Orbital Evolution of a Saturn-Jupiter configuration within a disk

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Orbital Evolution of a Saturn-Jupiter configuration within a disk

Post by Sirius_Alpha on 26th July 2010, 8:26 pm

On the orbital evolution of a giant planet pair embedded in a gaseous disk. II. A Saturn-Jupiter configuration
http://arxiv.org/abs/1007.4520

Abstract wrote:We carry out a series of high-resolution (1024 X 1024) hydrodynamic simulations to investigate the orbital evolution of a Saturn-Jupiter pair embedded in a gaseous disk. This work extends the results of our previous work by exploring a different orbital configuration---Jupiter lies outside Saturn (q<1, where q= M_i/M_o is the mass ratio of the inner planet and the outer one). We focus on the effects of different initial separations (d) between the two planets and the various surface density profiles of the disk, where \sigma \propto r^{-\alpha}. We also compare the results of different orbital configurations of the planet pair. Our results show that: (1) when the initial separation is relatively large(d>d_{iLr}, where d_{iLr} is the distance between Jupiter and its first inner Lindblad resonance), the two planets undergo divergent migration. However, the inward migration of Saturn could be halted when Jupiter compresses the inner disk in which Saturn is embedded. (2) Convergent migration occurs when the initial separation is smaller (d<d_{iLr}) and the density slope of the disk is nearly flat (\alpha<1/2). Saturn is then forced by Jupiter to migrate inward when the two planets are trapped into mean motion resonances (MMRs), and Saturn may get very close to the central star. (3) In the case of q<1, the eccentricity of Saturn could be excited to a very high value (e_{S}~0.4-0.5) by the MMRs and the system could maintain stability. These results explain the formation of MMRs in the exoplanet systems where the outer planet is more massive than the inner one. It also helps us to understand the origin of the "hot Jupiter/Saturn" undergoing high eccentric orbit.

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Re: Orbital Evolution of a Saturn-Jupiter configuration within a disk

Post by Roland Borrey on 26th September 2010, 9:54 pm

Comprehension of the Hot Jupiter/Saturn evolution is fundamental to understading of planetary systems stability (the fundamental necessity for the evolution of life) the mentionned paper is an eye opener on how the planetary system get stabilized in its early life.
If I read this right, a hot Jupiter means that the planetary system has been gobble by the star, and generaly any planet too close to the star is not a good sign of stability.
If this is true, we are currently discovering planetary system ruins. It could be advisable to switch the search for giant planet with period between 800 and 2000 days then look for earth twins in these system.

This paper has a part one, does any body knows where to find it?
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Re: Orbital Evolution of a Saturn-Jupiter configuration within a disk

Post by Sirius_Alpha on 26th September 2010, 10:09 pm

I'm not sure where to find a part 1 to the paper.

Also, I would disagree about systems with hot Jupiters representing the remains of systems, citing 55 Cnc, HD 74156, HD 37124 (WASP-3 and 10 if the TTVs turn out to be real) and perhaps Gliese 581 as examples. Hot Jupiter migration should occur early enough that it may not entirely clear the rest of the disk that it migrates through, allowing for future terrestrial planet formation.

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Re: Orbital Evolution of a Saturn-Jupiter configuration within a disk

Post by Roland Borrey on 29th September 2010, 4:37 pm

For whoever is interested, here is the part 1 of the paper
On the orbital evolution of a giant planet pair embedded in a gaseous disk. I: Jupiter-Saturn configuration http://arxiv.org/abs/1002.2201
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