Numerical simulations for terrestrial planets formation
نویسندگان
چکیده
منابع مشابه
Simulations for Terrestrial Planets Formation
In this paper, we investigate the formation of terrestrial planets in the late stage of planetary formation using two-planet model. At that time, the protostar has formed for about 3 Myr and the gas disk has dissipated. In the model, the perturbations from Jupiter and Saturn are considered. We also consider variations of the mass of outer planet, and the initial eccentricities and inclinations ...
متن کاملPlanetesimal Evolution and the Formation of Terrestrial Planets
Title of Dissertation: Planetesimal Evolution and the Formation of Terrestrial Planets Zoë Malka Leinhardt, Doctor of Philosophy, 2005 Dissertation directed by: Dr. Derek C. Richardson Department of Astronomy To create an accurate numerical model of solar system formation it is necessary to understand how planetesimals, the planetary building blocks, evolve and grow into larger bodies. Traditio...
متن کاملCore Formation on the Terrestrial Planets: Comparative Planetology
The Boundary Conditions: Basalts from the Earth, the Moon, Mars, and Vesta are strongly depleted in elements that prefer to reside in the metallic state (siderophile elements). Therefore, it is believed that all these bodies have metallic cores. We do not yet have siderophile element analyses of venusian basalts, but we assume that Venus, too, as a terrestrial planet, has a metallic core. For t...
متن کاملFormation of the Terrestrial Planets from a Narrow Annulus
We show that the assembly of the Solar System terrestrial planets can be successfully modelled with all of the mass initially confined to a narrow annulus between 0.7 and 1.0 AU. With this configuration, analogues of Mercury and Mars often form from the collisional evolution of material diffusing out of the annulus under the scattering of the forming Earth and Venus analogues. The final systems...
متن کاملOn the formation of terrestrial planets in hot–Jupiter systems
Context. There are numerous extrasolar giant planets which orbit close to their central stars. These ‘hot-Jupiters’ probably formed in the outer, cooler regions of their protoplanetary disks, and migrated inward to ∼ 0.1 AU. Since these giant planets must have migrated through their inner systems at an early time, it is uncertain whether they could have formed or retained terrestrial planets. A...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: EPJ Web of Conferences
سال: 2011
ISSN: 2100-014X
DOI: 10.1051/epjconf/20111605002