THE EFFECT OF SUBLIMATION TEMPERATURE DEPENDENCIES ON DISK WALLS AROUND T TAURI STARS
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 fi...
| Autores: | , , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2013 |
| País: | México |
| Institución: | Universidad Nacional Autónoma de México |
| Repositorio: | Redalyc-UNAM |
| OAI Identifier: | oai:redalyc.org:57126152005 |
| Acceso en línea: | https://www.redalyc.org/articulo.oa?id=57126152005 |
| Access Level: | acceso abierto |
| Palabra clave: | Física, Astronomía y Matemáticas stars: pre main sequence Infrared: general protoplanetary disks |
| Sumario: | 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. |
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