Understanding the temperature structure of protoplanetary disks (PPDs) is paramount to modeling disk evolution and future planet formation. PPDs around T Tauri stars have two primary heating sources, protostellar irradiation, which depends on the flaring of the disk, and accretional heating as viscous coupling between annuli dissipate energy. I have written a "1.5-D" radiative transfer code to calculate disk temperatures assuming hydrostatic and radiative equilibrium.
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- Partial requirement for: Ph.D., Arizona State University, 2012Note typethesis
- Includes bibliographical references (p. 170-177)Note typebibliography
- Field of study: Physics