124 citations · 835 across the 29 of their papers we have counts for
29 papers
The fragility of the Uranian moons during the giant planet instability
Matthew S. Clement, Nathan A. Kaib, Andre Izidoro +1
It is thought that, sometime after their formation, the solar system's giant planets experienced a dynamical instability that caused their orbits to excite, diverge, and ejected on…
Elevated Eccentricities in the Radius Valley Hint at Water-Rich Mini-Neptunes
Sho Shibata, Andre Izidoro
While recent planet-formation models broadly reproduce the observed population of super-Earths and mini-Neptunes, as well as the bimodal radius distribution (the ``radius valley'')…
The Role of Magnetospheric Rebound in Breaking Resonant Chains of Super-Earths and Mini-Neptunes
Mengrui Pan, Andre Izidoro, Sho Shibata
Stellar magnetic fields are thought to truncate the inner regions of protoplanetary disks around T Tauri stars, creating a magnetospheric cavity near the star. As the disk evolves…
Very-wide-orbit planets from dynamical instabilities during the stellar birth cluster phase
André Izidoro, Sean N. Raymond, Nathan A. Kaib +2
Gas giant planets have been detected on eccentric orbits several hundreds of astronomical units in size around other stars. It has been proposed that even the Sun hosts a wide-orbi…
A tale of dynamical instabilities and giant impacts in the radius valley
Sho Shibata, Andre Izidoro
The size distribution of planets with radii between 1 and peaks near 1.4 and , with a dip around -- the so-called "radius valley." Recent s…
Size-Frequency Distribution of Terrestrial Leftover Planetesimals and S-complex Implanted Asteroids
Rogerio Deienno, Andre Izidoro, David Nesvorny +3
The isotopic composition of meteorites linked to S-complex asteroids has been used to suggest that these asteroids originated in the terrestrial planet's region, i.e., within 1.5 a…
Formation of super-Earths and mini-Neptunes from rings of planetesimals
Sho Shibata, Andre Izidoro
The solar system planetary architecture has been proposed to be consistent with the terrestrial and giant planets forming from material rings at ~1 au and ~5 au, respectively. Here…
Accretion of the earliest inner solar system planetesimals beyond the water-snowline
Damanveer S. Grewal, Nicole X. Nie, Bidong Zhang +2
How and where the first generation of inner solar system planetesimals formed remains poorly understood. Potential formation regions are the silicate condensation line and water-sn…
The link between Athor and EL meteorites does not constrain the timing of the giant planet instability
Andre Izidoro, Rogerio Deienno, Sean N. Raymond +1
The asteroid Athor, residing today in the inner main asteroid belt, has been recently associated as the source of EL enstatite meteorites to Earth. It has been argued that Athor fo…
Accretion and Uneven Depletion of the Main Asteroid Belt
Rogerio Deienno, David Nesvorny, Matthew S. Clement +3
The main asteroid belt (MAB) is known to be primarily composed of objects from two distinct taxonomic classes, generically defined here as S- and C-complex. The former probably ori…
Oort cloud (exo)planets
Sean N. Raymond, Andre Izidoro, Nathan A. Kaib
Dynamical instabilities among giant planets are thought to be nearly ubiquitous, and culminate in the ejection of one or more planets into interstellar space. Here we perform N-bod…
Survival and dynamics of rings of co-orbital planets under perturbations
Sean N. Raymond, Dimitri Veras, Matthew S. Clement +3
In co-orbital planetary systems, two or more planets share the same orbit around their star. Here we test the dynamical stability of co-orbital rings of planets perturbed by outsid…
Constellations of co-orbital planets: horseshoe dynamics, long-term stability, transit timing variations, and potential as SETI beacons
Sean N. Raymond, Dimitri Veras, Matthew S. Clement +3
Co-orbital systems contain two or more bodies sharing the same orbit around a planet or star. The best-known flavors of co-orbital systems are tadpoles (in which two bodies' angula…
Assessing the spin-orbit obliquity of low-mass planets in the breaking the chain formation model: A story of misalignment
Leandro Esteves, André Izidoro, Othon C. Winter +2
The spin-orbit obliquity of a planetary system constraints its formation history. A large obliquity may either indicate a primordial misalignment between the star and its gaseous d…
The Exoplanet Radius Valley from Gas-driven Planet Migration and Breaking of Resonant Chains
Andre Izidoro, Hilke E. Schlichting, Andrea Isella +3
The size frequency distribution of exoplanet radii between 1 and 4 is bimodal with peaks at 1.4 and 2.4 , and a valley at 1.8…
Implications of Jupiter Inward Gas-Driven Migration for the Inner Solar System
Rogerio Deienno, Andre Izidoro, Alessandro Morbidelli +2
The migration history of Jupiter in the sun's natal disk remains poorly constrained. Here we consider how Jupiter's migration affects small-body reservoirs and how this constrains…
Explaining Mercury via a single giant impact is highly unlikely
P. Franco, A. Izidoro, O. C. Winter +2
The classical scenario of terrestrial planet formation is characterized by a phase of giant impacts among Moon-to-Mars mass planetary embryos. While the classic model and its adapt…
Planetesimal rings as the cause of the Solar System's planetary architecture
Andre Izidoro, Rajdeep Dasgupta, Sean N. Raymond +3
Astronomical observations reveal that protoplanetary disks around young stars commonly have ring- and gap-like structures in their dust distributions. These features are associated…
The effect of a strong pressure bump in the Sun's natal disk: Terrestrial planet formation via planetesimal accretion rather than pebble accretion
André Izidoro, Bertram Bitsch, Rajdeep Dasgupta
Mass-independent isotopic anomalies of carbonaceous and non-carbonaceous meteorites show a clear dichotomy suggesting an efficient separation of the inner and outer solar system. O…
Building the Galilean moons system via pebble accretion and migration: A primordial resonant chain
Gustavo Madeira, André Izidoro, Silvia M. Giuliatti Winter
The origins of the Galilean satellites - namely Io, Europa, Ganymede, and Callisto - is not fully understood yet. Here we use N-body numerical simulations to study the formation of…
Could Uranus and Neptune form by collisions of planetary embryos?
Alice Chau, Christian Reinhardt, André Izidoro +2
The origin of Uranus and Neptune remains a challenge for planet formation models. A potential explanation is that the planets formed from a population of a few planetary embryos wi…
The origins of nearly coplanar, non-resonant systems of close-in super-Earths
Leandro Esteves, André Izidoro, Sean N. Raymond +1
Some systems of close-in "super-Earths" contain five or more planets on non-resonant but compact and nearly coplanar orbits. The Kepler-11 system is an iconic representative of thi…
Dynamical evidence for an early giant planet instability
Rafael Ribeiro de Sousa, Alessandro Morbidelli, Sean N. Raymond +3
The dynamical structure of the Solar System can be explained by a period of orbital instability experienced by the giant planets. While a late instability was originally proposed t…
The excitation of a primordial cold asteroid belt as an outcome of the planetary instability
Rogerio Deienno, Andre Izidoro, Alessandro Morbidelli +3
The main asteroid belt (MB) is low in mass but dynamically excited. Here we propose a new mechanism to excite the MB during the giant planet ('Nice model') instability, which is ex…