The Evolution of Massive Young Stellar Objects in the Large Magellanic Cloud

This thesis presents an analysis of the largest catalog to date of infrared spectra of massive young stellar objects in the Large Magellanic Cloud. Evidenced by their very different spectral features, the luminous objects span a range of evolutionary states from those most embedded in their natal molecular material to those that have dissipated and ionized their surroundings to form compact HII regions and photodissociation regions. We quantify the contributions of the various spectral features using the statistical method of principal component analysis. Using this analysis, we classify the YSO spectra into several distinct groups based upon their dominant spectral features: silicate absorption (S Group), silicate absorption and fine-structure line emission (SE), polycyclic aromatic hydrocarbon (PAH) emission (P Group), PAH and fine-structure line emission (PE), and only fine-structure line emission (E). Based upon the relative numbers of sources in each category, we are able to estimate the amount of time massive YSOs spend in each evolutionary stage. We find that approximately 50% of the sources have ionic fine-structure lines, indicating that a compact HII region forms about half-way through the YSO lifetime probed in our study. Of the 277 YSOs we collected spectra for, 41 have ice absorption features, indicating they are surrounded by cold ice-bearing dust particles. We have decomposed the shape of the ice features to probe the composition and thermal history of the ice. We find that most the CO2 ice is embedded a polar ice matrix that has been thermally processed by the embedded YSO. The amount of thermal processing may be correlated with the luminosity of the YSO. Using the Australia Telescope Compact Array, we imaged the dense gas around a subsample of our sources in the HII complexes N44, N105, N113, and N159 using HCO+ and HCN as dense gas tracers. We find that the molecular material in star forming environments is highly clumpy, with clumps that range from subparsec to ~2 parsecs in size and with masses between 10^2 to 10^4 solar masses. We find that there are varying levels of star formation in the clumps, with the lower-mass clumps tending to be without massive YSOs. These YSO-less clumps could either represent an earlier stage of clump to the more massive YSO-bearing ones or clumps that will never form a massive star. Clumps with massive YSOs at their centers have masses larger than those with massive YSOs at their edges, and we suggest that the difference is evolutionary: edge YSO clumps are more advanced than those with YSOs at their centers. Clumps with YSOs at their edges may have had a significant fraction of their mass disrupted or destroyed by the forming massive star. We find that the strength of the silicate absorption seen in YSO IR spectra feature is well-correlated with the on-source HCO+ and HCN flux densities, such that the strength of the feature is indicative of the embeddedness of the YSO. We estimate that ~40% of the entire spectral sample has strong silicate absorption features, implying that the YSOs are embedded in circumstellar material for about 40% of the time probed in our study.

Influence of applied uniaxial stress upon the ultraviolet absorption bands in KBr and KI

The influence of uniaxial stress upon three types of imperfections occurring in the alkali halide crystal lattice has been investigated. The imperfections are the interstitial atom, the interstitial ion, and the negative ion vacancy. The interstitial atom, or H center, is a paraelastic defect which assumes a preferential crystal orientation in the field of an external mechanical stress. From the results of the reorientation kinetics - studies, it was possible to show that H centers are not stable in the KBr crystal lattice above 2SoK. At temperatures higher than 2SoK, the H centers are transformed into two new paraelastic defects, H(ii) and H(iii), possessing the same optical absorption band as the H center but differing both from the H' center and from each other in their reorientation kinetics. A study of the wavelength dependence of the H, H(ii), and VI (Na+) centers s~owed the 'existence of three similar-polarized transitions for each of these defects. One of these transitions, located at 230 run for all of the defects studied, was determined to be too high in energy to be explained by the simple X2 - level scheme. In addition, a comparison of various properties of the four defects indicates that the last three can be described as perturbed H centers. Dichroism measurements, performed as a function of temperature and wavelengt, h on the 230-nm I band in KBr, showed this band to be a composite of a band at 234 nm due to the I center and a band at 230 nm attributed to the H center. The I center dichroism was isolated and was observed under various experimental conditions. The results of these observations are consistent with a body-centered model for the I center in which the I-center absorption band is attributed to the excitation of a p-like electron on the interstitial Br- ion. Similar measurements were also perfonned on the a band in KI. The a-band dichroism measurements were found to be consistent with an electronic transition from an s-like ground state to a p-like excited state, indicating that the a center is best described as a quasi-molecule.