Constructing the secular architecture of the solar system II: The terrestrial planets

By R. Brasser, A. Morbidelli, Rodney Gomes, K. Tsiganis, Harold Levison. 2009

132 citations recorded by the source corpus.

We investigate the dynamical evolution of the terrestrial planets during the planetesimal-driven migration of the giant planets. A basic assumption of this work is that giant planet migration occurred after the completion of terrestrial planet formation, such as in the models that link the former to the origin of the Late Heavy Bombardment. The divergent migration of Jupiter and Saturn causes the g5 eigenfrequency to cross resonances of the form g5=gk with k ranging from 1 to 4. Consequently these secular resonances cause large-amplitude responses in the eccentricities of the terrestrial planets. We show that the resonances g5=g_4 and g5=g3 do not pose a problem if Jupiter and Saturn have a fast approach and departure from their mutual 2:1 mean motion resonance. On the other hand, the resonance crossings g5=g2 and g5=g1 are more of a concern as they tend to yield a terrestrial system incompatible with the current one. We offer two solutions to this problem. The first uses the fact that a secular resonance crossing can also damp the amplitude of a Fourier mode if the latter is large originally. A second scenario involves a 'jumping Jupiter' in which encounters between an ice giant and Jupiter, without ejection of the former, cause the latter to migrate away from Saturn much faster than if migration is driven solely by encounters with planetesimals. In this case, the g5=g2 and g5=g1 resonances can be jumped over, or occur very briefly.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/33601388ab97db8532b1bf21dbbd721b7959ed86

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Citations in the corpus

LATE ORBITAL INSTABILITIES IN THE OUTER PLANETS INDUCED BY INTERACTION WITH A SELF-GRAVITATING PLANETESIMAL DISK (2011, background): “It is the only migration model that is consistent with the current dynamical structure of the terrestrial planets (Brasser et al. 2009) and the main asteroid belt (Morbidelli et al. 2010).”
Debris disks as signposts of terrestrial planet formation (2011, background): “One explanation for the Earth and Venus’ orbits is that they formed in a dissipative environment but that were later dynamically perturbed during the instability that caused the late heavy bombardment (Gomes et al. 2005; Brasser et al. 2009; Morbidelli et al. 2010).”
YOUNG SOLAR SYSTEM's FIFTH GIANT PLANET? (2011, background): “This may become a problem, if g5 slowly swipes over the g1 or g2 modes, because the strong g1 = g5 and g2 = g5 resonances can produce excessive excitation and instabilities in the terrestrial planet system (Brasser et al. 2009, Agnor & Lin 2011).”
EVIDENCE FROM THE ASTEROID BELT FOR A VIOLENT PAST EVOLUTION OF JUPITER's ORBIT (2010, background): “In two previous studies, Morbidelli et al. (2009) and Brasser et al. (2009), henceforth labelled Paper I and Paper II respectively, we investigated how the giant planets (Paper I) and the terrestrial planets (Paper II) could have achieved orbits with their curent secular properties i.e. with their…”
A sawtooth-like timeline for the first billion years of lunar bombardment (2012, background): “Brasser et al. (2009) argued that the orbits of the terrestrial planets might have been significantly more circular and less inclined than the current orbits.”
FORETELLINGS OF RAGNARÖK: WORLD-ENGULFING ASYMPTOTIC GIANTS AND THE INHERITANCE OF WHITE DWARFS (2012, unknown): “2005; Brasser et al. 2009).”
EVIDENCE FOR SLOW MIGRATION OF NEPTUNE FROM THE INCLINATION DISTRIBUTION OF KUIPER BELT OBJECTS (2015, methodology): “A potentially more viable instability model, known as the jumping-Jupiter model, was later developed to avoid these problems (e.g., Brasser et al. 2009; Morbidelli et al. 2009a).”
CAPTURE OF TROJANS BY JUMPING JUPITER (2013, methodology): “…jumping-Jupiter model, is required to explain the secular architecture of the outer planets, orbital distribution of asteroids, and dynamical survival of the terrestrial planets (Morbidelli et al. 2009b, 2010, Brasser et al. 2009, Minton & Malhotra 2009, Walsh & Morbidelli 2011, Agnor & Lin 2012).”
Building Terrestrial Planets (2012, background): “…synthetic terrestrial planets with an AMD of −0.001, which is even smaller than the real one (the reader should keep in mind that the terrestrial planets might have achieved the current AMD after their formation, during a phase of late orbital migration of the giant planets; Brasser et al. 2009).”
STATISTICAL STUDY OF THE EARLY SOLAR SYSTEM'S INSTABILITY WITH FOUR, FIVE, AND SIX GIANT PLANETS (2012, background): “This may become a problem, if g5 slowly swipes over the g1 or g2 modes, because the strong g1 = g5 and g2 = g5 resonances can produce excessive excitation and instabilities in the terrestrial planet system (Brasser et al. 2009, Agnor & Lin 2011).”
Oort cloud and Scattered Disc formation during a late dynamical instability in the Solar System (2012, methodology): “The migration was accomplished by interpolation of the planets’ orbital elements with SWIFT RMVS3 (Petit et al., 2001; Brasser et al., 2009; Morbidelli et al., 2010).”