A self-concurrent algorithm to model young stellar disks

Details A self-concurrent algorithm to model young stellar disks A self-concurrent algorithm to model young stellar disks

Aug 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003basbr..23...32h&link_type=abstract

Boletim da Sociedade Astronômica Brasileira (ISSN 0101-3440), vol.23, no.1, p.32-32

Astronomy and Astrophysics

Astronomy

Scientific paper

The contribution of the circumstellar dust to the emitted radiation of young stellar systems is mainly evaluated by means of the IR excess observed in these objects. In our previous study of weak-T Tauri stars (WTTs), we adopted the simplest scenario assuming that the disk is flat, passive and re-radiates the energy absorbed from the central star. By considering a second component to the circumstellar structure: a tenuous dust envelope surrounding the star and the disk, our model reproduces the flattened spectral energy distribution (SED) exhibited by most of the studied TTs. In the present work this disk model has been improved to better be applied to Herbig Ae/Be stars, intermediate-mass young stars, which could not have their SED fitted as successful as the WTTs. Chiang et al. (2001) used hydrostatic, radiative equilibrium models for passive, reprocessing flared disks surrounding TT and HAe stars. The grains in the surface of the disk are directly exposed to the radiation from the star and the interior of the disk is heated by diffusion from the surface. By following the two-layers disk structure suggested by them, our disk model was improved and could calculate the SED for a sample of HAes stars. In this work we describe the calculation technique, which is based on algorithms presented by Bentley & Corne (2002). The obtained results were compared with the previous ones showing that a flared structure could better explain the SED of the studied stars. We also conclude that the parameter estimation by a self-concurrent algorithm results in a more accurate and faster calculation.

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