Magnetar formation through a convective dynamo in protoneutron stars

Abstract

The release of spin-down energy by a magnetar is a promising scenario to power several classes of extreme explosive transients. However, it lacks a firm basis because magnetar formation still represents a theoretical challenge. Using the first three-dimensional simulations of a convective dynamo based on a protoneutron star interior model, we demonstrate that the required dipolar magnetic field can be consistently generated for sufficiently fast rotation rates. The dynamo instability saturates in the magnetostrophic regime with the magnetic energy exceeding the kinetic energy by a factor of up to 10. Our results are compatible with the observational constraints on galactic magnetar field strength and provide strong theoretical support for millisecond protomagnetar models of gamma-ray burst and superluminous supernova central engines.

6 pages, 4 figures

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• Millisecond Magnetars
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• The Early Evolution of Magnetar Rotation I: Slowly Rotating "Normal" Magnetars
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• Exploring Supernova Gravitational Waves with Machine Learning
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• A Flat-Spectrum Radio Transient at 122 Mpc consistent with an Emerging Pulsar Wind Nebula
• The rocket effect mechanism in neutron stars in supernova remnants
• Magnetar central engines in gamma-ray busts follow the universal relation of accreting magnetic stars
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• Magnetorotational neutron star kicks
• Tayler-Spruit dynamo in binary neutron star merger remnants
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• Multipolar Electromagnetic Emission of Newborn Magnetar
• Magnetar field dynamics shaped by chiral anomalies and helicity
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