2016
DOI: 10.3847/0004-637x/820/1/55
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Difficulty in the Formation of Counter-Orbiting Hot Jupiters From Near-Coplanar Hierarchical Triple Systems: A Sub-Stellar Perturber

Abstract: Among a hundred transiting planets with a measured projected spin-orbit angle λ, several systems are suggested to be counter-orbiting. While they may be due to the projection effect, the mechanism to produce a counter-orbiting planet is not established. A promising scenario for the counter-orbiting planets is the extreme eccentricity evolution in near-coplanar hierarchical triple systems with eccentric inner and outer orbits. We examine this scenario in detail by performing a series of systematic numerical sim… Show more

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Cited by 30 publications
(24 citation statements)
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“…(ii) secular Lidov-Kozai (LK) oscillations (Lidov 1962;Kozai 1962) induced by a distant companion star or an additional (massive) planet on an inclined orbit (Wu & Murray 2003;Fabrycky & Tremaine 2007;Naoz et al 2012;Petrovich 2015a;Anderson et al 2016;Petrovich & Tremaine 2016); (iii) secular excitation induced by a close and coplanar, but eccentric planetary companion (Petrovich 2015b;Xue & Suto 2016), and (iv) secular chaos in multiplanet systems with at least three planets in mildly inclined and eccentric orbits Hamers et al 2016a). …”
Section: Introductionmentioning
confidence: 99%
“…(ii) secular Lidov-Kozai (LK) oscillations (Lidov 1962;Kozai 1962) induced by a distant companion star or an additional (massive) planet on an inclined orbit (Wu & Murray 2003;Fabrycky & Tremaine 2007;Naoz et al 2012;Petrovich 2015a;Anderson et al 2016;Petrovich & Tremaine 2016); (iii) secular excitation induced by a close and coplanar, but eccentric planetary companion (Petrovich 2015b;Xue & Suto 2016), and (iv) secular chaos in multiplanet systems with at least three planets in mildly inclined and eccentric orbits Hamers et al 2016a). …”
Section: Introductionmentioning
confidence: 99%
“…We solve the equations of motion described by Correia et al (2011) and Liu et al (2015); see also Appendix A of Xue & Suto (2016). Our simulation models are basically specified by seven parameters, m 2 , a 2,i , e 2,i , i 12,i , t v,p , f , and m 0 .…”
Section: Simulation Parameters and Fiducial Resultsmentioning
confidence: 99%
“…In this section, we perform a series of numerical simulations to study the orbital evolution of hierarchical triple systems in CHEM with a giant gas inner planet and a planetary outer perturber, similarly as our previous paper with a sub-stellar outer perturber (Xue & Suto 2016). We first present the model parameters and our fiducial case in subsection 3.1, and then consider how to interpret the numerical results in terms of the analytical argument in subsection 3.2.…”
Section: Giant Gas Inner Planet With a Planetary Outer Perturbermentioning
confidence: 99%
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