Constraining emission regions and magnetic field structures in cataclysmic variables through x-ray, UV and optical observations

This thesis examines observations from the unusual cataclysmic variable TT Arietis and the eclipsing magnetic cataclysmic binary DP Leo, utilizing multispectral data from ground and space-based observatories. The observation of emission from cataclysmic variables in the X-ray, ultraviolet and optical bands yields vital information on the emission regions and their environments. In addition, the analysis of the accretion stream flow in the highly magnetic cataclysmic variables allows the magnetic field structure of the white dwarf to be probed.; An intricate array of observations on TT Ari are examined and the relationship of this system to other cataclysmic binaries is explored. The dominating source of X-ray emission from TT Ari has previously been suggested to originate from the region where the accretion stream impacts the disk. However, observed hard X-ray emission cannot be sustained in such a model. It is found, at times, that nearly all of the X-ray emission appears strongly pulsed on periods close to quasi-periodic modulations found in the optical. This suggests a connection between the variations in the optical and those found in X-rays on timescales of order tens of minutes. An analysis of long term trends confirms that the X-ray and optical emission are not correlated on timescales of months to years. Further, the UV observations of this source show complex behavior with, at times, strong P Cygni features modulated at the system's orbital period.; DP Leo is an eclipsing cataclysmic binary containing a magnetic white dwarf. The eclipses allow the location of the emission regions in the system to be constrained. Times of increased X-ray absorption place limits on the shape and structure of the accretion stream. Systematic motion of the small X-ray emitting region on the white dwarf, relative to the secondary star, exists over the multi-year baseline of observations of this system. Mechanisms for producing this motion are explored.