Eccentric Extrasolar Planets: The Jumping Jupiter Model

By F. Marzari, S. Weidenschilling. 2002

216 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/247629622bc9bff499b02d6a8dedb0b208c981a8

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In Astronomy and Astrophysics

Citations in the corpus

Five New Extrasolar Planets (2005, background): “The presence of a second giant planet, in the form of Keplerian variation or long-term trends in the velocities, adds weight to models that invoke other giant planets to perturb the observed planet into its eccentric orbit (Marzari & Weidenschilling 2002; Ford et al. 2003).”
Tidal obliquity evolution of potentially habitable planets (2011, background): “Moreover, the high eccentricity of Gl581 d (Mayor et al. 2009), likely induced by planet-planet scattering (Marzari & Weidenschilling 2002), suggests a significant inclination between the orbits of planet e through f.”
Dynamical Outcomes of Planet-Planet Scattering (2007, background): “While planetary systems with more than two planets can not be provably stable, they can remain stable for very long timescales depending on their initial separations (Chambers et al. 1996; Marzari & Weidenschilling 2002).”
Toward a Deterministic Model of Planetary Formation. II. The Formation and Retention of Gas Giant Planets around Stars with a Range of Metallicities (2004, background): “The outer boundary radius of the distribution of gas giants aout / 10(10=27) Z (Paper I ), although interactions among gas giants, which are not taken into account in the present paper, may make the boundary less clear (Marzari & Weidenschilling 2002).”
Properties of planets in binary systems - The role of binary separation (2006, background): “…planet eccentricity up to 0.4–0.5 that are independent of the binarity of the planet host, and are characteristic of formation and evolution of a planetary system (e.g. disk-planet interactions: Tremaine & Zakamska 2004; planet-planet scattering: Marzari & Weidenschilling 2002; Ford et al. 2003).”
Formation of Hot Planets by a Combination of Planet Scattering, Tidal Circularization, and the Kozai Mechanism (2008, methodology): “On longer timescales than formation timescales, the multiple gas giant systems can be orbitally unstable (Lin & Ida 1997; Marzari & Weidenschilling 2002).”
MULTIPLE-PLANET SCATTERING AND THE ORIGIN OF HOT JUPITERS (2011, background): “While many works considered planet scattering (e.g. Marzari & Weidenschilling 2002, Chatterjee et al. 2008, Juric & Tremaine 2008), Nagasawa et al. (2008) pioneered the statistical studies of planet scattering with tidal effects.”
Origins of Eccentric Extrasolar Planets: Testing the Planet-Planet Scattering Model (2007, background): “Additionally, the chaotic evolution of multiple planet systems naturally provides a large dispersion in the time until dynamical instability results in close encounters (Chambers, Wetherill & Boss 1996; FHR; Marzari & Weidenschilling 2002; Chatterjee et al. 2008).”
Toward a Deterministic Model of Planetary Formation. I. A Desert in the Mass and Semimajor Axis Distributions of Extrasolar Planets (2003, background): “In the current analysis, we do not consider the interaction between multiple planets which can lead to dynamical instabilities (Chambers et al. 1996; Lin & Ida 1997; Marzari & Weidenschilling 2002).”
Debris disks as signposts of terrestrial planet formation (2011, background): “A prediction of the planet-planet scattering model is that most planetary systems should contain multiple giant planets, i.e., additional giant planets should exist exterior to most of the known ones (e.g., Rasio & Ford 1996; Marzari & Weidenschilling 2002).”
Dynamics of the Giant Planets of the Solar System in the Gaseous Protoplanetary Disk and Their Relationship to the Current Orbital Architecture (2007, background): “Planet eccentricities are believed to be the result of mutual perturbations (Rasio and Ford, 1996; Marzari and Weidenschilling, 2002).”
Five New Multicomponent Planetary Systems (2005, background): “Interactions between pairs of planets may result in orbital resonances and pumping of orbital eccentricities (Nelson & Papaloizou 2002; Nauenberg 2002; Marzari & Weidenschilling 2002; Goździewski 2003).”
EVIDENCE OF POSSIBLE SPIN–ORBIT MISALIGNMENT ALONG THE LINE OF SIGHT IN TRANSITING EXOPLANET SYSTEMS (2010, background): “…between newly formed planets and planetesimals at several AU predict that nonnegligible misalignments ψ can occur (e.g. Ford et al. 2001; Yu & Tremaine 2001; Papaloizou & Terquem 2001; Terquem & Papaloizou 2002; Marzari & Weidenschilling 2002; Chatterjee et al. 2008; Jurić & Tremaine 2008).”
EXOPLANETARY SPIN–ORBIT ALIGNMENT: RESULTS FROM THE ENSEMBLE OF ROSSITER–MCLAUGHLIN OBSERVATIONS (2009, background): “…would produce at least occasionally large misalignments (Ford et al. 2001; Yu & Tremaine 2001; Papaloizou & Terquem 2001; Terquem & Papaloizou 2002; Marzari & Weidenschilling 2002; Thommes & Lissauer 2003; Wu et al. 2007; Fabrycky & Tremaine 2007; Chatterjee et al. 2008; Jurić & Tremaine 2008;…”