Effect of Magnetic Field on Particle Emission from the Surface of Neutron Star

Studying the effect of magnetic fields on particle emission from the surface of neutron stars is vital for advancing our understanding of neutron star physics and high-energy astrophysical processes. One of the main topics in pulsar magnetospheric physics is the particle emission from neutron stars surface. This study investigates the role of multipolar magnetic fields in neutron star (NS) emission physics by incorporating higher-order field components into the standard dipole model. While past studies have primarily relied on a dipolar field configuration, recent observations suggest the presence of multipole components that significantly influence emission processes. Our findings show that higher-order multipole magnetic fields shape localized particle emission regions near the NS surface, while the dipole field dominates at larger distances. By considering the NS’s crust and superfluid core structure, as well as the effects of rapid rotation, we refine the understanding of magnetic field topologies and their impact on radiation mechanisms. This study highlights the necessity of incorporating multipolar magnetic fields for accurate modeling of pulsar and magnetar emissions. By investigating these effects, particularly the role of multipolar magnetic field components, researchers can refine theoretical models of emission mechanisms that go beyond the classical dipole framework. This has significant implications for interpreting observations of pulsars and magnetars, whose emission patterns, spectral features, and temporal variability often demand more complex field geometries. Furthermore, understanding particle emission driven by magnetic fields offers insight into neutron star spin-down evolution, magnetic field decay, and energy loss processes. Future work will involve detailed numerical simulations incorporating general relativistic effects and magnetosphere-plasma interactions.