Measuring the Orbital Parameters of Radial Velocity Systems in Mean-motion Resonance: A Case Study of HD 200964

Rosenthal, M. M.; Jacobson-Galán, W. V.; Nelson, Brent D.; Murray-Clay, Ruth; Burt, Jennifer; Holden, B. P.; Chang, Eonho; Kaaz, Nicholas; Yant, Jackson; Butler, R. Paul; Vogt, Steven S.

doi:10.3847/1538-3881/ab3b02

Cited by 6 publications

(6 citation statements)

References 55 publications

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“…We made use of the code RVStab (Rosenthal et al 2019) as the backbone of our analysis to dynamically fit the RV data by integrating the entire system with the inclusion of planet-planet interaction using an N-body integrator REBOUND (Rein & Liu 2012), and to carry out a posterior parameter search with MCMC exploration. We used IAS15 (Rein & Spiegel 2015), a nonsymplectic integrator with adaptive time stepping, and chose the coordinate system to be with reference to the central star.…”

Section: Dynamical Modelmentioning

confidence: 99%

“…To account for the potential presence of planet-planet interaction between the b and c planet, a full dynamical model is needed to integrate the planets along their orbits and obtain the induced motion on the host star at each step. We made use of the code RVStab (Rosenthal et al 2019) as the backbone of our analysis to dynamically fit the RV data by integrating the entire system with the inclusion of planet-planet interaction using an Nbody integrator REBOUND (Rein & Liu 2012), and to carry out posterior parameter search with MCMC exploration. We used IAS15 (Rein & Spiegel 2015), a nonsymplectic integrator with adaptive time stepping, and chose the coordinate system to be with reference to the central star.…”

Section: Dynamical Modelmentioning

confidence: 99%

“…Therefore, the giant planets within an MMR chain at locations within the snow line are likely to have initially formed beyond the snow line, then gradually migrated inwards through convergent migration while being embedded within the protoplanetary disk. Such interacting planets undergoing migration thus provide important constraints on planetary formation, planet migration history, system evolution, and architecture (Correia et al 2009;Rosenthal et al 2019). Additionally, the presence of giant planets within the system could greatly influence the habitability of terrestrial planets (Georgakarakos et al 2018;Sánchez et al 2018;Kane & Blunt 2019;Kane et al 2020;Bailey & Fabrycky 2022).…”

Section: Introductionmentioning

confidence: 99%

“…Software: GLS (Zechmeister & Kürster 2009), RadVel (Fulton et al 2018), REBOUND (Rein & Liu 2012), RVSearch (Rosenthal et al 2021) , RVStab (Rosenthal et al 2019)…”

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New Dynamical State and Habitability of the HD 45364 Planetary System

Kane

Dalba

et al. 2022

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Planetary systems with multiple giant planets provide important opportunities to study planetary formation and evolution. The HD 45364 system hosts two giant planets that reside within the habitable zone (HZ) of their host star and was the first system discovered with a 3:2 mean motion resonance (MMR). Several competing migration theories with different predictions have previously provided explanations regarding the observed resonance through dynamical simulations that utilized limited data. Here, over ten years since the original discovery, we revisit the system with a substantially increased radial velocity (RV) sample from High Accuracy Radial Velocity Planet Searcher spectrograph and High Resolution Echelle Spectrometer that significantly extends the observational baseline. We present the revised orbital solutions for the two planets using both Keplerian and dynamical models. Our RV models suggest orbits that are more circular and separated than those previously reported. As a result, the predicted strong planet–planet interactions were not detected. The system dynamics were reanalyzed, and the planet pair was found to exhibit apsidal behavior of both libration and circulation, indicating a quasi-resonance state rather than being truly in MMR. The new orbital solution and dynamical state of the system confirm migration models that predicted near-circular orbits as the preferred scenario. We also study the habitability prospects of this system and found that an additional Earth-mass planet and exomoons in the HZ are possible. This work showcases the importance of continued RV observations and its impact on our knowledge of the system’s dynamical history. HD 45364 continues to be an interesting target for both planetary formation and habitability studies.

