2014/06/30 by Peng-Cheng Chu, Lie-Wen Chen, Xin Wang · 1 citation
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics #Condensed matter physics #Field (mathematics) #Field strength #Geometry #Geophysics and Gravity Measurements #High-pressure geophysics and materials #Magnetic field #Magnetic pressure #Magnetization #Orientation (vector space) #Perpendicular #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Stars #Strange matter #astro-ph.SR #hep-ph #nucl-ex #nucl-th
paper · pdf · doi:10.1103/physrevd.90.063013
published as Phys. Rev. D 90, 063013 (2014) · 9 pages, 4 figures. Discussions added. Accepted version to appear in PRD
arxiv created 2014/09/09 · openalex publication_date 2014/09/25 · arxiv updated 2014/10/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Within the confined isospin- and density-dependent mass model, we study the properties of strange quark matter (SQM) and quark stars (QSs) in strong magnetic fields. The equation of state of SQM under a constant magnetic field is obtained self-consistently and the pressure perpendicular to the magnetic field is shown to be larger than that parallel to the magnetic field, implying that the properties of magnetized QSs generally depend on both the strength and the orientation of the magnetic fields distributed inside the stars. Using a density-dependent magnetic field profile which is introduced to mimic the magnetic field strength distribution in a star, we study the properties of static spherical QSs by assuming two extreme cases for the magnetic field orientation in the stars, i.e., the radial orientation in which the local magnetic fields are along the radial direction, and the transverse orientation in which the local magnetic fields are randomly oriented but perpendicular to the radial direction. Our results indicate that including the magnetic fields with radial (transverse) orientation can significantly decrease (increase) the maximum mass of QSs, demonstrating the importance of the magnetic field orientation inside the magnetized compact stars.