{"id":{"repo_id":"mit","oai_identifier":"oai:dspace.mit.edu:1721.1/78488"},"canonical_url":"https://search.dev.ndltd.org/etd/mit/oai:dspace.mit.edu:1721.1/78488","repository":{"repo_id":"mit","name":"MIT","base_url":"https://dspace.mit.edu/oai/request"},"display":{"title":"Coronal properties of pre-main sequence stars in the Orion Trapezium Cluster","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.","abstract_html":"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.","abstract_has_math":false,"creators":["Shen, Nancy"],"institution":"Massachusetts Institute of Technology","degree_name":null,"degree_level":null,"degree_discipline":null,"degree_department":"Massachusetts Institute of Technology. Department of Physics.","school":null,"contributors":[],"advisors":["Norbert Schulz."],"committee_chairs":[],"committee_members":[],"year":2012,"date_issued":"2012","date_published":"2012","updated_at":"2026-07-22T22:22:12Z","subjects":["Physics."],"languages":["eng"],"rights":["M.I.T. theses are protected by copyright. They may be viewed from this source for any purpose, but reproduction or distribution in any format is prohibited without written permission. See provided URL for inquiries about permission."],"rights_urls":["http://dspace.mit.edu/handle/1721.1/7582"],"identifier_entries":[]},"links":{"outbound_url":"http://hdl.handle.net/1721.1/78488","outbound_label":"Handle","outbound_source":"dc:identifier.uri"},"metadata_groups":[{"id":"people","label":"People","entries":[{"key":"dc:contributor.advisor","label":"Advisor","values":["Norbert Schulz."]},{"key":"dc:contributor.department","label":"Department","values":["Massachusetts Institute of Technology. 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They may be viewed from this source for any purpose, but reproduction or distribution in any format is prohibited without written permission. See provided URL for inquiries about permission."]},{"key":"dc:rights.uri","label":"Rights URI","values":["http://dspace.mit.edu/handle/1721.1/7582"]}]},{"id":"identifiers","label":"Identifiers","entries":[{"key":"dc:identifier.uri","label":"Identifier URI","values":["http://hdl.handle.net/1721.1/78488"]}]},{"id":"additional","label":"Additional Metadata","entries":[{"key":"dc:description","label":"Description","values":["Thesis (S.B.)--Massachusetts Institute of Technology, Dept. of Physics, 2012.","Cataloged from PDF version of thesis.","Includes bibliographical references (p. 47-48)."]},{"key":"dc:description.abstract","label":"Abstract","values":["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."]},{"key":"dc:description.degree","label":"Dc Description Degree","values":["S.B."]},{"key":"dc:title","label":"Title","values":["Coronal properties of pre-main sequence stars in the Orion Trapezium Cluster"]}]}],"canonical_facts":{"dc:contributor.advisor":["Norbert Schulz."],"dc:contributor.department":["Massachusetts Institute of Technology. Department of Physics."],"dc:contributor.other":["Massachusetts Institute of Technology. Department of Physics."],"dc:creator":["Shen, Nancy"],"dc:date.accessioned":["2013-04-12T19:29:00Z"],"dc:date.available":["2013-04-12T19:29:00Z"],"dc:date.issued":["2012"],"dc:description":["Thesis (S.B.)--Massachusetts Institute of Technology, Dept. of Physics, 2012.","Cataloged from PDF version of thesis.","Includes bibliographical references (p. 47-48)."],"dc:description.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."],"dc:description.degree":["S.B."],"dc:identifier.uri":["http://hdl.handle.net/1721.1/78488"],"dc:language.iso":["eng"],"dc:publisher":["Massachusetts Institute of Technology"],"dc:rights":["M.I.T. theses are protected by copyright. They may be viewed from this source for any purpose, but reproduction or distribution in any format is prohibited without written permission. See provided URL for inquiries about permission."],"dc:rights.uri":["http://dspace.mit.edu/handle/1721.1/7582"],"dc:subject":["Physics."],"dc:title":["Coronal properties of pre-main sequence stars in the Orion Trapezium Cluster"],"dc:type":["Thesis"]},"updated_at":"2026-07-22T22:22:12Z"}