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The dynamics of the charged particles in the fluid interior of rotating magnetized neutron stars (pulsars) is investigated. It is shown that a magnetohydrodynamic approach is valid under a wide variety of conditions. The small amplitude waves that can propagate in the "charged" <-4 fluid are sound waves (period ^> 10 sec), inertial waves (-1 sec) and hydromagnetic-inertial waves (£ months). Generally, the most effective damping mechanism is viscosity. Viscous damping times for hydromagneticinertial waves can be as long as hundreds of years. Several normal sound mode and normal inertial mode calculations are performed. The motion of the charged fluid over the time scales of inertial waves and hydromagnetic-inertial waves is simulated on a computer. Mode-mode coupling, boundary layers, and the acceleration of the crust due to charged fluid motion are also studied. The most important conclusion in this thesis is that the time the charged fluid as a whole takes to respond to a sudden disturbance such as a change in the angular velocity or acceleration of the crust is the time for a long wavelength hydromagnetic-inertial wave to cross the star. Contrary to an assumption which has been made in models of pulsar postglitch behaviour, the charged fluid response time is not necessarily small compared to post-glitch relaxation times. In view of this, models of post-glitch behaviour which assume that the charged fluid response time is small compared to post-glitch relaxation times should be reexamined .

A configuration-interaction calculation of the electronic energies of the O H radical has been performed, using from 34 to 46 configurations for the doublet states; and from 11 to 25 configurations for the quartet states. The results are presented for the six lowest states of 'Z+, 'Z-, 'II, 'A; 4Z+ , 4Z-, , 411 and 4A symmetries. The calculations have been performed for a range of internuclear distances from 0.8 to 3 A. The method of computation has been designed to give the kind of accuracy for the lowest three or four states of each symmetry which could be useful in the empirical analysis of the hitherto unanalyzed spectrum of O H in the 1850 A region.