1999/11/30 by Luciano Rezzolla, Frederick K. Lamb, Stuart L. Shapiro · 2 citations
Engineering · Physics and Astronomy · #Amplitude #Astrophysics #Atomic and Subatomic Physics Research #Atomic physics #Excited state #Geophysics and Sensor Technology #Gravitational wave #Magnetic field #Mode (computer interface) #Neutron star #Optics #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Saturation (graph theory) #Stars #astro-ph #gr-qc
paper · pdf · doi:10.1086/312539
published as Astrophys.J. 531 (2000) L141-144 · 4 pages, 1 postscript figure, uses emulateapj; submitted to ApJ Letters 1999 Nov 8; accepted 2000 Jan 25; this version is essentially identical to the original version except that Figure 2 was deleted in order to fit within the ApJ Letters page limit
arxiv created 2000/01/26 · openalex publication_date 2000/03/10 · arxiv updated 2009/11/30 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
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 greater, similar1016(Omega/OmegaB) G, where Omega and OmegaB 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 will 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 1010 G poloidal magnetic field that threads the star's superconducting core is likely to prevent the l=2 mode from being excited unless Omega exceeds 0.35OmegaB. If Omega is larger than 0.35OmegaB initially, the l=2 mode may be excited but is likely to decay rapidly once Omega falls below 0.35OmegaB, which happens in less, similar15 days if the saturation amplitude is greater, similar0.1. The r-mode oscillations may play an important role in determining the structure of neutron star magnetic fields.