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Physics 3150: Introduction to Stellar Astrophysics |
| Winter 2008 |
Instructor: Chris Stevenson, C4063
Email: csteven at physics dot mun dot ca |
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Lectures
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Introduction
This is the webpage for P3150, "Introduction to Stellar Astrophysics" ("Astrophysics I").
In addition to meeting the expected prerequisites such as Modern Physics P2750, etc.,
it is presumed that those taking this course will have completed
an introductory astronomy/astrophysics course
like P2151, and so will have covered in a summary-fashion such topics as distance and magnitude-scales,
colour-magnitude (Herzsprung-Russell) diagrams and the basics of stellar evolution. (At any rate,
there will be a quick recap of these things as they come up, to set the context).
The existance of luminous matter in the Universe - stars, for example - is the direct consequence of
matter reacting to being forced into itself by self-gravitation. Mass and circumstance drive
the many manifestations of stars, and in this course we will look at some of the physics underlying
the birth, life, and death of stars. Topics covered will be from among examining cloud collapse criteria
for stellar formation; hydrostatic equilibrium (Equations of State and what a polytrope is, sources
of opacity, sources of energy such as nuclear fusion chains); computer modeling of a star;
radiative transfer processes as they relate
to the formation of spectral lines in stellar atmospheres; stellar pulsation mechanisms (e.g., Cepheids);
the usefulness of looking at stars in clusters; and stellar evolution off the main
sequence - stellar death throes that can lead to more exotic entities formed of degenerate matter
(white dwarves, neutron stars), pulsars, black holes, and their respective properties.
Weather-permitting, there may be an opportunity for a non-credit observational component to
illustrate some of this material, for those interested (and brave enough!)
Text
Lectures
Slot 16 (12am-1pm Tue & Thurs, 1-2pm Fri)
Evaluation
HII Talk
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