Coronal properties of pre-main sequence stars in the Orion Trapezium Cluster
Name
836717459-MIT.pdf
Description
Full printable version
Size
8.72 MB
Format
Adobe PDF
Checksum (MD5)
798598b478524d3b0a3c1315391a3c4f
Author(s)
Shen, Nancy
Advisor(s)
Norbert Schulz.
Date Issued
2012
Publisher
Massachusetts Institute of Technology
Abstract
Most of the young stars in the Orion Trapezium Cluster are much more peculiar in X-rays than expected, considering their structure, environment, and age. Highly resolved X-ray spectra provide many more details in order to study these peculiarities, specifically with respect to abundances and accretion signatures. We analyzed the high resolution X-ray spectra of six young stars in Orion using data from the Chandra X-Ray Observatory. We fit plasma models to the spectra, calculated temperature-insensitive elemental abundances from individual spectral line fits, determined common elemental abundances to refit the data, and computed confidence maps for pairs of model parameters. These results may provide insights into the physical properties and processes that cause certain stars to exhibit high temperatures in X-rays. This may lead to a better understanding of stellar structure and evolution in young stars.
Description
Thesis (S.B.)--Massachusetts Institute of Technology, Dept. of Physics, 2012.
Cataloged from PDF version of thesis.
Includes bibliographical references (p. 47-48).
Subjects
Physics.
MIT Department
Massachusetts Institute of Technology. Department of Physics
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copyright. They may be viewed from this source for any purpose, but
reproduction or distribution in any format is prohibited without written
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