Date of Award
Master of Science (MS)
Physics and Astronomy
Bradley S Meyer
Mounib F El-Eid
Dieter H Hartmann
Stephen R Kaeppler
In this thesis, we investigate the eects of rotation on the evolution of stars
in the mass range of 2-15 M assuming solar-like initial composition. We have used
a well tested hydrodynamical stellar evolution program [El Eid et al., 2009], which
has been extended to include a one-dimensional treatment of rotational instabilities.
The calculations for stars in the mass range up to 8 M have been performed
to include the Asymptotic Giant Branch (AGB) in order to gure out
whether rotational instabilities can eect the so called "third dredge up", leading
to a neutron source for the s-process nucleosynthesis.
In the case of massive stars, above 8 M, rotational eects are expected
to become important during the main sequence evolution, mainly owing to the
so called "Eddington-Sweet" circulation. An indication of the eect of rotation
should show up through the surface enrichment of 4He and 14N at the end of
core Hydrogen burning. Another important aspect of rotation is the study of
its eect on the shell carbon burning phase, where the s-process nucleosynthesis
occurs.[El Eid et al., 2000]
Tannous, Jaad Antoun, "The Effect of Rotation on Stellar Structure and Evolution" (2020). All Theses. 3267.