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Section: Dynamical Modelmentioning

confidence: 99%

Section: Dynamical Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

“…Software: GLS (Zechmeister & Kürster 2009), RadVel (Fulton et al 2018), REBOUND (Rein & Liu 2012), RVSearch (Rosenthal et al 2021) , RVStab (Rosenthal et al 2019)…”

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New Dynamical State and Habitability of the HD 45364 Planetary System

Kane

Dalba

et al. 2022

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“…Moreover, in our solar system Saturn-Uranus and Uranus-Neptune systems are in 3:1 and 2:1 near MMRs respectively. There are several scientists who have studied the orbital evolution of resonant planetary systems (Crida et al, 2008;Petrovich et al, 2013;Barnes et al, 2015;Mia and Kushvah, 2016a;Rosenthal et al, 2019).…”

Section: Introductionmentioning

confidence: 99%

Analysis of the dynamics of the resonant planetary system HD 45364

Mia

Paul

2022

Preprint

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The aim of this work is to analyse the orbital dynamics and stability of exoplanetary system in which two planets are in nearly 3:2 MMR. We have taken HD 45364 system for our study in which two planets are most likely in a 3:2 MMR. We have plotted two resonant angles and the relative apsidal longitudes and it is observed that they are librating around a constant value. From this observation our opinion is that there exist nearly 3:2 MMR between HD 45364b and HD 45364c. The perturbative solution is obtained for the time variation of the semi-major axes. The short and long term variations of semimajor axes are studied. For the validation of our analytical results we have compared our analytical solutions with the numerical solutions. The effect of planetary perturbations on eccentricity is studied with the help of secular resonance dynamics theory. The short and long term variations of eccentricities of HD 45364b and HD 45364c are shown graphically. Moreover, using the latest stability criteria, we have studied the dynamical stability of HD 45364 system.

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Stability constrained characterization of multiplanet systems

Tamayo

Gilbertson

Foreman-Mackey

2020

Monthly Notices of the Royal Astronomical Society

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Many discovered multiplanet systems are tightly packed. This implies that wide parameter ranges in masses and orbital elements can be dynamically unstable and ruled out. We present a case study of Kepler-23, a compact three-planet system where constraints from stability, transit timing variations (TTVs), and transit durations can be directly compared. We find that in this tightly packed system, stability can place upper limits on the masses and orbital eccentricities of the bodies that are comparable to or tighter than current state of the art methods. Specifically, stability places 68 per cent upper limits on the orbital eccentricities of 0.09, 0.04, and 0.05 for planets b, c, and d, respectively. These constraints correspond to radial velocity signals ≲ 20 cm s−1, are significantly tighter to those from transit durations, and comparable to those from TTVs. Stability also yields 68 per cent upper limits on the masses of planets b, c, and d of 2.2, 16.1, and 5.8 M⊕, respectively, which were competitive with TTV constraints for the inner and outer planets. Performing this stability constrained characterization is computationally expensive with N-body integrations. We show that SPOCK, the Stability of Planetary Orbital Configurations Klassifier, is able to faithfully approximate the N-body results over 4000 times faster. We argue that such stability constrained characterization of compact systems is a challenging ‘needle-in-a-haystack’ problem (requiring removal of 2500 unstable configurations for every stable one for our adopted priors) and we offer several practical recommendations for such stability analyses.

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Measuring the Orbital Parameters of Radial Velocity Systems in Mean-motion Resonance: A Case Study of HD 200964

Cited by 6 publications

References 55 publications

New Dynamical State and Habitability of the HD 45364 Planetary System

New Dynamical State and Habitability of the HD 45364 Planetary System

Analysis of the dynamics of the resonant planetary system HD 45364

Stability constrained characterization of multiplanet systems

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