Speaker
Dr
Justin Elfritz
(Anton Pannekoek Institute, University of Amsterdam)
Description
State-of-the-art 2D simulations of coupled magnetic and temperature evolution have shown us that we can explain different neutron star (NS) classes by varying only magnetic field strength and geometry at birth. In this work we address evolutionary differences that arise as a consequence of including the physics driving magnetic field evolution in the NS core. Forcing in the core arises due to the interactions between superfluid neutron vortices and the entrained magnetic flux-tubes. We describe, for the first time, the results from self-consistent magneto-thermal simulations considering not only the effects of Hall-driven field dissipation in the crust, but adding a complete set of proposed driving forces in the core. We emphasize how each of these theorized processes drive magnetic evolution and affect observables, and show that when all forces are considered vectorially, the net expulsion rate is negligible, and will have no observable effect in the crust on megayear timescales.
Primary author
Dr
Justin Elfritz
(Anton Pannekoek Institute, University of Amsterdam)
Co-authors
Dr
Daniele Vigano
(CSIC-IEEC, Autonomous University of Barcelona)
Dr
Jose Pons
(Department of Applied Physics, University of Alicante)
Dr
Nanda Rea
(Anton Pannekoek Institute, University of Amsterdam)
