Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994mnras.267..523m&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Vol. 267, NO. 3/APR1, P. 523, 1994
Astronomy and Astrophysics
Astronomy
13
Mhd - Stars: Magnetic Fields - Stars: Neutron
Scientific paper
We calculate the decay of the magnetic field in a neutron star crust, with allowance for the Hall effect. The magnetic field is represented by the large-scale (dipole and quadrupole) poloidal modes initially confined to the outer crust, as well as the toroidal component wound around the core of the neutron star. We perform our calculations using rapid and relatively slow cooling histories, both implying the possibility of a direct Urca process in the core. At the late stages, after ˜108 yr, the poloidal modes become strongly coupled (due to the Hall term in the conductivity tensor) to each other via the toroidal component. We show that this coupling may strongly affect the subsequent evolution of poloidal modes. In particular, we demonstrate that the presence of an initially very weak quadrupole mode substantially modifies the evolution of the dipole mode. Also, we have found that at t≳109 yr sign reversal of the poloidal modes may occur.
No associations
LandOfFree
Magnetic Field Evolution in Neutron Stars - Coupling Between Poloidal and Toroidal Components in the Crust does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Magnetic Field Evolution in Neutron Stars - Coupling Between Poloidal and Toroidal Components in the Crust, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Magnetic Field Evolution in Neutron Stars - Coupling Between Poloidal and Toroidal Components in the Crust will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1260128