The effect of sublimation temperature dependencies on disk walls around T Tauri stars
Erick Nagel,1 Paola D'Alessio,2 Nuria Calvet,3 Catherine Espaillat,4 and Miguel Angel Trinidad1
1 Departamento de Astronomía, Universidad de Guanajuato, 36240, Guanajuato, Guanajuato, México. (erick@astro.ugto.mx, trinidad@astro.ugto.mx).
2 Centro de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Apdo. Postal 3–72, 58090 Morelia, Michoacán, México. (p.dalessio@crya.unam.mx).
3 Department of Astronomy, University of Michigan, Ann Arbor, MI, 48109, USA. (ncalvet@umich.edu).
4 Harvard–Smithsonian Center for Astrophysics, Cambridge, MA, 02138, USA. (cespaillat@cfa.harvard.edu).
]]>Received 2012 July 23.
Accepted 2012 October 4.
RESUMEN
El polvo no puede sobrevivir más cerca de la estrella de un punto donde alcanza una temperatura igual a la temperatura de sublimación. La frontera entre una región sin polvo y polvosa define la pared de sublimación. En la literatura se usan dos modelos para la estructura de la pared: una pared con temperatura de sublimación fija y una con temperatura de sublimación dependiente de la densidad. En la primera, la pared es vertical y en la segunda, la pared es curva. Encontramos diferencias importantes entre la SEDs de estos modelos en el intervalo de longitudes de onda desde 3 a 8 µm, siendo la emisión de la primera más grande que la segunda. Cuantificamos las diferencias en los colores de IRAC cuando se usan estos modelos para explicar las observaciones. En el diagrama de IRAC color–color ([3.6]–[4.5] vs. [5.8]–[8.0]), los modelos están localizados en regiones específicas, dada la inclinación, la tasa de acreción de masa, o el modelo usado.
ABSTRACT
The dust cannot survive closer to the star from the point where a grain reaches a temperature equal to the sublimation temperature. The boundary between a dust–free and a dusty region defines the sublimation wall. In the literature two models for the structure of the wall are used: a wall with a fixed sublimation temperature and a wall with a density–dependent sublimation temperature. In the former case, the wall is vertical and in the latter, the wall is curved. We find important differences between these models' SEDs in the wavelength range from 3 to 8 µm, the emission of the former being larger than that of the latter model. We quantify the differences in IRAC colors when these models are used to explain the observations. In the IRAC color–color diagram ([3.6]–[4.5] vs. [5.8]–[8.0]), the models are located in specific regions, either depending on the inclination, the mass accretion rate, or the model used.
Key Words: infrared: general — protoplanetary disks — stars: pre–main sequence.
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