Abstract
In order to obtain the expression for the transport of radiant energy through the layers of the star in terms of ρ, T, and X, we need to spend a little time exploring the envelopes of stars. We will revisit the energy density and pressure due to radiation and discuss the consequences of local thermodynamic equilibrium. Finally, we will also look in more detail at the nature of absorption lines in stellar spectra.
This is a preview of subscription content, log in via an institution to check access.
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
Author information
Authors and Affiliations
Rights and permissions
Copyright information
© 2013 Springer Science+Business Media New York
About this chapter
Cite this chapter
Benacquista, M. (2013). Radiative Transfer and Stellar Atmospheres. In: An Introduction to the Evolution of Single and Binary Stars. Undergraduate Lecture Notes in Physics. Springer, New York, NY. https://doi.org/10.1007/978-1-4419-9991-7_6
Download citation
DOI: https://doi.org/10.1007/978-1-4419-9991-7_6
Published:
Publisher Name: Springer, New York, NY
Print ISBN: 978-1-4419-9990-0
Online ISBN: 978-1-4419-9991-7
eBook Packages: Physics and AstronomyPhysics and Astronomy (R0)