Dynamics of the Giant Planets of the Solar System in the Gaseous Protoplanetary Disk and Their Relationship to the Current Orbital Architecture

By A. Morbidelli, Kleomenis Tsiganis, A. Crida, Harold Levison, R. Gomes. 2007

274 citations recorded by the source corpus.

We study the orbital evolution of the four giant planets of our solar system in a gas disk. Our investigation extends the previous works by Masset & Snellgrove and Morbidelli & Crida, which focused on the dynamics of the Jupiter-Saturn system. The only systems we found to reach a steady state are those in which the planets are locked in a quadruple mean-motion resonance (i.e., each planet is in resonance with its neighbor). In total, we found six such configurations. For the gas-disk parameters found in Morbidelli & Crida, these configurations are characterized by a negligible migration rate. After the disappearance of the gas, and in the absence of planetesimals, only two of these six configurations (the least compact ones) are stable for a time of hundreds of millions of years or more. The others become unstable on a timescale of a few Myr. Our preliminary simulations show that, when a planetesimal disk is added beyond the orbit of the outermost planet, the planets can evolve from the most stable of these configurations to their current orbits in a fashion qualitatively similar to that described in Tsiganis et al.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/6a735510d95d127b615d01551780c0b2fb401650

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. A. Morbidelli
2. D. Nesvorný
3. S. Raymond
4. D. Charbonneau
5. G. Marcy
6. M. Perryman
7. Timothy Morton
8. J. Johnson

Citations in the corpus

• EVIDENCE FOR SLOW MIGRATION OF NEPTUNE FROM THE INCLINATION DISTRIBUTION OF KUIPER BELT OBJECTS (2015, background): “The case with =a 28N,0 AU and =e 0.3N,0 is similar to runs A, B, and C in Levison et al. (2008), whose choice was motivated by the strong planetary instability occurring in the Nice model (Tsiganis et al. 2005; Morbidelli et al. 2007).”
• Forming the cores of giant planets from the radial pebble flux in protoplanetary discs (2014, result): “To do so, a mass in planetesimals of about 50 ME is required (Morbidelli et al. 2007; Batygin & Brown 2010; Levison et al. 2011), in good agreement with our estimate.”
• Origin and Evolution of Short-period Comets (2017, methodology): “Here we use the model developed in Nesvorný & Morbidelli (2012; hereafter NM12), which was inspired by many previous studies (e.g, Tsiganis et al. 2005, Morbidelli et al. 2007).”
• EVIDENCE FROM THE ASTEROID BELT FOR A VIOLENT PAST EVOLUTION OF JUPITER's ORBIT (2010, background): “This implies that the giant planets had to reside on quasi-circular orbits before the LHB, in accordance withthe hydro-dynamical simulations of Morbidelli et al. (2007) (c.f. the top-left panel of Fig.”
• LATE ORBITAL INSTABILITIES IN THE OUTER PLANETS INDUCED BY INTERACTION WITH A SELF-GRAVITATING PLANETESIMAL DISK (2011, methodology): “5 In the published version of Morbidelli et al. (2007), we claimed to have found only two stable configurations of the giant planets.”
• STATISTICAL STUDY OF THE EARLY SOLAR SYSTEM'S INSTABILITY WITH FOUR, FIVE, AND SIX GIANT PLANETS (2012, methodology): “First, as Morbidelli et al. (2007) was stable. the jump must be rather large, it is hard find cases where PSat/PJup is larger than 2.3 and smaller than 2.5 after the jump.”
• The significance of meteorite density and porosity (2008, background): “Recent dynamical studies (Bottke et al., 2002; Levison and Morbidelli, 2003; Morbidelli et al., 2007) suggest that TNOs are the remnants of bodies that formed outward of the accreting gas-giant planets and were likely ‘‘pushed’’ into their present position in the socalled Kuiper belt by the outward ”
• Oort cloud and Scattered Disc formation during a late dynamical instability in the Solar System (2012, background): “…planetary orbits have been achieved during a phase of dynamical instability of the planets that occurred after gas removal (Tsiganis et al., 2005; Morbidelli et al., 2007), possibly as late as the Late Heavy Bombardment event (approximately 500 Myr after gas removal; Gomes et al., 2005a; Levison…”
• Compositional distributions and evolutionary processes for the near-Earth object population: Results from the MIT-Hawaii Near-Earth Object Spectroscopic Survey (MITHNEOS) (2019, background): “We do not consider this schematic definitive as we recognize that the history of planetessimal scattering in the early solar system (e.g. Gomes et al., 2005; Morbidelli et al., 2007; Walsh et al., 2011) makes the distribution of sources much more complex than can be shown.”
• The Complete Census of 70 μm-Bright Debris Disks within “The Formation and Evolution of Planetary Systems” Spitzer Legacy Survey of Sun-like Stars (2007, background): “Interestingly, there are no planetesimals in this region of the solar system, due to the earlier migration of the outer planets (in particular Neptune; e.g., Morbidelli et al. 2007).”
• Water delivery and giant impacts in the 'Grand Tack' scenario (2014, unknown): “ and Saturn first migrate inwards for 100 kyr then outwards for 500 kyr, with Jupiter reversing its migration at 1.5 AU. Their end locations coincide with the initial conditions in the Nice Model (eg. Morbidelli et al. 2007; Levison et al. 2011), such that Jupiter (a=5.285 AU) and Saturn (a=7.106 AU)”
• Building the terrestrial planets: Constrained accretion in the inner Solar System (2009, methodology): “Given that the “time zero” for our simulations is probably 1-3 Myr after the formation of the Solar Nebula, this is consistent with isotopic measurements.”
• The primordial nucleus of comet 67P/Churyumov-Gerasimenko (2015, background): “…Hubickyj et al. 2005; Dodson-Robinson et al. 2008; Weidenschilling 2008) and migration (e.g., Masset & Snellgrove 2001; Morbidelli & Crida 2007; Morbidelli et al. 2007; Walsh et al. 2011) in a gas disk show that Jupiter, Saturn, Uranus, and Neptune likely had a compact orbital configuration at…”
• DISSIPATIVE DIVERGENCE OF RESONANT ORBITS (2012, background): “Furthermore, it has been shown that multi-resonant states can serve as good candidates for the initial condition of the solar system (Morbidelli et al. 2007; Batygin & Brown 2010).”
• Constructing the secular architecture of the solar system II: The terrestrial planets (2009, unknown): “As a consequence, if Jupiter passed through or was originally close to the 2:1 resonance with Saturn, as in the Nice model (Tsiganis et al. 2005; Gomes et al. 2005; Morbidelli et al. 2007) or in the scenario of Thommes et al. (2007), also the secular resonances g5 = g4 and g5 = g3 had to be crossed.”
• Accretion and differentiation of the terrestrial planets with implications for the compositions of early-formed Solar System bodies and accretion of water (2014, background): “These locations are appropriate for a late giant planet instability at ~500 Myr (Nice model; Morbidelli et al., 2007) that will place them and the outer ice giants (Neptune and 5 Uranus) on their current orbits (Levison et al., 2011).”