Help Privacy Policy Disclaimer
  Advanced SearchBrowse




Journal Article

Magnetar formation through a convective dynamo in protoneutron stars


Janka,  Hans-Thomas
Stellar Astrophysics, MPI for Astrophysics, Max Planck Society;

External Resource
No external resources are shared
Fulltext (restricted access)
There are currently no full texts shared for your IP range.
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available

Raynaud, R., Guilet, J., Janka, H.-T., & Gastine, T. (2020). Magnetar formation through a convective dynamo in protoneutron stars. Science Advances, 6(11): eaay2732. doi:10.1126/sciadv.aay2732.

Cite as: https://hdl.handle.net/21.11116/0000-0006-79BB-0
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.