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The great dichotomy of the Solar System: Small terrestrial embryos and massive giant planet cores [PDF]
Icarus, 2015 In press in ...
Alessandro Morbidelli, Seth A. Jacobson
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Did the terrestrial planets of the solar system form by pebble accretion?
Earth and Planetary Science LettersThe dominant accretion process leading to the formation of the terrestrial planets of the Solar System is a subject of intense scientific debate. Two radically different scenarios have been proposed. The classic scenario starts from a disk of planetesimals which, by mutual collisions, produce a set of Moon to Mars-mass planetary embryos.
Alessandro Morbidelli +2 more
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A Consistent Model of Terrestrial Planet Magnetospheres and Rotations in Our Solar System ()
World Journal of Condensed Matter Physics, 2021 The Sun comprises 99.9% of the solar system mass so it is expected that Sun terrestrial planet interactions can influence the motion as well as the rotation of the terrestrial planets. Gravity affects the planet orbital motions while the changing magnetic fields of the Sun can influence the planet rotations.
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Orbital stability of massive protoplanets in the terrestrial planet region of the solar system
The Moon and the Planets, 1978A number of theories of the formation of the planets advocate that the terrestrial planets were originally of cosmic composition and that it is only subsequent evolution that has removed their volatile components. This paper shows that such protoplanets could have remained in the terrestrial planet region without significant changes occurring in their ...
J R Donnison, I P Williams
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Astrophysical Journal, 2012 A model of coupled mantle convection and planetary tectonics is used to demonstrate that history dependence can outweigh the effects of a planet's energy content and material parameters in determining its tectonic state. The mantle convection-surface tectonics system allows multiple tectonic modes to exist for equivalent planetary parameter values. The
Adrian Lenardic
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Atmospheric Escape from Solar System Terrestrial Planets and Exoplanets
Annual Review of Earth and Planetary Sciences, 2015It has been known for decades that atmospheric escape is important for the evolution of terrestrial planets in the Solar System, although exactly how atmospheric escape changes the atmospheres of these bodies is still hotly debated. Rapidly increasing numbers of exoplanet observations provide new targets against which atmospheric escape models are ...
Feng Tian
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Formation of the terrestrial planets in the solar system around 1 au via radial concentration of planetesimals [PDF]
Astronomy and Astrophysics, 2018 Context. No planets exist inside the orbit of Mercury and the terrestrial planets of the solar system exhibit a localized configuration. According to thermal structure calculation of protoplanetary disks, a silicate condensation line (~1300 K) is located around 0.1 au from the Sun except for the early phase of disk evolution, and planetesimals could ...
Alessandro Morbidelli +2 more
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Late Accretion and the Origin of Water on Terrestrial Planets in the Solar System
2021<p>Terrestrial planets in the Solar system generally lack surface liquid water. Earth is at odd with this observation and with the idea of the giant Moon-forming impact that should have vaporized any pre-existing water, leaving behind a dry Earth.
Cédric Gillmann +6 more
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Impact bombardment of the terrestrial planets and the early history of the Solar System
Nature Geoscience, 2013About 4 billion years ago, the terrestrial planets were bombarded by asteroids following an orbital shake-up of the outer Solar System. Lunar samples, planetary cratering records and dynamical models piece together an increasingly coherent view of this bombardment interval.
Caleb I. Fassett, David A. Minton
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A Postulated Planetary Collision, the Terrestrial Planets, the Moon and Smaller Solar-System Bodies
Earth, Moon, and Planets, 2013In a scenario produced by the Capture Theory of planetary formation, a collision between erstwhile solar-system giant planets, of masses 798.75 and 598.37 M⊕, is simulated using smoothed-particle hydrodynamics. Due to grain-surface chemistry that takes place in star-forming clouds, molecular species containing hydrogen, with a high D/H ratio taken as 0.
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