Volume 392, Number 3, September IV 2002
|Page(s)||1015 - 1024|
|Section||Interstellar and circumstellar matter|
|Published online||09 September 2002|
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, email@example.com
Accepted: 28 June 2002
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.
Key words: stars: neutron / stars: magnetic fields / stars: evolution / stars: pulsars: general
© ESO, 2002
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