Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..aprn17032m&link_type=abstract
American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As
Astronomy and Astrophysics
Astrophysics
Scientific paper
The r-mode oscillations (Rossby waves) of rapidly spinning young neutron stars have been proposed as a promising source of detectable gravitational radiation. The magnetic fields of such stars may influence significantly the velocity field and time evolution of these oscillations. We show that the r-waves of a thin spherical shell of rotating fluid quite generally produce kinematic and dynamic fluid drifts that amplify the star's magnetic field. This effect occurs for any initial magnetic field geometry. In the shell model, the amplified magnetic field eventually becomes strong enough to alter substantially the velocity field and other properties of the normal modes. Our results indicate that for weakly non-linear r-waves (δ v/Ω R ~ 0.1, where δ v is the wave velocity and Ω and R are the angular frequency and radius of the star), interaction between the fluid motion and the star's magnetic field produces long-period non-linear oscillations in the velocity pattern and the direction of the differential fluid drift. For stronger waves, the resulting tangling and reconnection of the magnetic field may cause significant damping of the wave motion.
Chen Yun
Lamb Frederick
Markovic Draza
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