On the Origin of Pulsar and Magnetar Magnetic Fields

Abstract

In order to address the generation of neutron star magnetic fields, with particular focus on the dichotomy between magnetars and radio pulsars, we consider the properties of dynamos as inferred from other astrophysical systems. With sufficiently low (modified) Rossby number, convective dynamos are known to produce dipole-dominated fields whose strength scales with convective flux, and we argue that these expectations should apply to the convective proto-neutron stars at the centers of core-collapse supernovae. We analyze a suite of three-dimensional simulations of core collapse, featuring a realistic equation of state and full neutrino transport, in this context. All our progenitor models, ranging from 9 solar masses to 25 solar masses, including one with initial rotation, have sufficiently vigorous proto-neutron-star convection to generate dipole fields of order ~10^15 gauss, if the modified Rossby number resides in the critical range. Thus, the magnetar/radio pulsar dichotomy may arise naturally in part from the distribution of core rotation rates in massive stars.

Accepted for publication in ApJ; very minor changes from previous version

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Cited by in corpus (3)

• Angular Momentum Transport in Proto-Neutron Stars and the Fate of Neutron Star Merger Remnants
• A new scenario for magnetar formation: Tayler-Spruit dynamo in a proto-neutron star spun up by fallback
• The Early Evolution of Magnetar Rotation I: Slowly Rotating "Normal" Magnetars