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Claude R. Canizares. Migliazzo, Joshua Marc, 1977- Massachusetts Institute of Technology. Dept. of Physics. Massachusetts Institute of Technology. Department of Physics 2010-09-22T16:04:11Z 2010-09-22T16:04:11Z 2003 2003 http://hdl.handle.net/1721.1/58659 52562103 Thesis (S.M.)--Massachusetts Institute of Technology, Dept. of Physics, 2003. This electronic version was submitted by the student author. The certified thesis is available in the Institute Archives and Special Collections. Includes bibliographical references (p. 87-98). Using the Chandra High Energy Transmission Grating Spectrometer, we observed the young Supernova Remnant N103B in the Large Magellanic Cloud as part of the Guaranteed Time Observation program. N103B has a small overall extent and shows substructure on arcsecond spatial scales. The spectrum, based on 116ks of data, reveals unambiguous Mg, Ne, and O emission lines. Due to the elemental abundances, we are able to tentatively reject suggestions that N103B arose from a Type Ia supernova, in favor of the massive progenitor, core-collapse hypothesis indicated by earlier radio and optical studies, and by some recent X-ray results. We present our latest two-temperature shock and two-dimensional spatial-spectral modeling of the remnant. If the massive progenitor conclusion holds true, it would significantly changes previous conceptions of the young SNR population in the LMC. (cont.) Using the Very Large Array and the Pie Town antenna, we have measured the position of the radio pulsar B1995+32 relative to nearby background radio sources at four epochs between 1989 and 2000. These data show a clear motion for the pulsar of (25 +/- 4) milliarcsec/yr at a position angle (252 +/- 7) degrees (north through east), corresponding to a transverse velocity (240 +/- 40) km/s for a distance to the source of 2 kpc. The measured direction of motion confirms that the pulsar is moving away from the center of its associated supernova remnant, the first time that such a result has been demonstrated. Independent of assumptions made about the pulsar birth-place, we show that the measured proper motion implies an age for the pulsar of (64 +/- 18) kyr, somewhat less than its characteristic age of 107 kyr. This discrepancy can be explained if the initial spin period of the pulsar was P0 = (27 +/- 6) ms. by Joshua Marc Migliazzo. S.M. 98 p. eng Massachusetts Institute of Technology 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. http://dspace.mit.edu/handle/1721.1/7582 Physics. On understanding the lives of dead stars : Supernova Remnant N103B, radio pulsar B1951+32, and the Rabbit Thesis application/pdf Publication unknown unknown <Publication xmlns="https://www.openaire.eu/cerif-profile/1.1/" id="4817cb71-0e14-4472-88db-729fe01f2f28"> <Type xmlns="https://www.openaire.eu/cerif-profile/vocab/COAR_Publication_Types">http://purl.org/coar/resource_type/c_1843</Type> <Language>eng</Language> <Title>On understanding the lives of dead stars : Supernova Remnant N103B, radio pulsar B1951+32, and the Rabbit</Title> <PublishedIn> <Publication> </Publication> </PublishedIn> <PublicationDate>2003</PublicationDate> <Authors> <Author> <DisplayName>Migliazzo, Joshua Marc, 1977-</DisplayName> <Affiliation> <OrgUnit> </OrgUnit> </Affiliation> </Author> </Authors> <Editors> </Editors> <Publishers> <Publisher> <DisplayName>Massachusetts Institute of Technology</DisplayName> <OrgUnit /> </Publisher> </Publishers> <License>http://dspace.mit.edu/handle/1721.1/7582</License> <Keyword>Physics.</Keyword> <Abstract>Using the Chandra High Energy Transmission Grating Spectrometer, we observed the young Supernova Remnant N103B in the Large Magellanic Cloud as part of the Guaranteed Time Observation program. N103B has a small overall extent and shows substructure on arcsecond spatial scales. The spectrum, based on 116ks of data, reveals unambiguous Mg, Ne, and O emission lines. Due to the elemental abundances, we are able to tentatively reject suggestions that N103B arose from a Type Ia supernova, in favor of the massive progenitor, core-collapse hypothesis indicated by earlier radio and optical studies, and by some recent X-ray results. We present our latest two-temperature shock and two-dimensional spatial-spectral modeling of the remnant. If the massive progenitor conclusion holds true, it would significantly changes previous conceptions of the young SNR population in the LMC.</Abstract> <Abstract>(cont.) Using the Very Large Array and the Pie Town antenna, we have measured the position of the radio pulsar B1995+32 relative to nearby background radio sources at four epochs between 1989 and 2000. These data show a clear motion for the pulsar of (25 +/- 4) milliarcsec/yr at a position angle (252 +/- 7) degrees (north through east), corresponding to a transverse velocity (240 +/- 40) km/s for a distance to the source of 2 kpc. The measured direction of motion confirms that the pulsar is moving away from the center of its associated supernova remnant, the first time that such a result has been demonstrated. Independent of assumptions made about the pulsar birth-place, we show that the measured proper motion implies an age for the pulsar of (64 +/- 18) kyr, somewhat less than its characteristic age of 107 kyr. This discrepancy can be explained if the initial spin period of the pulsar was P0 = (27 +/- 6) ms.</Abstract> <Access xmlns="http://purl.org/coar/access_right" > </Access> </Publication>