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Asteroseismic Data AnalysisFoundations and Techniques$
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Sarbani Basu and William J. Chaplin

Print publication date: 2017

Print ISBN-13: 9780691162928

Published to Princeton Scholarship Online: May 2018

DOI: 10.23943/princeton/9780691162928.001.0001

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Theoretical Underpinnings: Modeling Stars

Theoretical Underpinnings: Modeling Stars

Chapter:
(p.16) 2 Theoretical Underpinnings: Modeling Stars
Source:
Asteroseismic Data Analysis
Author(s):

Sarbani Basu

William J. Chaplin

Publisher:
Princeton University Press
DOI:10.23943/princeton/9780691162928.003.0002

This chapter provides a brief description of the process of constructing models for the interpretation of stellar oscillation data. The equations of stellar structure are basically statements of conservation—of mass, momentum, and energy—along with the conditions required for thermal equilibrium. The equations of stellar structure are written with mass as the independent variable. Here, a star is divided into many mass shells, from the center at m = 0 to the surface at m = M, where M is the total mass of the star, and a model is obtained by solving the set of equations at each mass shell in a self-consistent manner. In addition, the chapter considers energy generation and how energy is transported from the core to the surface, as well as how elemental abundances change as a function of time.

Keywords:   modeling stars, constructing models, stellar oscillation data, mass, momentum, energy, energy generation

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