Applications of the code include work on the solar chromosphere and on the atmospheres of hot stars. We are able to resolve relatively small inhomogeneous structures on the sun. These structures dissipate their thermal energy through radiation and dynamic expansion, and their physical states may be determined by their radiative spectrum. Distant stars are too far away to resolve individual features, so one must rely more on theoretical simulations and regions of the spectrum which accentuate particular features (e.g. the infrared and/or ultraviolet).
As an outgrowth of his interest in radiative transfer problems, Dr. Anderson- Huang maintains collaborations and communication with atomic physicists, and works on problems concerning absorption and emission processes and electron and atom collision processes important for stellar atmospheres and interiors. He also maintains a continued interest in convection theory and modeling, and the signatures of convection imprinted on the emergent radiation spectra of stars.
Anderson, L., and Athay, R.G. 1989. Model solar chromosphere with prescribed heating. Ap. J. 346:1010.
A description of his code appears in: Kalkofen, W., ed. 1986. Numerical radiative transfer. Cambridge: Cambridge Univ. Press.