2009/03/13 by Carmine Cuofano, A. Drago, Alessandro Drago
Earth and Planetary Sciences · Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Differential rotation #Gravitational wave #High-pressure geophysics and materials #Magnetar #Magnetic field #Millisecond #Millisecond pulsar #Neutron star #Physics #Pulsar #Pulsars and Gravitational Waves Research #Stars #astro-ph.HE
paper · pdf · doi:10.1088/1742-6596/168/1/012008
6 pages, 3 figures, Proceedings conference "Theoretical Nuclear Physics", Cortona October 2008
arxiv created 2009/03/13 · openalex publication_date 2009/05/01 · arxiv updated 2015/05/12 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
In millisecond pulsars the existence of the Coriolis force allows the development of the so-called Rossby oscillations (r-modes) which are know to be unstable to emission of gravitational waves. These instabilities are mainly damped by the viscosity of the star or by the existence of a strong magnetic field. A fraction of the observed millisecond pulsars are known to be inside Low Mass X-ray Binaries (LMXBs), systems in which a neutron star (or a black hole) is accreting from a donor whose mass is smaller than 1 M ⊙ . Here we show that the r-mode instabilities can generate strong toroidal magnetic fields by inducing differential rotation. In this way we also provide an alternative scenario for the origin of the magnetars.