Diversity of planetary systems in low-mass disks: terrestrial-type planet formation and water delivery
<b>Context.</b> Several studies, observational and theoretical, suggest that planetary systems with only rocky planets are the most common in the Universe. <b>Aims.</b> We study the diversity of planetary systems that might form around Sun-like stars in low-mass disks without...
| Autores: | , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2014 |
| País: | Argentina |
| Institución: | Universidad Nacional de La Plata |
| Repositorio: | SEDICI (UNLP) |
| Idioma: | inglés |
| OAI Identifier: | oai:sedici.unlp.edu.ar:10915/85235 |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/85235 |
| Access Level: | acceso abierto |
| Palabra clave: | Ciencias Astronómicas Astrobiology Methods: numerical Protoplanetary disks |
| Sumario: | <b>Context.</b> Several studies, observational and theoretical, suggest that planetary systems with only rocky planets are the most common in the Universe. <b>Aims.</b> We study the diversity of planetary systems that might form around Sun-like stars in low-mass disks without gas-giant planets. We focus especially on the formation process of terrestrial planets in the habitable zone (HZ) and analyze their water contents with the goal to determine systems of astrobiological interest. In addition, we study the formation of planets on wide orbits because they can be detected with the microlensing technique. <b>Methods.</b> N-body simulations of high resolution were developed for a wide range of surface density profiles. A bimodal distribution of planetesimals and planetary embryos with different physical and orbital configurations was used to simulate the planetary accretion process. The surface density profile combines a power law for the inside of the disk of the form r-γ, with an exponential decay to the outside. We performed simulations adopting a disk of 0.03 M ⊙ and values of γ = 0.5, 1 and 1.5. <b>Results.</b> All our simulations form planets in the HZ with different masses and final water contents depending on the three different profiles. For γ = 0.5, our simulations produce three planets in the HZ with masses ranging from 0.03 MŠ to 0.1 M⊕ and water contents between 0.2 and 16 Earth oceans (1 Earth ocean =2.8 × 10-4⊕). For γ = 1, three planets form in the HZ with masses between 0.18 M⊕ and 0.52 M⊕ and water contents from 34 to 167 Earth oceans. Finally, for γ = 1.5, we find four planets in the HZ with masses ranging from 0.66 M⊕ to 2.21 M⊕ and water contents between 192 and 2326 Earth oceans. This profile shows distinctive results because it is the only one of those studied here that leads to the formation of water worlds. <b>Conclusions.</b> Since planetary systems with γ = 1 and 1.5 present planets in the HZ with suitable masses to retain a long-lived atmosphere and to maintain plate tectonics, they seem to be the most promising candidates to be potentially habitable. Particularly, these systems form Earths and Super-Earths of at least 3 M⊕ around the snow line, which can be discovered by the microlensing technique. |
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