Stability and Instability of the Terrestrial Protoplanet System and Their Possible Roles in the Final Stage of Planet Formation

Itô, Takashi; Tanikawa, Kiyotaka

doi:10.1006/icar.1999.6112

Cited by 45 publications

(32 citation statements)

References 27 publications

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“…Such interplay affects the long-term stability of this type of orbits. Ito & Tanikawa (1999) argued that the terrestrial planets share the effect of the secular perturbation from Jupiter. In particular, the Earth shares the increase in eccentricity of Venus on the long term; the two planets exchange angular momentum (Ito & Tanikawa 2002).…”

Section: Relative Eccentricity-relative Argument Of Perihelionmentioning

confidence: 99%

Infrequent visitors of the Kozai kind: the dynamical lives of 2012 FC₇₁, 2014 EK₂₄, 2014 QD₃₆₄, and 2014 UR

Marcos¹,

Marcos²

2015

A&A

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Context. Asteroids with semi-major axes very close to that of a host planet can avoid node crossings when their nodal points are at perihelion and at aphelion. This layout protects the asteroids from close encounters, and eventual collisions, with the host planet. Aims. Here, we study the short-term dynamical evolution of four recently discovered near-Earth asteroids (NEAs) -2012 FC 71 , 2014 EK 24 , 2014 , and 2014 UR -that follow very Earth-like orbits. Methods. Our analysis is based on results of direct N-body calculations that use the most updated ephemerides and include perturbations from the eight major planets, the Moon, the barycentre of the Pluto-Charon system, and the three largest asteroids. Results. These four NEAs exhibit an orbital evolution unlike any other known near-Earth object (NEO). Beyond horseshoe, tadpole, or quasi-satellite trajectories, they follow co-orbital passing orbits relative to the Earth within the Kozai domain. Our calculations show that secular interactions induce librations of their relative argument of perihelion with respect to our planet but also to Venus, Mars, and Jupiter. Secular chaos is also present. The size of this transient population is probably large. Conclusions. Although some of these NEAs can remain orbitally stable for many thousands of years, their secular dynamics are substantially more complicated than commonly thought and cannot be properly described within the framework of the three-body problem alone owing to the overlapping of multiple secular resonances. Objects in this group are amongst the most atypical NEOs regarding favourable visibility windows because these are separated in time by many decades or even several centuries.

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Section: Relative Eccentricity-relative Argument Of Perihelionmentioning

confidence: 99%

Infrequent visitors of the Kozai kind: the dynamical lives of 2012 FC₇₁, 2014 EK₂₄, 2014 QD₃₆₄, and 2014 UR

Marcos¹,

Marcos²

2015

A&A

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“…Timescales for orbital instability to occur (T cross ) very sensitively depend on orbital separation between planets, their eccentricities, and masses (Chambers et al 1996;Chambers & Wetherill 1998;Ito & Tanikawa 1999Yoshinaga et al 1999). Chambers et al (1996) found that for systems with equal-mass (m) planets in initially almost circular orbits of orbital separation bR H , log T cross ¼ b þ , where and are constants in terms of b.…”

Section: Planet-planet Interactionsmentioning

confidence: 99%

Formation of Hot Planets by a Combination of Planet Scattering, Tidal Circularization, and the Kozai Mechanism

Nagasawa

Ida

Bessho

2008

ApJ

486

530

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We have investigated the formation of close-in extrasolar giant planets through a coupling effect of mutual scattering, the Kozai mechanism, and tidal circularization, by orbital integrations. Close-in gas giants would have been originally formed at several AU beyond the ice lines in protoplanetary disks and migrated close to their host stars. Although type II migration due to planet-disk interactions may be a major channel for the migration, we show that this scattering process would also give a nonnegligible contribution. We carried out orbital integrations of three planets with Jupiter mass, directly including the effect of tidal circularization. We have found that in about 30% of the runs close-in planets are formed, which is much higher than suggested by previous studies. Three-planet orbit crossing usually results in the ejection of one or two planets. Tidal circularization often occurs during three-planet orbit crossing, but previous studies have monitored only the final stage after the ejection, significantly underestimating the formation probability. We have found that the Kozai mechanism in outer planets is responsible for the formation of close-in planets. During three-planet orbital crossing, Kozai excitation is repeated and the eccentricity is often increased secularly to values close enough to unity for tidal circularization to transform the inner planet to a close-in planet. Since a moderate eccentricity can retain for the close-in planet, this mechanism may account for the observed close-in planets with moderate eccentricities and without nearby secondary planets. Since these planets also remain a broad range of orbital inclinations (even retrograde ones), the contribution of this process would be clarified by more observations of Rossiter-McLaughlin effects for transiting planets.

