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Modeling Layered Accretion and the Magnetorotational Instability in Protoplanetary Disks

Abstract 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. The model solves for the temperature at all locations simultaneously using Rybicki's method, converges rapidly at high optical depth, and retains full frequency dependence. The likely cause of accretional heating in PPDs is the magnetorotational instability (MRI)... (more)
Created Date 2012
Contributor Lesniak Iii, Michael V. (Author) / Desch, Steven J. (Advisor) / Scannapieco, Evan (Committee member) / Timmes, Francis (Committee member) / Starrfield, Sumner (Committee member) / Belitsky, Andrei (Committee member) / Arizona State University (Publisher)
Subject Astrophysics / Astronomy / Physics / accretion disks / ionization chemistry / layered accretion / magnetorotational instability / protoplanetary disks
Type Doctoral Dissertation
Extent 195 pages
Language English
Reuse Permissions All Rights Reserved
Note Ph.D. Physics 2012
Collaborating Institutions Graduate College / ASU Library
Additional Formats MODS / OAI Dublin Core / RIS

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Description Dissertation/Thesis