Tootfinder

Dynamical and Secular Stability of Mutually Inclined Planetary Systems
Hareesh Gautham Bhaskar, Hagai Perets
https://arxiv.org/abs/2404.07264 https://

Dynamical and Secular Stability of Mutually Inclined Planetary Systems
Multiple analytical and empirical stability criteria have been derived in the literature for two planet systems. But, the dependence of the stability limit on the initial mutual inclination between the inner and outer orbits is not well modeled by previous stability criteria. Here, we derive a semi-analytical stability criteria for two planet systems, at arbitrary inclinations, in which the inner planet is a test particle. Using perturbation theory we calculate the characteristic fractional cha…

Coupling nanoscopic tomography and micromagnetic modelling to assess the stability of geomagnetic recorders
Ualisson Donardelli Bellon, Wyn Williams, Ricardo Ivan Ferreira Trindade, Ana Diaz, Douglas Galante
https://arxiv.org/abs/2404.07769

Coupling nanoscopic tomography and micromagnetic modelling to assess the stability of geomagnetic recorders
The recording of planetary magnetic fields is often attributed to uniformly-magnetised nanoscopic iron oxides, called single-domain (SD). Yet, the main magnetic constituents of rocks are more complex, non-uniformly magnetised grains in single or multi-vortex states. We know little about their behaviour due to limitations in defining their precise shape and internal magnetic structure. We propose a novel approach combining non-destructive synchrotron-based ptychographic nanotomography with micro…

Differences between Stable and Unstable Architectures of Compact Planetary Systems
Kathryn Volk, Renu Malhotra
https://arxiv.org/abs/2404.06567 https://

Differences between Stable and Unstable Architectures of Compact Planetary Systems
We present a stability analysis of a large set of simulated planetary systems of three or more planets based on architectures of multiplanet systems discovered by \textit{Kepler} and \textit{K2}. We propagated 21,400 simulated planetary systems up to 5 billion orbits of the innermost planet; approximately 13% of these simulations ended in a planet-planet collision within that timespan. We examined trends in dynamical stability based on dynamical spacings, orbital period ratios, and mass ratios …

Full orbital solutions in pre-main sequence high-order multiple systems: GG Tau Ab and UX Tau B
Gaspard Duch\^ene, Jean-Baptiste LeBouquin, Fran\c{c}ois M\'enard, Nicol\'as Cuello, Claudia Toci, Maud Langlois
https://arxiv.org/abs/2404.02469

Full orbital solutions in pre-main sequence high-order multiple systems: GG Tau Ab and UX Tau B
High-order multiple (triple and beyond) systems are relatively common. Their interaction with circumstellar and circumbinary material can have a large impact on the formation and evolution of planetary systems and depends on their orbital properties. GG\,Tau and UX\,Tau are two pre-main sequence high-order multiple systems in which the tightest pair has a projected separation of $\approx5$--20\,au. Characterizing precisely their orbits is crucial to establish their long-term stability, to predi…

Empirical stability criteria for 3D hierarchical triple systems I: Circumbinary planets
Nikolaos Georgakarakos, Siegfried Eggl, Mohamad Ali-Dip, Ian Dobbs-Dixon
https://arxiv.org/abs/2404.13746

Empirical stability criteria for 3D hierarchical triple systems I: Circumbinary planets
In this work we revisit the problem of the dynamical stability of hierarchical triple systems with applications to circumbinary planetary orbits. We carry out more than 3 10^8 numerical simulations of planets between the size of Mercury and the lower fusion boundary (13 Jupiter masses) which revolve around the center of mass of a stellar binary over long timescales. For the first time, three dimensional and eccentric planetary orbits are considered. We explore systems with a variety of binary a…

Trojan Exoplanets
Philippe RobutelIMCCE, Adrien Leleu
https://arxiv.org/abs/2402.15168 https://arxiv.org/pdf/2402.15168

Trojan Exoplanets
Co-orbital exoplanets are a by-product of the models of formation of planetary systems. However, none have been detected in nature thus far. Although challenging, the observation of co-orbital exoplanets would provide valuable information on the formation of planetary systems as well as on the interactions between planets and their host star. After a brief review of the stability and formation issues of co-orbital systems, some observational methods dedicated to their detection are presented.