Schedule Aug 3, 2000
How Can R-Mode Heating Prevent Crust Formation?
Benjamin Owen (Max-Planck, Gravity)
Nine months ago, Lars Bildsten and Greg Ushomirsky kicked off the discussion of r-mode crust effects. Since then, most of the dozen or so papers on the topic have asked, how does the crust prevent the r-modes from going unstable? There is now good reason to believe that, for young neutron stars, the interesting question is actually the reverse: How do the r-modes prevent crust formation? When a young neutron star cools to the temperature of crust formation, the r-modes are already unstable. If the r-mode amplitude exceeds a fairly small value, intense heating in the boundary layer prevents normal crust formation. Instead, a likely scenario is that a sort of flowing icepack forms, maintained at melting temperature by the r-mode shear, and that the original spindown scenario for purely fluid neutron stars is almost unchanged.

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