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“…Without the damping force by remnant planetesimals and /or gas, a multiple protoplanet system undergoes an orbital instability after a certain time T inst . This instability time T inst depends on the orbital separation, eccentricities, and absolute mass of protoplanets (Chambers et al 1996;Ito & Tanikawa 1999;Yoshinaga et al 1999;Iwasaki & Ohtsuki 2006). We switch the code and reduce the value of g from 4.3 to 1 at t ¼ 10 5 yr. For run 6, T inst at this time is estimated to be 10 5 Y10 6 yr from above studies.…”

Section: An Example Of Evolution: Runmentioning

confidence: 99%

Formation and Accretion History of Terrestrial Planets from Runaway Growth through to Late Time: Implications for Orbital Eccentricity

Morishima

Schmidt

Stadel

et al. 2008

Astrophysical Journal

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Remnant planetesimals might have played an important role in reducing the orbital eccentricities of the terrestrial planets after their formation via giant impacts. However, the population and the size distribution of remnant planetesimals during and after the giant impact stage are unknown, because simulations of planetary accretion in the runaway growth and giant impact stages have been conducted independently. Here we report results of direct N-body simulations of the formation of terrestrial planets beginning with a compact planetesimal disk. The initial planetesimal disk has a total mass and angular momentum as observed for the terrestrial planets, and we vary the width (0.3 and 0.5 AU ) and the number of planetesimals (1000Y5000). This initial configuration generally gives rise to three final planets of similar size, and sometimes a fourth small planet forms near the location of Mars. Since a sufficient number of planetesimals remains, even after the giant impact phase, the final orbital eccentricities are as small as those of the Earth and Venus.

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Stability and Instability of the Terrestrial Protoplanet System and Their Possible Roles in the Final Stage of Planet Formation

Cited by 45 publications

References 27 publications

Infrequent visitors of the Kozai kind: the dynamical lives of 2012 FC₇₁, 2014 EK₂₄, 2014 QD₃₆₄, and 2014 UR

Infrequent visitors of the Kozai kind: the dynamical lives of 2012 FC₇₁, 2014 EK₂₄, 2014 QD₃₆₄, and 2014 UR

Formation of Hot Planets by a Combination of Planet Scattering, Tidal Circularization, and the Kozai Mechanism

Formation and Accretion History of Terrestrial Planets from Runaway Growth through to Late Time: Implications for Orbital Eccentricity

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Stability and Instability of the Terrestrial Protoplanet System and Their Possible Roles in the Final Stage of Planet Formation

Cited by 45 publications

References 27 publications

Infrequent visitors of the Kozai kind: the dynamical lives of 2012 FC71, 2014 EK24, 2014 QD364, and 2014 UR

Infrequent visitors of the Kozai kind: the dynamical lives of 2012 FC71, 2014 EK24, 2014 QD364, and 2014 UR

Formation of Hot Planets by a Combination of Planet Scattering, Tidal Circularization, and the Kozai Mechanism

Formation and Accretion History of Terrestrial Planets from Runaway Growth through to Late Time: Implications for Orbital Eccentricity

Contact Info

Product

Resources

About

Infrequent visitors of the Kozai kind: the dynamical lives of 2012 FC₇₁, 2014 EK₂₄, 2014 QD₃₆₄, and 2014 UR

Infrequent visitors of the Kozai kind: the dynamical lives of 2012 FC₇₁, 2014 EK₂₄, 2014 QD₃₆₄, and 2014 UR