The Magnetic Field Distribution in Strongly Magnetized Neutron Stars
arXiv:1709.01914 · doi:10.1002/asna.201713434
Abstract
In this work, we expand on a previously reported realistic calculation of the magnetic field profile for the equation of state inside strongly magnetized neutron stars. In addition to showing that magnetic fields increase quadratically with increasing baryon chemical potential of magnetized matter (instead of exponentially, as previously assumed), we show here that the magnetic field increase with baryon number density is more complex and harder to model. We do so by the analysis of several different realistic models for the microscopic description of matter in the star (including hadronic, hybrid and quark models) combined with general relativistic solutions by solving Einstein-Maxwell's field equations in a self-consistent way for stars endowed with a poloidal magnetic field.
arXiv commentProceedings of the 4th Caribbean Symposium on Cosmology, Gravitation, Nuclear and Astroparticle Physics (STARS2017) and 5th International Symposium on Strong Electromagnetic Fields and Neutron Stars (SMFNS2017)
References in corpus (7)
- QCD Phenomenology based on a Chiral Effective Lagrangian
- Quantizing magnetic field and quark-hadron phase transition in a neutron star
- A Novel Approach to Model Hybrid Stars
- Hybrid Stars in a Strong Magnetic Field
- Bumpy Spin-Down of Anomalous X-Ray Pulsars: The Link with Magnetars
- Many-body forces in the equation of state of hyperonic matter
- What is the magnetic field distribution for the equation of state of magnetized neutron stars?
Cited by in corpus (6)
- Constraining strangeness in dense matter with GW170817
- Magnetic field distribution in magnetars
- Structure of ultra-magnetised neutron stars
- Massive neutron stars as mass gap candidates: Exploring equation of state and magnetic field
- Effects of Landau quantization on neutrino emission and absorption
- Structural Properties of Magnetized Neutron Stars under f (R, T ) Gravity Framework