Thermal Energy and R-Mode Evolution

Details Thermal Energy and R-Mode Evolution Thermal Energy and R-Mode Evolution

Aug 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000rmns.proge..12s&link_type=abstract

Presented at the KITP Miniprogram: R-Modes in Neutron Stars, Aug 3, 2000, Kavli Institute for Theoretical Physics, University of

Physics

Scientific paper

Discussions of r-mode spindown generally assume that the effectof the back-reaction on the star as it loses energy and angularmomentum will be to spin the star down, so that we will alwaysbe dealing with an approximately axisymmetric equilibrium starwith a small-ish r-mode perturbation. I examine the conditionson energy and angular momentum loss that are required for theexistence of such a sequence of "background" axisymmetric models,and show that they require the viscous energy dissipation rate to betied to the angular momentum loss rate in a particular way. Itfollows that this is not likely to happen, that spindown willbe more complicated. I speculate on what might happen. Onepath would be that the system evolves into one that is stationaryin a rotating frame. I show how to calculate the angular velocityof this frame from the viscous dissipation rate.

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