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R-Mode Oscillations in Rotating Magnetic Neutron Stars | | Luciano Rezzolla
; Frederick K. Lamb
; Stuart L. Shapiro
; | | Date: |
10 Nov 1999 | | Journal: | Astrophys.J. 531 (2000) L141-144 | | Subject: | astro-ph gr-qc | | Affiliation: | 1,2,4), Frederick K. Lamb (1,2,3), Stuart L. Shapiro (1,2,3,4) ( U. Illinois Center for Theoretical Astrophysics, U. Illinois Physics Dept., U. Illinois Astronmy Dept., U. Illinois NCSA | | Abstract: | We show that r-mode oscillations distort the magnetic fields of neutron stars and that their occurrence is likely to be limited by this interaction. If the field is gtrsim 10^{16} (Omega/Omega_B) G, where Omega and Omega_B are the angular velocities of the star and at which mass shedding occurs, r-mode oscillations cannot occur. Much weaker fields will prevent gravitational radiation from exciting r-mode oscillations or damp them on a relatively short timescale by extracting energy from the modes faster than gravitational wave emission can pump energy into them. For example, a 10^{10} G poloidal magnetic field that threads the star’s superconducting core is likely to prevent the ell=2 mode from being excited unless Omega exceeds 0.35 Omega_B. If Omega is larger than 0.35 Omega_B initially, the ell=2 mode may be excited but is likely to decay rapidly once Omega falls below 0.35 Omega_B, which happens in lesssim 15^d if the saturation amplitude is gtrsim 0.1. The r-mode oscillations may play an important role in determining the structure of neutron star magnetic fields. | | Source: | arXiv, astro-ph/9911188 | | Services: | Forum | Review | PDF | Favorites | |
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