Of the billions of stars which compose a galaxy, a few will be members of the so called eclipsing binary star systems. These are systems in which two stars orbit a common center of mass and the orbital plane is oriented along the observer's line of sight. Even though such systems appear as a single point of light, due to the extreme distance from the earth, the structure can be inferred from the observed light variations produced as each star eclipses its companion.The writer constructed the necessary equipment and carried out photoelectric observations of the star system V566 Ophiuchi. A mathematical model was also constructed which produced some approximate dimensions of this system. Three time:; of minimum light were found that indicate that the orbital period has undergone some change during the last few years. The most likely cause for this change is some type of physical interaction between the two stellar components.

Photocopy of typescript. / Thesis (Ph. D.)--University of Hawaii at Manoa, 1979. / Bibliography: leaves 127-138. / Microfiche. / x, 138 leaves ill., maps 29 cm

Typescript. / Thesis (Ph. D.)--University of Hawaii at Manoa, 1990. / Includes bibliographical references. / Microfiche. / xii, 178 leaves, bound ill. 29 cm

Thesis (Ph. D.)--University of Hawaii at Manoa, 1995. / Includes bibliographical references (leaves 106-112). / Microfiche. / x, 112 leaves, bound ill. (some col.) 29 cm

This thesis describes the development of a red tip/tilt and fringe detection system at the Sydney University Stellar Interferometer (SUSI), modelling the instrumental performance and effects of seeing at SUSI, making observations of Mira variable stars and finally modelling the atmospheres of Mira variables with physically self-consistent models. The new SUSI tip/tilt system is based around a CCD detector and has been successfully used to both track the majority of tip/tilt power in median seeing at an R magnitude of 4.5, and to provide seeing measures for post processing. The new fringe-detection system rapidly scans 33 to 140 $\mu$m in delay and detects the fringes using two avalanche-photodiodes. It has been used to acquire fringe data, provide user feedback and to track the fringe group-delay position. The system visibility (fringe visibility for a point source) and throughput were found to be consistent with models of the SUSI optical beam train. Observations were made of a variety of sources, including the Mira variables R Car and RR Sco, which were observed in two orthogonal polarization states. These measurements were the first successful use of Optical Interferometric Polarimetry (OIP), and enabled scattered light to be separated from bright photospheric flux. Dust scattering was found to originate from a thin shell 2-3 continuum radii from these stars, with an optical depth of 0.1 to 0.2 at 900 nm. Physical models of Mira variables including dust formation were developed, providing consistent explanations for these results as well as many other photometric and interferometric observations.

Thesis (Ph.D.)--McMaster University (Canada), 1994. / Source: Dissertation Abstracts International, Volume: 58-06, Section: B, page: 3088. Adviser: D. L. Welch.

Thesis (Ph. D.)--University of Texas at Austin, 2008. / Vita. Includes bibliographical references.

Thesis (Ph.D.)--Michigan State University. Dept. of Physics and Astronomy, 2008. / Title from PDF t.p. (viewed on July 22, 2009) Includes bibliographical references (p. 243-249). Also issued in print.

Thesis (Ph. D.)--University of Hawaii at Manoa, 2004. / On title page "[mu]" appears as Greek symbol. Includes bibliographical references (leaves 167-180).

Thesis (M.S.)--Ball State University, 2009. / Title from PDF t.p. (viewed on June 07, 2010). Includes bibliographical references (p. [46]).