We analyse viscous damping of nonradial oscillations of relativistic superfluid neutron stars. To this aim the approximate method, first suggested in Gusakov & Kantor (2011), and based on the decoupling of superfluid and normal oscillation modes, is extended to account for dissipation. Frequency spectrum and damping times are calculated for oscillation modes with multipolarities l = 0, 1, 2, and 3. All calculations are made self-consistently within the finite temperature superfluid hydrodynamics. For the first time it is shown that viscous damping of normal modes can be much more effective in certain stages of neutron-star thermal evolution, than it is commonly assumed.
Nucleon Superfluidity and its Influence on Damping of Neutron Star Oscillations / E. M., Kantor; M. E., Gusakov; A. I., Chugunov; Gualtieri, Leonardo. - 466:(2012), pp. 223-224. (Intervento presentato al convegno Electromagnetic Radiation from Pulsars and Magnetars tenutosi a Zielona Góra, Poland nel 24-27 April 2012).
Nucleon Superfluidity and its Influence on Damping of Neutron Star Oscillations
GUALTIERI, Leonardo
2012
Abstract
We analyse viscous damping of nonradial oscillations of relativistic superfluid neutron stars. To this aim the approximate method, first suggested in Gusakov & Kantor (2011), and based on the decoupling of superfluid and normal oscillation modes, is extended to account for dissipation. Frequency spectrum and damping times are calculated for oscillation modes with multipolarities l = 0, 1, 2, and 3. All calculations are made self-consistently within the finite temperature superfluid hydrodynamics. For the first time it is shown that viscous damping of normal modes can be much more effective in certain stages of neutron-star thermal evolution, than it is commonly assumed.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
