The dynamics of Jupiter and Saturn in the gaseous protoplanetary disk

By Morbidelli Alessandro, A. Crida. 2007

191 citations recorded by the source corpus.

Abstract We study the possibility that the mutual interactions between Jupiter and Saturn prevented Type II migration from driving these planets much closer to the Sun. Our work extends previous results by Masset and Snellgrove [Masset, F., Snellgrove, M., 2001. Mon. Not. R. Astron. Soc. 320, L55–L59], by exploring a wider set of initial conditions and disk parameters, and by using a new hydrodynamical code that properly describes for the global viscous evolution of the disk. Initially both planets migrate towards the Sun, and Saturn's migration tends to be faster. As a consequence, they eventually end up locked in a mean motion resonance. If this happens in the 2:3 resonance, the resonant motion is particularly stable, and the gaps opened by the planets in the disk may overlap. This causes a drastic change in the torque balance for the two planets, which substantially slows down the planets' inward migration. If the gap overlap is substantial, planet migration may even be stopped or reversed. As the widths of the gaps depend on disk viscosity and scale height, this mechanism is particularly efficient in low viscosity, cool disks. The initial locking of the planets in the 2:3 resonance is a likely outcome if Saturn formed at the edge of Jupiter's gap, but also if Saturn initially migrated rapidly from further away. We also explore the possibility of trapping in other resonances, and the subsequent evolutions. We discuss the compatibility of our results with the initial conditions adopted in Tsiganis et al. [Tsiganis, K., Gomes, R., Morbidelli, A., Levison, H.F., 2005. Nature 435, 459–461] and Gomes et al. [Gomes, R., Levison, H.F., Tsiganis, K., Morbidelli, A., 2005. Nature 435, 466–469] to explain the current orbital architecture of the giant planets and the origin of the Late Heavy Bombardment of the Moon.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/1ed2fc9a04be33c8a62607cdab28272082f5cf6a

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Citations in the corpus

Origin and evolution of the atmospheres of early Venus, Earth and Mars (2018, methodology): “After the accretion of gas, Saturn migrated also inward but faster than Jupiter (e.g., Masset and Papaloizou 2003) and entered into a 2:3 mean motion resonance with Jupiter (Masset and Snellgrove 2001; Morbidelli and Crida 2007; Pierens and Nelson 2008).”
EVIDENCE FROM THE ASTEROID BELT FOR A VIOLENT PAST EVOLUTION OF JUPITER's ORBIT (2010, background): “Depending on the disk parameters, the two planets either stay in place, or migate outward in resonance, until the disappearance of the disk (Morbidelli and Crida, 2007).”
Constructing the secular architecture of the solar system II: The terrestrial planets (2009, unknown): “More precisely, Jupiter and Saturn are trapped in their mutual 3:2 resonance (see also Masset & Snellgrove 2001; Morbidelli & Crida 2007; Pierens & Nelson 2008); Uranus is in the 3:2 resonance with Saturn and Neptune is caught in the 4:3 resonance with Uranus.”
Building Terrestrial Planets (2012, background): “…of tens of millions of years into two Earth-mass planets at ∼0.7 AU and 1 AU and a small Mars at 1.5 AU (see Figure 4). typically migrate outward, locked in a 2:3 mean motion resonance (in which the orbital period of Saturn is 3/2 that of Jupiter; Masset & Snellgrove 2001, Morbidelli & Crida 2007).”
Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion (2017, methodology): “At this point the direction of migration was reversed (Masset and Snellgrove, 2001; Morbidelli and Crida, 2007; Pierens and Nelson, 2008) and the two planets migrated back outward until the disk dispersed (Pierens and Raymond, 2011).”
Water delivery and giant impacts in the 'Grand Tack' scenario (2014, background): “For the “disk” population, the corresponding factors are 28.0 with q<1.5 AU and 44.5 with q<2.0 AU. We can find the total masses of the q<1.5 AU and q<2.0 AU belts and disk populations using these factors and the total implanted mass of C-type material (3.9 × 10 M⊕) calculated above. The total mass ”
Dynamics of Protoplanetary Disks (2010, background): “In other instances, however, the overlapping gravitational torques from multiple gas giant planets (Morbidelli & Crida 2007, Z. Zhu, private communication), acting in concert more like a viscous process, may be needed if one is to explain the data within a planetary scenario.”
YOUNG SOLAR SYSTEM's FIFTH GIANT PLANET? (2011, background): “Jupiter and Saturn, for example, were most likely trapped in the 3:2 resonance (Masset & Snellgrove 2001, Morbidelli & Crida 2007, Pierens & Nelson 2008), defined as PSaturn/PJupiter = 1.5, where PJupiter and PSaturn are the orbital periods of Jupiter and Saturn (this ratio is 2.49 today).”
The great dichotomy of the Solar System: Small terrestrial embryos and massive giant planet cores (2015, background): “The key aspect of the Solar System evolution was that Jupiter avoided to migrate inwards of a few AU, probably due to the presence of Saturn (Masset and Snellgrove, 2001; Morbidelli and Crida, 2007; Walsh et al., 2011).”
Dynamics of the Giant Planets of the Solar System in the Gaseous Protoplanetary Disk and Their Relationship to the Current Orbital Architecture (2007, result): “This event excited their orbital eccentricities to values similar to those presently observed.”
STATISTICAL STUDY OF THE EARLY SOLAR SYSTEM'S INSTABILITY WITH FOUR, FIVE, AND SIX GIANT PLANETS (2012, background): “Jupiter and Saturn, for example, were most likely trapped in the 3:2 resonance (Masset & Snellgrove 2001, Morbidelli & Crida 2007, Pierens & Nelson 2008, Pierens & Raymond 2011, Walsh et al. 2011), defined as PSat/PJup = 1.5, where PJup and PSat are the orbital periods of Jupiter and Saturn (this…”
Accretion and differentiation of the terrestrial planets with implications for the compositions of early-formed Solar System bodies and accretion of water (2014, background): “Meanwhile, Saturn’s mass grows linearly from 10 Me to its current mass, and when it reaches a mass close to its current mass the migration physics in the resonance changes and the giant planets then migrate outwards (Masset and Snellgrove, 2001; Morbidelli and Crida, 2007; Pierens and Nelson, 2008).”
Forming the cores of giant planets from the radial pebble flux in protoplanetary discs (2014, background): “This is a desirable feature for the Grand Tack scenario (Masset & Snellgrove 2001; Morbidelli & Crida 2007; Walsh et al. 2011), where Saturn catches up with Jupiter to share a common gap, which leads to outward migration.”
THE FORMATION MECHANISM OF GAS GIANTS ON WIDE ORBITS (2009, unknown): “In addition, Morbidelli & Crida (2007) propose that two giant planets in a 2:3 mean motion resonance that open overlapping gaps in the disk may halt or reverse the normally inward Type II migration process.”