Abstract
We study the anomalous electromagnetic transport properties of a quark-matter phase that can be realized in the presence of a magnetic field in the low-temperature/moderate-high-density region of the Quantum Chromodynamics (QCD) phase map. In this so-called Magnetic Dual Chiral Density Wave phase, an inhomogeneous condensate is dynamically induced producing a nontrivial topology, a consequence of the asymmetry of the lowest Landau level modes of the quasiparticles in this phase. The nontrivial topology manifests in the electromagnetic effective action via a chiral anomaly term θ F μ ν F ˜ μ ν , with an axion field θ given by the phase of the Dual Chiral Density Wave condensate. The coupling of the axion with the electromagnetic field leads to several macroscopic effects that include, among others, an anomalous, nondissipative Hall current, an anomalous electric charge, magnetoelectricity, and the formation of a hybridized propagating mode known as an axion polariton. The possible existence of this phase in the inner core of neutron stars opens a window to search for signals of its anomalous transport properties.
Highlights
Neutron stars, the remnants of supernova collapse, are very dense objects produced by the gravitational colapse of very massive stars
To the best of our knowledge, the question of which color superconductivity (CS) phase is the most favorable in the region of intermediate densities still remains unanswered. In addition to their high densities, neutron stars typically have strong magnetic fields, which become extremely large in the case of magnetars, with inner values that have been estimated to range from 1018 G for nuclear matter [72] to 1020 G for quark matter [73]
The system under study has a non-trivial topology, which is due to the combined effect of a ground state having an inhomogeneous particle-hole condensate and the dimensional reduction affecting the quasiparticles occupying the LLL
Summary
The remnants of supernova collapse, are very dense objects produced by the gravitational colapse of very massive stars (stars with masses between 10 and 30 solar masses). Even assuming that neutron stars can realize a quark phase, this does not take place at asymptotically large densities Their location in the QCD phase map will better correspond to the low-temperature, intermediate-density region. To the best of our knowledge, the question of which CS phase is the most favorable in the region of intermediate densities still remains unanswered In addition to their high densities, neutron stars typically have strong magnetic fields, which become extremely large in the case of magnetars, with inner values that have been estimated to range from 1018 G for nuclear matter [72] to 1020 G for quark matter [73]. This opens the possibility to take advantage of new understandings within these materials to infer potentially measurable effects in the MDCDW phase of quark matter, and use that insight to design clever ways to probe the presence of this quark phase in neutron stars
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