Astronomy and Astrophysics – Astrophysics – General Relativity and Quantum Cosmology
Scientific paper
2001-07-17
Phys. Rev. D, 64 104014 (2001)
Astronomy and Astrophysics
Astrophysics
General Relativity and Quantum Cosmology
16 pages, 12 figures. To appear in Phys. Rev. D
Scientific paper
10.1103/PhysRevD.64.104014
The evolution of the r-mode instability is likely to be accompanied by secular kinematic effects which will produce differential rotation with large scale drifts of fluid elements, mostly in the azimuthal direction. As first discussed by Rezzolla, Lamb and Shapiro 2000, the interaction of these secular velocity fields with a pre-existing neutron star magnetic field could result in the generation of intense and large scale toroidal fields. Following their derivation in the companion paper, we here discuss the numerical solution of the evolution equations for the magnetic field. The values of the magnetic fields obtained in this way are used to estimate the conditions under which the r-mode instability might be prevented or suppressed. We also assess the impact of the generation of large magnetic fields on the gravitational wave detectability of r-mode unstable neutron stars. Our results indicate that the signal to noise ratio in the detection of gravitational waves from the r-mode instability might be considerably decreased if the latter develops in neutron stars with initial magnetic fields larger than 10^10 G.
Lamb Frederick L.
Markovic Dragoljub
Rezzolla Luciano
Shapiro Stuart L.
No associations
LandOfFree
Properties of r modes in rotating magnetic neutron stars. II. Evolution of the r modes and stellar magnetic field 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 Properties of r modes in rotating magnetic neutron stars. II. Evolution of the r modes and stellar magnetic field, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Properties of r modes in rotating magnetic neutron stars. II. Evolution of the r modes and stellar magnetic field will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-642664