Review of the works on the orbital evolution of solar system major planets

Холшевников, К. В.; Kuznetsov, E. D.

doi:10.1134/s0038094607040016

Cited by 12 publications

(6 citation statements)

References 66 publications

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“…With a MS lifetime of over 10 Gyr, a Solar-mass, Solar-metallicity star with orbiting planets is particularly prohibitive to integrate. This long timescale helps explain the uncertainties in long-term evolution of the Solar System planets (Kholshevnikov & Kuznetsov 2007;Laskar et al 2011). Figure 6 provides estimates for the number of planetary orbits that would be achieved during the MS as a function of stellar progenitor mass, for a variety of planetary semimajor axes.…”

Section: Main Sequence Timescalesmentioning

confidence: 99%

Simulations of two-planet systems through all phases of stellar evolution: implications for the instability boundary and white dwarf pollution

Veras

Mustill

Bonsor

et al. 2013

Monthly Notices of the Royal Astronomical Society

183

205

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Exoplanets have been observed at many stages of their host star's life, including the main sequence (MS), subgiant and red giant branch stages. Also, polluted white dwarfs (WDs) likely represent dynamically active systems at late times. Here, we perform 3-body simulations which include realistic post-MS stellar mass loss and span the entire lifetime of exosystems with two massive planets, from the endpoint of formation to several Gyr into the WD phase of the host star. We find that both MS and WD systems experience ejections and star-planet collisions (Lagrange instability) even if the planet-planet separation well-exceeds the analytical orbit-crossing (Hill instability) boundary. Consequently, MS-stable planets do not need to be closely-packed to experience instability during the WD phase. This instability may pollute the WD directly through collisions, or, more likely, indirectly through increased scattering of smaller bodies such as asteroids or comets. Our simulations show that this instability occurs predominately between tens of Myr to a few Gyrs of WD cooling.A planet's life may be split into four distinct stages: 1) formation and concurrent dynamical excitation, 2) main sequence (MS) evolution, 3) evolution during post-MS stellar phase changes, and 4) white dwarf (WD) evolution. The first stage generally lasts no longer than 0.1% of the entire MS lifetime. The second stage is relatively dynamically quiescent, with only occasional but often important scattering interactions. In the third stage, the planet is subject to dynamical changes due to the star's violent actions as it becomes a giant. In the final stage, the star has become a WD, and the planet again enters and remains in a phase of relative dynamical quiescence occasionally punctuated by scattering interactions or external forcing. This general picture, which does not include possibilities such as the capture of free-floating planets, planetary destruction due to supernovae, or multiple host stars, describes the life cycle of the vast majority of known exoplanets.The volume of planetary literature investigating the ⋆

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Section: Main Sequence Timescalesmentioning

confidence: 99%

Simulations of two-planet systems through all phases of stellar evolution: implications for the instability boundary and white dwarf pollution

Veras

Mustill

Bonsor

et al. 2013

Monthly Notices of the Royal Astronomical Society

183

205

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“…Instead, the primary driver of dynamical change in the Solar System during the Sun's main sequence will arise from the mutual secular perturbations of the orbiting bodies. Kholshevnikov & Kuznetsov (2007) provide a comprehensive review of the investigations up until the year 2007 which have contributed to our understanding of this evolution. These studies describe orbital evolution beyond 10 4 yrs from now in a primarily qualitative manner because numerical integrations typically cannot retain the orbital phase information of the terrestrial planets over the Sun's main sequence lifetime.…”

Section: Introductionmentioning

confidence: 99%

The Solar system’s post-main-sequence escape boundary

Veras

Wyatt

2012

Monthly Notices of the Royal Astronomical Society

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The Sun will eventually lose about half of its current mass non‐linearly over several phases of post‐main‐sequence evolution. This mass loss will cause any surviving orbiting body to increase its semimajor axis and perhaps vary its eccentricity. Here, we use a range of solar models spanning plausible evolutionary sequences and assume isotropic mass loss to assess the possibility of escape from the Solar system. We find that the critical semimajor axis in the Solar system within which an orbiting body is guaranteed to remain bound to the dying Sun due to perturbations from stellar mass loss alone is ≈103–104 au. The fate of objects near or beyond this critical semimajor axis, such as the Oort Cloud, outer scattered disc and specific bodies such as Sedna, will significantly depend on their locations along their orbits when the Sun turns off the main sequence. These results are applicable to any exoplanetary system containing a single star with a mass, metallicity and age which are approximately equal to the Sun’s, and suggest that few extrasolar Oort Clouds could survive post‐main‐sequence evolution intact.

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“…In this moment by the investigations of above mentioned authors the following ideas about the dynamic properties of the Solar system on long time intervals are formed. It is fully reviewed in [17]. The planetary motion in the Solar system is quasi-periodic on time scales of about 10 6 − 10 7 years.…”

Section: Introductionmentioning

confidence: 99%

The construction of averaged planetary motion theory by means of computer algebra system Piranha

Perminov,

Kuznetsov

2018

Preprint

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The application of computer algebra system Piranha to the investigation of the planetary problem is described in this work. Piranha is an echeloned Poisson series processor authored by F. Biscani from Max Planck Institute for Astronomy in Heidelberg. Using Piranha the averaged semi-analytical motion theory of four-planetary system is constructed up to the second degree of planetary masses. In this work we use the algorithm of the Hamiltonian expansion into the Poisson series in only orbital elements without other variables. The motion equations are obtained analytically in time-averaged elements by Hori-Deprit method. Piranha showed high-performance of analytical manipulations. Different properties of obtained series are discussed. The numerical integration of the motion equations is performed by Everhart method for the Solar system's giantplanets and some exoplanetary systems.

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Review of the works on the orbital evolution of solar system major planets

Cited by 12 publications

References 66 publications

Simulations of two-planet systems through all phases of stellar evolution: implications for the instability boundary and white dwarf pollution

Simulations of two-planet systems through all phases of stellar evolution: implications for the instability boundary and white dwarf pollution

The Solar system’s post-main-sequence escape boundary

The construction of averaged planetary motion theory by means of computer algebra system Piranha

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