Jupiter & Saturn 4of4: -- and the Building of the Solar System. Konstantin Batygin, California Institute of Technology.

Aug 03, 02:18 AM
Photo:Titan's atmosphere makes Saturn's largest moon look like a fuzzy orange ball in this natural color view from the Cassini spacecraft. Titan's north polar hood is visible at the top of the image, and a faint blue haze also can be detected above the south pole at the bottom of this view. This view looks toward the anti-Saturn side of Titan (3,200 miles, or 5,150 kilometers across). North is up. Images taken using red, green and blue spectral filters were combined to create this natural color view. The images were obtained with the Cassini spacecraft wide-angle camera on Jan. 30, 2012 at a distance of approximately 119,000 miles (191,000 kilometers) from Titan. Image scale is 7 miles (11 kilometers) per pixel.
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  • File:Titan in true color.jpg
  • Created: 30 January 2012

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Jupiter & Saturn 4of4: -- and the Building of the Solar System. Konstantin Batygin, California Institute of Technology.


The early stages of dynamical evolution of planetary systems are often shaped by dissipative processes that drive orbital migration. In multi-planet systems, convergent amassing of orbits inevitably leads to encounters with rational period ratios, which may result in establishment of mean-motion resonances. The success or failure of resonant capture yields exceedingly different subsequent evolutions, and thus plays a central role in determining the ensuing orbital architecture of planetary systems. In this work, we employ an integrable Hamiltonian formalism for first order planetary resonances that allows both secondary bodies to have finite masses and eccentricities, and construct a comprehensive theory for resonant capture. Particularly, we derive conditions under which orbital evolution lies within the adiabatic regime, and provide a generalized criterion for guaranteed resonant locking as well as a procedure for calculating capture probabilities when capture is not certain. Subsequently, we utilize the developed analytical model to examine the evolution of Jupiter and Saturn within the protosolar nebula, and investigate the origins of the dominantly non-resonant orbital distribution of sub-Jovian extrasolar planets. Our calculations show that the commonly observed extrasolar orbital structure can be understood if planet pairs encounter mean-motion commensurabilities on slightly eccentric (e ˜ 0.02) orbits. Accordingly, we speculate that resonant capture among low-mass planets is typically rendered unsuccessful due to subtle axial asymmetries inherent to the global structure of protoplanetary discs.

Monthly Notices of the Royal Astronomical Society, Volume 451, Issue 3, p.2589-2609
Pub Date: August 2015DOI: 10.1093/mnras/stv1063 arXiv: arXiv:1505.01778 Bibcode: 2015MNRAS.451.2589B Keywords: 
  • methods: analytical;
  • celestial mechanics;
  • planets and satellites: dynamical evolution and stability;
  • Astrophysics - Earth and Planetary Astrophysics;
  • Mathematics - Dynamical Systems