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We study the spindown of pulsars due to gravitational wave emission and showthat r-modes in neutron stars provide a quantitative explanation for theobserved low rotation frequencies of young pulsars if the r-mode saturationamplitude is sufficiently large. In contrast for such large saturationamplitudes old hadronic millisecond pulsars would spin down much faster thanobserved. We discuss resolutions of this apparent discrepancy that could makethis mechanism consistent with the observational data.

On the consistency of the spindown behavior of young and old pulsars