How Can R-Mode Heating Prevent Crust Formation?

Details How Can R-Mode Heating Prevent Crust Formation? How Can R-Mode Heating Prevent Crust Formation?

Aug 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000rmns.proge..11o&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

Nine months ago, Lars Bildsten and Greg Ushomirsky kicked off the discussion ofr-modecrust effects. Since then, most of the dozen or so papers on the topic haveasked, how doesthe crust prevent the r-modes from going unstable? There is now good reason tobelievethat, for young neutron stars, the interesting question is actually the reverse:How do ther-modes prevent crust formation? When a young neutron star cools to thetemperature ofcrust formation, the r-modes are already unstable. If the r-mode amplitudeexceeds afairly small value, intense heating in the boundary layer prevents normal crustformation. Instead, a likely scenario is that a sort of flowing icepack forms,maintained at melting temperature by the r-mode shear, and that the originalspindown scenario for purely fluid neutron stars is almost unchanged.

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