scholarly journals Dynamical Shake‐up of Planetary Systems. II.N‐Body Simulations of Solar System Terrestrial Planet Formation Induced by Secular Resonance Sweeping

2008 ◽  
Vol 676 (1) ◽  
pp. 728-739 ◽  
Author(s):  
E. Thommes ◽  
M. Nagasawa ◽  
D. N. C. Lin
Keyword(s):  
Solar System ◽  
Planet Formation ◽  
Planetary Systems ◽  
Terrestrial Planet ◽  
Secular Resonance

scholarly journals N-body Simulations of Planet Formation

2003 ◽  
Vol 208 ◽  
pp. 25-35 ◽  
Author(s):  
Shigeru Ida ◽  
Eiichiro Kokubo ◽  
Junko Kominami
Keyword(s):  
Final Stage ◽  
Planet Formation ◽  
Planetary Systems ◽  
Terrestrial Planet ◽  
The Other ◽  
Other Hand ◽  
Giant Impacts ◽  
Gas Accretion

Accretion from many small planetesimals to planets is reviewed. Solid protoplanets accrete through runaway and oligarchic growth until they become isolated. The isolation mass of protoplanets in terrestrial planet region is about 0.1-0.2 Earth mass, which suggests giant impacts among the protoplanets in the final stage of terrestrial planet formation. On the other hand, the isolation mass in Jupiter's and Saturn's orbits is about a few to 5 Earth masses, which may be massive enough to trigger gas accretion onto the cores. The isolation mass in Uranus and Neptune's orbits is as large as their present cores. Extending the above arguments to extrasolar planetary systems that are formed from disks with various initial masses, we also discuss diversity of extrasolar planetary systems.

scholarly journals Can narrow discs in the inner Solar system explain the four terrestrial planets?

2020 ◽  
Vol 496 (3) ◽  
pp. 3688-3699 ◽  
Author(s):  
Patryk Sofia Lykawka
Keyword(s):  
Solar System ◽  
Planet Formation ◽  
Terrestrial Planet ◽  
Giant Planets ◽  
System Model ◽  
Terrestrial Planets ◽  
P System ◽  
Orbital Mass ◽  
System A ◽  
System 2

ABSTRACT A successful Solar system model must reproduce the four terrestrial planets. Here, we focus on (1) the likelihood of forming Mercury and the four terrestrial planets in the same system (a 4-P system); (2) the orbital properties and masses of each terrestrial planet; and (3) the timing of Earth’s last giant impact and the mass accreted by our planet thereafter. Addressing these constraints, we performed 450 N-body simulations of terrestrial planet formation based on narrow protoplanetary discs with mass confined to 0.7–1.0 au. We identified 164 analogue systems, but only 24 systems contained Mercury analogues, and eight systems were 4-P ones. We found that narrow discs containing a small number of embryos with individual masses comparable to that of Mars and the giant planets on their current orbits yielded the best prospects for satisfying those constraints. However, serious shortcomings remain. The formation of Mercury analogues and 4-P systems was too inefficient (5 per cent and 2 per cent, respectively), and most Venus-to-Earth analogue mass ratios were incorrect. Mercury and Venus analogues also formed too close to each other (∼0.15–0.21 au) compared to reality (0.34 au). Similarly, the mutual distances between the Venus and Earth analogues were greater than those observed (0.34 versus 0.28 au). Furthermore, the Venus–Earth pair was not reproduced in orbital-mass space statistically. Overall, our results suggest serious problems with using narrow discs to explain the inner Solar system. In particular, the formation of Mercury remains an outstanding problem for terrestrial planet formation models.

scholarly journals Terrestrial planet formation in low-mass disks: dependence with initial conditions

2014 ◽  
Vol 9 (S310) ◽  
pp. 218-219
Author(s):  
M. P. Ronco ◽  
G. C. de Elía ◽  
O. M. Guilera
Keyword(s):  
Gas Phase ◽  
Analytical Model ◽  
Ad Hoc ◽  
Planet Formation ◽  
Initial Conditions ◽  
Planetary Systems ◽  
Terrestrial Planet ◽  
Initial Distribution ◽  
Protoplanetary Disk ◽  
Low Mass

AbstractIn general, most of the studies of terrestrial-type planet formation typically use ad hoc initial conditions. In this work we improved the initial conditions described in Ronco & de Elía (2014) starting with a semi-analytical model wich simulates the evolution of the protoplanetary disk during the gas phase. The results of the semi-analytical model are then used as initial conditions for the N-body simulations. We show that the planetary systems considered are not sensitive to the particular initial distribution of embryos and planetesimals and thus, the results are globally similar to those found in the previous work.

scholarly journals RELATIVISTIC EFFECTS IN EXTRASOLAR PLANETARY SYSTEMS

2006 ◽  
Vol 15 (12) ◽  
pp. 2133-2140 ◽  
Author(s):  
FRED C. ADAMS ◽  
GREGORY LAUGHLIN
Keyword(s):  
General Relativity ◽  
Solar System ◽  
Planetary Systems ◽  
Relativistic Effects ◽  
Interaction Theory ◽  
Orbital Elements ◽  
Secular Resonance ◽  
The Future ◽  
General Relativistic ◽  
Temporal Coverage

This paper considers general relativistic (GR) effects in currently observed extrasolar planetary systems. Although GR corrections are small, they can compete with secular interactions in these systems and thereby play an important role. Specifically, some of the observed multiple planet systems are close to secular resonance, where the dynamics is extremely sensitive to GR corrections, and these systems can be used as laboratories to test general relativity. For the three-planet solar system Upsilon Andromedae, secular interaction theory implies an 80% probability of finding the system with its observed orbital elements if GR is correct, compared with only a 2% probability in the absence of GR. In the future, tighter constraints can be obtained with increased temporal coverage.

