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Neutrino Propagation In Color Superconducting Quark Matter

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arxiv hep-ph/0005228 v1 pith:LKUE4LG5 submitted 2000-05-23 hep-ph astro-phnucl-th

Gregory W. Carter , Sanjay Reddy This is my paper · ORCID
classification hep-phastro-phnucl-th
keywords matterquarkneutrinophasesuperconductingcoolingcolorearly
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abstract

We calculate the neutrino mean free path in color superconducting quark matter, and employ it to study the cooling of matter via neutrino diffusion in the superconducting phase as compared to a free quark phase. The cooling process slows when quark matter undergoes a second order phase transition to a superconducting phase at the critical temperature $T_c$. Cooling subsequently accelerates as the temperature decreases below $T_c$. This will directly impact the early evolution of a newly born neutron star should its core contain quark matter. Consequently, there may be observable changes in the early neutrino emission which would provide evidence for superconductivity in hot and dense matter.

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Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Neutrino absorption in two-flavor color-superconducting quark matter

    nucl-th 2025-09 conditional novelty 7.0 of 10

    In 2SC quark matter, neutrino absorption is dominated by strange-quark capture at low temperature, and a degenerate neutrino gas at electron lepton fraction 0.1 has a mean free path of meters or less.

  2. The petit four of color-superconducting phases in proto-neutron star evolution

    nucl-th 2026-07 conditional novelty 6.0 of 10

    Along constant-baryon-number cooling tracks, color-superconducting cores in proto-neutron stars follow four scenarios, with stable cold CSC only in a narrow high-mass band for the chosen EoS.

  3. Determining the minimal mass of a proto-neutron star with chirally constrained nuclear equations of state

    nucl-th 2024-11 conditional novelty 6.0 of 10

    For chirally constrained nuclear equations of state, the minimal proto-neutron star mass is about 0.62 solar masses with trapped neutrinos (YL=0.4, s=1) and about 0.22 solar masses after deleptonization (s=2).

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