Statistics – Computation
Scientific paper
Jun 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999phdt.........4r&link_type=abstract
Thesis (PhD). CORNELL UNIVERSITY, Source DAI-B 59/12, p. 6353, Jun 1999, 191 pages.
Statistics
Computation
Orionis, Be Stars, Starburst Galaxies
Scientific paper
I have explored stellar evolution through several different scientific studies, including mid-infrared (MIR) imaging of α Orionis, examination of ultraviolet (UV) periodicities from α Orionis, MIR spectroscopy of Be stars, and modelling of starburst galaxies evolution. Mid-infrared imaging techniques were used in concert with computational modelling to determine parameters for the dust shell surrounding the late-type star α Orionis. I found that the circumstellar dust has a spherical shell geometry, and quantitatively determined the density profile and temperature profile for the dust shell. I have used archival International Ultraviolet Observer data to look for periodicities in the ultraviolet flux of α Orionis, looking for the presence of a binary companion. While the examination of the IUE dataset was inconclusive, I can rule out the presence of a blue companion to α Ori. As part of my work in infrared astronomy, I have also worked on developing a new instrument for Palomar, SCORE (SIRTF Cornell Echelle, the prototype of the short-hi module of the Infrared Spectrograph instrument for SIRTF). I discuss the characteristics and abilities of SCORE, and suggest some possible future directions for similar instrumentation in the future. Using the unique abilities of SCORE, I also present the results of R ~ 600 MIR spectroscopy on Be stars. These objects have a wealth of hydrogen recombination lines in the MIR, with an excess of MIR continuum flux. These observations can be used to determine electron temperatures in the circumstellar envelopes of these objects by fitting free-free emission curves to the observed MIR continuum. Results from some of our fits are presented here, along with some discussion of future modelling projects which can lead to new insights into the Be star phenomena. Finally, we present redshift data for infrared-luminous galaxies at the North Ecliptic Pole. Using the 60μm fluxes from these objects, as measured by IRAS, and the redshifts obtained by our redshift survey, I examine models of starburst galaxy evolution. I compare the results of various evolutionary models to the data, and conclude that only no evolution or weak evolution is allowed by these observations.
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