Secular evolution of close-in planets: the effects of general relativity

Marzari, F.; Nagasawa, Makiko

doi:10.1093/mnras/staa271

Cited by 5 publications

(6 citation statements)

References 30 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…From the study of such systems, our results indicated that the efficiency of formation of HJ candidates from high-eccentricity mechanisms is about 3.3% (2.9%) in numerical experiments without (with) GR effects. The slightly smaller number of HJ candidates in simulations with GR is consistent with studies developed by Marzari & Nagasawa (2020), who showed the GR can significantly reduce the oscillations of eccentricity of close-in planets in their secular evolution. We remark that the percentages of HJ candidates produced in the present investigation are also in a good agreement with previous works that focused on different high-eccentricity mechanisms (see Beaugé & Nesvorný 2012;Petrovich 2015b;Muñoz et al 2016;Petrovich & Tremaine 2016;Wang et al 2017;Teyssandier et al 2019).…”

Section: Discussionsupporting

confidence: 89%

“…In other words, the efficiencies of production of HJ candidates were 3.32% and 2.89% with respect to the total number of systems with dynamic instability events in No-GR and GR simulations, respectively. This reduction in the number of HJ candidates in the GR scenario may be explained by the fact that GR contributes to reducing the periods and amplitudes of the eccentricity oscillations of the planets in secular evolution as Marzari & Nagasawa (2020) recently showed.…”

Section: Efficiencies Of High-eccentricity Mechanisms In the Producti...mentioning

confidence: 79%

See 1 more Smart Citation

Production of hot Jupiter candidates from high-eccentricity mechanisms for different initial planetary mass configurations

Garzón

Rodríguez

Elía

2022

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Hot Jupiters (HJs) are giant planets with orbital periods of the order of a few days with semimajor axis within ∼0.1 au. Several theories have been invoked in order to explain the origin of this type of planets, one of them being the high-eccentricity migration. This migration can occur through different high-eccentricity mechanisms. Our investigation focused on six different kinds of high-eccentricity mechanisms, namely, direct dispersion, coplanar, Kozai-Lidov, secular chaos, E1 and E2 mechanisms. We investigated the effciency of these mechanisms for the production of HJ candidates in multi-planet systems initially tightly-packed in the semimajor axis, considering a large set of numerical simulations of the exact equations of motion in the context of the N-body problem. In particular, we analyzed the sensitivity of our results to the initial number of planets, the initial semimajor axis of the innermost planetary orbit, the initial conffguration of planetary masses, and to the inclusion of general relativity effects. We found that the E1 mechanism is the most effcient in producing HJ candidates both in simulations with and without the contribution of general relativity, followed by the Kozai-Lidov and E2 mechanisms. Our results also revealed that, except for the initial equal planetary mass conffguration, the E1 mechanism was notably effcient in the other initial planetary mass conffgurations considered in this work. Finally, we investigated the production of HJ candidates with prograde, retrograde, and alternating orbits. According to our statistical analysis, the Kozai-Lidov mechanism has the highest probability of significantly exciting the orbital inclinations of the HJ candidates.

show abstract

Section: Discussionsupporting

confidence: 89%

Section: Efficiencies Of High-eccentricity Mechanisms In the Producti...mentioning

confidence: 79%

Production of hot Jupiter candidates from high-eccentricity mechanisms for different initial planetary mass configurations

Garzón

Rodríguez

Elía

2022

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Moreover, we see that the eccentricity excitation of the inner planet is reduced with the GR contribution (see e.g. Migaszewski & Goździewski 2009;Sansottera et al 2014;Marzari & Nagasawa 2020). For i mut = 50 • (bottom panels), we note an additional consequence: the libration of the angle ω 1 (bottom left) vanishes when considering relativistic corrections (bottom right).…”

Section: Influence Of Gr On the Extent Of The Lk Regionmentioning

confidence: 87%

“…By using the same approximation but limited to the octupole level, Naoz et al (2013) discussed how GR can suppress or excite the eccentricities in triple-star systems. More recently, employing linear secular theory, Marzari & Nagasawa (2020) showed that, for coplanar two-planet systems with a close-in planet, a significant damping of the eccentricities of the inner and outer planets occurs when GR is included, which implies that systems with a chaotic behaviour caused by mutual interactions between the planets could actually have a stable evolution thanks to GR effects.…”

