Protoneutron Star Dynamo:. Theory and Observations

Details Protoneutron Star Dynamo:. Theory and Observations Protoneutron Star Dynamo:. Theory and Observations

Feb 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008esnm.conf..155b&link_type=abstract

EXOTIC STATES OF NUCLEAR MATTER. Proceedings of the International Symposium EXOCT07. Held 11-15 June 2007 in Catania University,

Physics

Scientific paper

We briefly review the turbulent mean-field dynamo action in protoneutron stars that are subject to convective and neutron finger instabilities during the early evolutionary phase. By solving the mean-field induction equation with the simplest model of α-quenching we estimate the strength of the generated magnetic field. If the initial period of the protoneutron star is short, then the generated large-scale field is very strong (> 3 × 1013G) and exceeds the small-scale field at the neutron star surface, while if the rotation is moderate, then the pulsars are formed with more or less standard dipole fields (< 3 × 1013G) but with surface small-scale magnetic fields stronger than the dipole field. If rotation is very slow, then the mean-field dynamo does not operate, and the neutron star has no global field.

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