Is the Grand Tack model compatible with the orbital distribution of main belt asteroids?
| Autor: | Rodney S. Gomes, Alessandro Morbidelli, Rogerio Deienno, David Nesvorný, Kevin J. Walsh |
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| Rok vydání: | 2017 |
| Předmět: |
Physics
Earth and Planetary Astrophysics (astro-ph.EP) Solar System 010504 meteorology & atmospheric sciences Nice model Giant planet Orbital resonance Astronomy FOS: Physical sciences Astronomy and Astrophysics Astrophysics 01 natural sciences Jumping-Jupiter scenario Space and Planetary Science Asteroid 0103 physical sciences Physics::Space Physics Asteroid belt Astrophysics::Earth and Planetary Astrophysics Formation and evolution of the Solar System 010303 astronomy & astrophysics 0105 earth and related environmental sciences Astrophysics - Earth and Planetary Astrophysics |
| DOI: | 10.48550/arxiv.1701.02775 |
| Popis: | The Asteroid Belt is characterized by the radial mixing of bodies with different physical properties, a very low mass compared to Minimum Mass Solar Nebula expectations and has an excited orbital distribution. Models of the evolution of the Asteroid Belt show that the origin of its structure is strongly linked to the process of terrestrial planet formation. The Grand Tack model presents a possible solution to the conundrum of reconciling the small mass of Mars with the properties of the Asteroid Belt, including the mass depletion, radial mixing and orbital excitation. However, while the inclination distribution produced in the Grand Tack model is in good agreement with the one observed, the eccentricity distribution is skewed towards values larger than those found today. Here, we evaluate the evolution of the orbital properties of the Asteroid Belt from the end of the Grand Tack model (at the end of the gas nebula phase when planets emerge from the dispersing gas disk), throughout the subsequent evolution of the Solar System including an instability of the Giant Planets approximately 400 My later. Before the instability, the terrestrial planets were modeled on dynamically cold orbits with Jupiter and Saturn locked in a 3:2 mean motion resonance. The model continues for an additional 4.1 Gy after the giant planet instability. Our results show that the eccentricity distribution obtained in the Grand Tack model evolves towards one very similar to that currently observed, and the semimajor axis distribution does the same. The inclination distribution remains nearly unchanged with a slight preference for depletion at low inclination; this leads to the conclusion that the inclination distribution at the end of the Grand Tack is a bit over-excited. Comment: published on Icarus |
| Databáze: | OpenAIRE |
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