Non–linear magnetic field decay in neutron stars

Theory and observations

Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany

Corresponding author: U. Geppert, ugeppert@aip.de

Received: 22 April 2002
Accepted: 28 June 2002

Abstract

There exists both theoretical and observational evidence that the magnetic field decay in neutron stars may proceed in a pronounced non–linear way during a certain episode of the neutron star's life. In the presence of a strong magnetic field the Hall–drift dominates the field evolution in the crust and/or the superfluid core of neutron stars. Analysing observations of P and for sufficiently old isolated pulsars we gain strong hints for a significantly non–linear magnetic field decay. Under certain conditions with respect to the geometry and strength of a large–scale magnetic background field an instability is shown to occur which rapidly raises small–scale magnetic field modes. Their growth rates increase with the background field strength and may reach ~ 10⁴ times the ohmic decay rate. Consequences for the rotational and thermal evolution as well as for the cracking of the crust of neutron stars are discussed.