Spectral synthesis of inner gaseous protoplanetary disks with PHOENIX

Details Spectral synthesis of inner gaseous protoplanetary disks with PHOENIX Spectral synthesis of inner gaseous protoplanetary disks with PHOENIX

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1094..389h&link_type=abstract

COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun.

Physics

Circumstellar Shells, Clouds, And Expanding Envelopes, Circumstellar Masers, Infall, Accretion, And Accretion Disks, Radiative Transfer, Scattering

Scientific paper

The inner gaseous regions of protoplanetary disks are of special interest in the formation and evolution of planets and stars because they are the likely birthplaces of planets and serve as the accretion reservoir for young stars. The study of inner disks may give rise to a better understanding of the dynamics, physical and chemical structure, and gas content of the region. As a first step, we have developed a 1+1D disk radiative transfer package as an extension to the well established multipurpose stellar atmosphere program PHOENIX. The solution of the equations of momentum and energy conservation as well as the radiative transfer equation is adopted for the physical conditions in and the geometry of disks. Irradiation by the central star is treated in detail. Comparison of our models with high-resolution infrared spectra will enable us to constrain the structure, dynamics, and gas content of disks, and thus give new insights on the physical processes governing star and planet formation. Additionally, we present our current construction site: a 3D radiative transfer code for accretion disks.

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