From circumstellar disks to planetary systems: observation and modeling of protoplanetary disks
The existence of exoplanetary systems was first predicted after the discovery of accretion disks around young stars. Nowadays, with nearly 3500 exoplanets discovered, and almost 5000 more candidates identified by the Kepler space mission, planetary systems are now known to be ubiquitous around low-m...
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| Tipo de recurso: | tesis doctoral |
| Estado: | Versión publicada |
| Fecha de publicación: | 2016 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/149498 |
| Acceso en línea: | http://hdl.handle.net/10261/149498 |
| Access Level: | acceso abierto |
| Palabra clave: | Discos protoplanetarios Materia interestelar Planetas extrasolares: formación Exoplanetas |
| Sumario: | The existence of exoplanetary systems was first predicted after the discovery of accretion disks around young stars. Nowadays, with nearly 3500 exoplanets discovered, and almost 5000 more candidates identified by the Kepler space mission, planetary systems are now known to be ubiquitous around low-mass stars. The formation of these systems takes place during the stellar formation itself, from the dust and gas orbiting around the star in the protoplanetary disks. However, the process that leads to this formation is still not well understood. Studying the physical and chemical conditions of circumstellar disks is, thus, key to understand the planetary formation process. Planets can interact with the disk, creating structures such as spiral density waves, gaps, cavities or lopsided asymmetries. Studying disks showing these features could provide us with critical information about the planetary formation process itself. In particular, transitional disks, which are protoplanetary disks with central gaps or cavities in the dust distribution, appear as excellent candidates to study the first stages of planetary formation. Cavities in transitional disks were first identified through modeling of their spectral energy distributions (SEDs). This modeling also lead to the discovery of a subfamily of transitional disks, the so-called pre-transitional disks, which are thought to present a residual inner disk inside the cavity. (Sub-)mm and polarimetric IR observations have been able to image several of these disks and confirm the presence of the central cavities or gaps. |
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