FINAL PROJECT
ASTR 5420 - Stellar Evolution & Interiors
Spring 2016
The final project will make up 25% of your total grade for the class.
Your write-up will count for half the final project grade, and your poster
presentation for the other half.
The abstract/proposal for your project will be due as part of
the final problem set.
It is strongly recommended to discuss project ideas with the instructor
for approval beforehand.
The format of the paper should conform to the standards of
an ApJ Letter. To wit, no more than 3500 words and
no more than 5 figures and tables.
See
http://aastex2.aas.org/ApJL/countwords.html
for detailed length limits.
Your poster should be no more than 48''×48'' in size.
All posters will be presented during the last day of class,
Friday, May 2, 2016.
You will be graded using the same criteria used for the Chambliss
Poster Prize: see
https://aas.org/files/resources/aas227_chambliss_judging_form_graduate_v4.pdf.
Your project may either be a review of a topic in stellar astrophysics
not covered in detail in class, or computational in nature,
dealing with models published in the literature or developing your own.
Whatever topic you choose, you should incorporate the relevant
physics of stars discussed during the semester into your discussion.
The following is a representative list of possible project topics.
You may choose from this list, or develop a topic of your own.
In either case, your topic is subject to instructor approval.
Sample literature review topics:
- Population III (zero metallicity) stars
- Hyper-velocity stars
- Solar/stellar coronae
- Blue stragglers
- Asteroseismology
- Star formation
- Stellar remnants
- Cataclysmic variables, dwarf novae
- Binary stars
Sample computational projects:
- Download and run a Monte-Carlo radiative transfer code,
such as RADMC-3D, Hyperion, or DUSTY. Explain how
the radiative transfer problem is solved in the code and
show an example of how to use the code for an astrophysical context
- Apply Kurucz stellar photosphere models to stellar spectra
- Apply pre-main sequence stellar evolution models to YSOs
- Apply main sequence fitting to a cluster
- Apply a population synthesis model to a galaxy
- Compare and contrast stellar atmosphere or interior models
- Write a code to implement the Eddington standard model for
stellar interiors, following 7.2.7 of HKT.
FINAL PROJECT
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