} s and bulk viscosity timescale for two-layer hybrid stars, giving frequency minima of 451.87 Hz and 517.47 Hz that explain stability of pulsars including XTE J0929-314.

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  • Modelling Dissipative Dynamics of r-mode Instability in Hybrid Stars astro-ph.HE · 2026-06-25 · unverdicted · none · ref 18 · internal anchor

    Bayesian inference on observational data yields shear viscosity timescale τ_s=(4.99^{+0.49}_{-0.52})×10^8 T^{5/3} s and bulk viscosity timescale for two-layer hybrid stars, giving frequency minima of 451.87 Hz and 517.47 Hz that explain stability of pulsars including XTE J0929-314.