2026-09-21T08:21:48Zhttps://dspace.mit.edu/server/oai/requestoai:dspace.mit.edu:1721.1/1056252022-01-13T07:54:07Zcom_1721.1_7582com_1721.1_7581col_1721.1_131024
Nevin Weinberg.
Belland, Brent (Brent R.)
Massachusetts Institute of Technology. Department of Physics.
Massachusetts Institute of Technology. Department of Physics
2016-12-05T19:55:28Z
2016-12-05T19:55:28Z
2016
2016
http://hdl.handle.net/1721.1/105625
963174760
Thesis: S.B., Massachusetts Institute of Technology, Department of Physics, 2016.
Cataloged from PDF version of thesis.
Includes bibliographical references (page 43).
Hot Jupiters raise strong tides in their host stars due to their large masses (around a Jupiter mass) and tight orbits (orbital periods P </~ 3 days). These tides remove orbital energy and angular momentum, causing the planet's orbit to decay. The rate of decay depends on the detailed structure of the host star through the coefficients of nonlinear tidal coupling. Here we calculate these coefficients over a range of stellar mass and age on the main sequence (0.8 </= M/M < 1.2). These coefficients provide crucial input for future studies of nonlinear tidal dissipation; our analysis enables these studies to be extended to systems with non-solar-type hosts.
by Brent Belland.
S.B.
43 pages
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.
Orbital decay of hot Jupiters : coefficients of nonlinear tidal coupling as a function of the stellar host type
Thesis
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<Abstract>Hot Jupiters raise strong tides in their host stars due to their large masses (around a Jupiter mass) and tight orbits (orbital periods P </~ 3 days). These tides remove orbital energy and angular momentum, causing the planet's orbit to decay. The rate of decay depends on the detailed structure of the host star through the coefficients of nonlinear tidal coupling. Here we calculate these coefficients over a range of stellar mass and age on the main sequence (0.8 </= M/M < 1.2). These coefficients provide crucial input for future studies of nonlinear tidal dissipation; our analysis enables these studies to be extended to systems with non-solar-type hosts.</Abstract>
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