scholarly journals Terrestrial Planet Formation: The Solar System and Other Systems

2004 ◽  
Vol 202 ◽  
pp. 159-166
Author(s):  
Shigeru Ida ◽  
Eiichiro Kokubo
Keyword(s):  
Solar System ◽  
Final Stage ◽  
Extrasolar Planets ◽  
Planet Formation ◽  
Terrestrial Planet ◽  
The Other ◽  
Terrestrial Planets ◽  
Giant Impacts ◽  
Earth Like Planets ◽  
Jovian Planet

Accretion of terrestrial planets and solid cores of jovian planets is discussed, based on the results of our N-body simulations. Protoplanets accrete from planetesimals through runaway and oligarchic growth until they become isolated. The isolation mass of protoplanets in terrestrial planet region is about 0.2 Earth mass, which suggests that in the final stage of terrestrial planet formation giant impacts between the protoplanets occur. On the other hand, the isolation mass in jovian planet region is about a few to 10 Earth masses, which may be massive enough to form a gas giant. Extending the above arguments to disks with various initial masses, we discuss diversity of planetary systems. We predict that the extrasolar planets so far discovered may correspond to the systems formed from disks with large initial masses and that the other disks with smaller masses, which are the majority of the disks, may form Earth-like planets.

scholarly journals The Diversity of Extrasolar Terrestrial Planets

2009 ◽  
Vol 5 (S265) ◽  
pp. 399-402
Author(s):  
Jade C. Bond ◽  
Dante S. Lauretta ◽  
David P. O'Brien
Keyword(s):  
Chemical Equilibrium ◽  
Planet Formation ◽  
Planetary Systems ◽  
Solid Material ◽  
Terrestrial Planet ◽  
Building Blocks ◽  
Terrestrial Planets ◽  
Dynamical Models ◽  
Diverse Range ◽  
Host Stars

AbstractExtrasolar planetary host stars are enriched in key planet-building elements. These enrichments have the potential to drastically alter the building blocks available for terrestrial planet formation. Here we report on the combination of dynamical models of late-stage terrestrial planet formation within known extrasolar planetary systems with chemical equilibrium models of the composition of solid material within the disk. This allows us to constrain the bulk elemental composition of extrasolar terrestrial planets. A wide variety of resulting planetary compositions exist, ranging from those that are essentially “Earth-like”, containing metallic Fe and Mg-silicates, to those that are dominated by graphite and SiC. This implies that a diverse range of terrestrial planets are likely to exist within extrasolar planetary systems.

scholarly journals Tandem planet formation for solar system-like planetary systems

2017 ◽  
Vol 8 (2) ◽  
pp. 223-231 ◽  
Author(s):  
Yusuke Imaeda ◽  
Toshikazu Ebisuzaki
Keyword(s):  
Solar System ◽  
Planet Formation ◽  
Planetary Systems

scholarly journals Terrestrial planet formation from lost inner solar system material

2021 ◽  
Vol 7 (52) ◽  
Author(s):  
Christoph Burkhardt ◽  
Fridolin Spitzer ◽  
Alessandro Morbidelli ◽  
Gerrit Budde ◽  
Jan H. Render ◽  
...  
Keyword(s):  
Solar System ◽  
Planet Formation ◽  
Terrestrial Planet

Chemical evolution of planetary materials in a dynamic solar nebula

2019 ◽  
Vol 15 (S350) ◽  
pp. 152-157
Author(s):  
Fred J. Ciesla
Keyword(s):  
Solar System ◽  
Chemical Evolution ◽  
Planet Formation ◽  
Solar Nebula ◽  
Planetary Systems ◽  
Protoplanetary Disks ◽  
Complete Picture ◽  
The Sun ◽  
Laboratory Studies ◽  
Planetary Materials

AbstractAs observational facilities improve, providing new insights into the chemistry occurring in protoplanetary disks, it is important to develop more complete pictures of the processes that shapes the chemical evolution of materials during this stage of planet formation. Here we describe how primitive meteorites in our own Solar System can provide insights into the processes that shaped planetary materials early in their evolution around the Sun. In particular, we show how this leads us to expect protoplanetary disks to be very dynamic objects and what modeling and laboratory studies are needed to provide a more complete picture for the early chemical evolution that occurs for planetary systems.

scholarly journals Formation and detectability of Earth-like planets around Alpha-Centauri B

2007 ◽  
Vol 3 (S249) ◽  
pp. 313-318
Author(s):  
Erica Davis
Keyword(s):  
Radial Velocity ◽  
Planet Formation ◽  
Planetary Systems ◽  
Terrestrial Planet ◽  
Mass Range ◽  
Noise Spectrum ◽  
Habitable Zone ◽  
Earth Like Planets ◽  
Late Stages ◽  
High Cadence

AbstractWe simulate the late stages of planet formation around Alpha Centauri B and analyze the detectability of the resulting terrestrial planet systems. The N-body accretionary evolution of a Σ ∝ r−-1 disk populated with 400–900 lunar-mass oligarchs is followed for 200 Myr for each simulation. All of eight runs result in the formation of multiple-planet systems with at least one planet in the 1–2 M⊕ mass range at 0.5–1.5 AU. We examine the detectability of our simulated planetary systems by generating synthetic radial velocity observations including noise based on the radial velocity residuals to the recently published three planet fit to the nearby K0V star HD 69830. Using these synthetic observations, we find that we can reliably detect a 1.8 M⊕ planet in the habitable zone of α Centauri B after only three years of high cadence observations. We also find that the planet is detectable even if the radial velocity precision is 3 ms−1, as long as the noise spectrum is white.

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