Date of Award

May 2020

Document Type


Degree Name

Master of Science (MS)


Physics and Astronomy

Committee Member

Bradley S Meyer

Committee Member

Mounib F El-Eid

Committee Member

Dieter H Hartmann

Committee Member

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]



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