Abstract
In this article, we calculate the magnetization and other thermodynamical quantities for strongly magnetized quark matter within the Nambu-Jona-Lasinio model at zero temperature. We assume two scenarios, chemically equilibrated charge neutral matter present in the interior of compact stars and zero-strangeness isospin-symmetric matter created in nuclear experiments. We show that the magnetization oscillates with density but in a much more smooth form than what was previously shown in the literature. As a consequence, we do not see the unphysical behavior in the pressure in the direction perpendicular to the magnetic field that was previously found. Finally, we also analyze the effects of a vector interaction on our results.
Highlights
Understanding dense and/or hot matter in the presence of strong magnetic fields is one of the most important challenges of nuclear physics today
We do not see the unphysical behavior in the pressure in the direction perpendicular to the magnetic field that was previously found
We showed that the inclusion of magnetic fields in quark matter within the Nambu–Jona-Lasinio formalism does not generate the unphysical behavior previously found in Refs. [31,32] for the magnetization and pressure in the direction perpendicular to the magnetic field
Summary
Understanding dense and/or hot matter in the presence of strong magnetic fields is one of the most important challenges of nuclear physics today. Extremely high magnetic fields have been estimated to be briefly created in relativistic heavy-ion collisions [1,2,3,4,5], with strengths of up to 1019 and 1020 G expected to be generated during noncentral heavy-ion collisions at the BNL Relativistic Heavy Ion Collider (RHIC) and at European Organization for Nuclear Research (CERN), respectively In this regime, the role played by magnetic fields in quark deconfinement and chiral symmetry restoration can, to some extent, be extracted from lattice QCD data. These estimates have motivated a large amount of research on the issue of how magnetic fields modify the microscopic structure (represented in the equation of state) and the macroscopic structure (obtained from the solution of the Einstein-Maxwell equations) of neutron stars In this regime, there is no guidance from lattice QCD concerning the effect of magnetic fields on deconfined quark matter. We verify that our conclusions hold even when vector interactions (which allow us to reproduce astrophysical constraints) are added to the model
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