Hydromagnetic stability of differentially rotating neutron stars

Details Hydromagnetic stability of differentially rotating neutron stars Hydromagnetic stability of differentially rotating neutron stars

Nov 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003a%26a...410..975u&link_type=abstract

Astronomy and Astrophysics, v.410, p.975-981 (2003)

Astronomy and Astrophysics

Astrophysics

2

Magnetohydrodynamics (Mhd), Stars: Neutron, Stars: Rotation, Stars: Pulsars: General

Scientific paper

The stability properties of differentially rotating magnetic neutron stars are considered, and the instability criteria are obtained. The influence of the magnetic field is twofold: it may stabilize a fluid against some instabilities, on the one hand, and it can lead to new branches of instabilities, on the other hand. It turns out that some of the instability criteria of magnetic neutron stars can be satisfied at smaller departures from the uniform rotation than the criteria of non-magnetic stars. Interaction of hydrodynamic motions caused by instabilities in the core with the neutron star crust can result in small irregularities in the measured spin period of pulsars.

Affiliated with

Also associated with

No associations

Rating

Hydromagnetic stability of differentially rotating neutron stars 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 Hydromagnetic stability of differentially rotating neutron stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Hydromagnetic stability of differentially rotating neutron stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1086195