  Almost all pulsars with anomalous positive $\ddot \Omega $ measurements
(corresponding to anomalous braking indices in the range 5$<n<$100), including
all the pulsars with observed large glitches ($\Delta\Omega/\Omega$ $>$
10$^{-7}$) as well as post glitch or interglitch $\ddot \Omega$ measurements
obey the scaling between $\ddot \Omega$ and glitch parameters originally noted
in the Vela pulsar. Negative second derivative values can be understood in
terms of glitches that were missed or remained unresolved. We discuss the
glitch rates and a priori probabilities of positive and negative braking
indices according to the model developed for the Vela pulsar. This behavior
supports the universal occurrence of a nonlinear dynamical coupling between the
neutron star crust and an interior superfluid component. The implied lower
limit to dynamical energy dissipation in a neutron star with spindown rate
$\dot \Omega$ is $\dot E_{diss}> 1.7 \times 10 ^{-6} \dot E_{rot}$. Thermal
luminosities and surface temperatures due to dynamical energy dissipation are
estimated for old neutron stars which are spinning down as rotating magnetic
dipoles beyond the pulsar death line.
