Schedule Aug 3, 2000
Thermal Energy and R-Mode Evolution
Bernard Schutz (Max-Planck, Gravity)
Discussions of r-mode spindown generally assume that the effect of the back-reaction on the star as it loses energy and angular momentum will be to spin the star down, so that we will always be dealing with an approximately axisymmetric equilibrium star with a small-ish r-mode perturbation. I examine the conditions on energy and angular momentum loss that are required for the existence of such a sequence of "background" axisymmetric models, and show that they require the viscous energy dissipation rate to be tied to the angular momentum loss rate in a particular way. It follows that this is not likely to happen, that spindown will be more complicated. I speculate on what might happen. One path would be that the system evolves into one that is stationary in a rotating frame. I show how to calculate the angular velocity of this frame from the viscous dissipation rate.

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