Modelling Gravitationally Coupled Modes of High Stellar Mass Protostellar Star-Disk Systems Public Deposited

http://ir.library.oregonstate.edu/concern/undergraduate_thesis_or_projects/fn1073736

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  • We computationally modeled protostellar star-disk systems with star to disk mass ratio of 10. Our computational models looked at the development of density perturbations in these systems for different geometries of the system. The ratio of the star’s height and radius (rₚ/rₑ) is varied between 0.1746 and 0.88095. We modeled systems with differentially rotating stars. The results of this research were compared with earlier research done by Hadley et al. (2017) to see if there are consistent trends between models with moderate star to disk mass ratio (M = 4) and models with high star to disk mass ratio (M = 10). A quantity that was considered was β, which is the ratio of the rotational kinetic energy to the gravitational potential energy. Prior research tells us that stellar barlike modes are unstable for values of β greater than 0.274. This was confirmed for the models run in our research. However, unexpected perturbations at the center of the star were also observed in higher modes that were not seen for the M = 4 case.
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  • description.provenance : Approved for entry into archive by Steven Van Tuyl(steve.vantuyl@oregonstate.edu) on 2017-07-24T23:48:18Z (GMT) No. of bitstreams: 2license_rdf: 1232 bytes, checksum: bb87e2fb4674c76d0d2e9ed07fbb9c86 (MD5)AneeqAhmedPhysicsThesis.pdf: 1189997 bytes, checksum: f4e3fdb639fd3554c7a9e6d55bb8b417 (MD5)
  • description.provenance : Submitted by Aneeq Ahmed (ahmedan@oregonstate.edu) on 2017-07-14T22:49:07ZNo. of bitstreams: 2license_rdf: 1232 bytes, checksum: bb87e2fb4674c76d0d2e9ed07fbb9c86 (MD5)AneeqAhmedPhysicsThesis.pdf: 1189997 bytes, checksum: f4e3fdb639fd3554c7a9e6d55bb8b417 (MD5)
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