Section: Introductionmentioning

confidence: 99%

The effects of general relativity on close-in radial-velocity-detected exosystems

Volpi,

Libert

2024

A&A

View full text Add to dashboard Cite

The detection of the first exoplanet around a solar-type star revealed the existence of close-in planets. Several of these close-in planets are part of multi-planet systems. For systems detected via the radial velocity (RV) method, we lack information on the mutual inclination of the orbital planes. The aim of this work is to study the long-term stability of RV-detected two-planet systems with close-in planets and identify possible three-dimensional configurations for these systems that are compatible with observations. To do so, we focused on the protective mechanism of the Lidov-Kozai (LK) secular resonance and studied the effects of general relativity (GR) on long-term evolution. By means of an analytical study based on a high-order secular Hamiltonian expansion in the eccentricities and inclinations, we first identified ranges of values for the orbital and mutual inclinations that are compatible with the presence of the LK resonance in the purely gravitational case. Then, adding the secular contribution of the relativistic corrections exerted by the central star on the inner planet, namely the advance of its pericenter precession, we analysed the outcomes of the two sets of simulations. We compared our results to analytical estimates to determine the importance of GR effects. We find that for the majority of the systems considered, GR strongly affects the dynamics of the system and, most of the time, voids the LK resonance, as observed for GJ $649$, GJ $832$, HD $187123$, HD $190360$, HD $217107$, and HD $47186$. The long-term stability of these systems is then possible whatever the mutual inclination of the orbits. On the contrary, for GJ $682$, HD $11964$, HD $147018$, and HD $9446$, the LK resonant region in the parameter space of the orbital and mutual inclinations is left (almost) unchanged when GR effects are considered, and consequently their long-term stability is only possible if the mutual inclination of the orbits is low or if the systems are in the LK regime with a high mutual inclination.

show abstract

“…Precession due to General Relativity (GR) can become a significant effect for planets orbiting close to their host stars, and in particular can influence the secular interactions within planetary systems, as shown for example in the recent study by Marzari & Nagasawa (2020). As discussed in section 4.3.1, the dominant effect that perturbs the inner systems in our study is the mutual scattering of outer giants, such that during pericentre passage they enter the inner system and cause strong scattering of the planets there.…”

Section: Relativistic Precessionmentioning

confidence: 99%

On the origin of the eccentricity dichotomy displayed by compact super-Earths: dynamical heating by cold giants

Poon,

Nelson

2020

Preprint

View full text Add to dashboard Cite

Approximately half of the planets discovered by NASA's Kepler mission are in systems where just a single planet transits its host star, and the remaining planets are observed to be in multi-planet systems. Recent analyses have reported a dichotomy in the eccentricity distribution displayed by systems where a single planet transits compared with that displayed by the multi-planet systems. Using N-body simulations, we examine the hypothesis that this dichotomy has arisen because inner systems of super-Earths are frequently accompanied by outer systems of giant planets that can become dynamically unstable and perturb the inner systems. Our initial conditions are constructed using a subset of the known Kepler five-planet systems as templates for the inner systems, and systems of outer giant planets with masses between those of Neptune and Saturn that are centred on orbital radii 2 ≤ a p ≤ 10 au. The parameters of the outer systems are chosen so that they are always below an assumed radial velocity detection threshold of 3 m s −1 . The results show an inverse relation between the mean eccentricities and the multiplicites of the systems. Performing synthetic transit observation of the final systems reveals dichotomies in both the eccentricity and multiplicity distributions that are close to being in agreement with the Kepler data. Hence, understanding the observed orbital and physical properties of the compact systems of super-Earths discovered by Kepler may require holistic modelling that couples the dynamics of both inner and outer systems of planets during and after the epoch of formation.

show abstract

Secular evolution of close-in planets: the effects of general relativity

Cited by 5 publications

References 30 publications

Production of hot Jupiter candidates from high-eccentricity mechanisms for different initial planetary mass configurations

Production of hot Jupiter candidates from high-eccentricity mechanisms for different initial planetary mass configurations

The effects of general relativity on close-in radial-velocity-detected exosystems

On the origin of the eccentricity dichotomy displayed by compact super-Earths: dynamical heating by cold giants

Contact Info

Product

Resources

About