Explaining why the uranian satellites have equatorial prograde orbits despite the large planetary obliquity

  title={Explaining why the uranian satellites have equatorial prograde orbits despite the large planetary obliquity},
  author={Alessandro Morbidelli and Kleomenis Tsiganis and Konstantin Batygin and Aur{\'e}lien Crida and Rodney Gomes},

Figures from this paper

Primordial Giant Planet Obliquity Driven by a Circumplanetary Disk
Detached circumplanetary disks are unstable to tilting as a result of the stellar tidal potential. We examine how a tilted circumplanetary disk affects the evolution of the spin axis of an oblate
Coaccretion + Giant-impact Origin of the Uranus System: Tilting Impact
The origin of the Uranian satellite system remains uncertain. The four major satellites have nearly circular, coplanar orbits, and the ratio of the satellite system to planetary mass resembles
Uranian satellite formation by evolution of a water vapour disk generated by a giant impact
The ice-giant planet Uranus probably underwent a giant impact, given that its spin axis is tilted by 98 degrees 1 – 3 . That its satellite system is equally inclined and prograde suggests that it was
Co-accretion + impact origin of the Uranian satellites?
We consider the origin of the Uranian satellites in a scenario proposed by Morbidelli et al. [6], in which an initial satellite system produced by co-accretion is disrupted by mutual collisions as a
Could Uranus and Neptune form by collisions of planetary embryos?
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 with masses of a few
Accretion of Uranus and Neptune from inward-migrating planetary embryos blocked by Jupiter and Saturn
Reproducing Uranus and Neptune remains a challenge for simulations of solar system formation. The ice giants' peculiar obliquities suggest that they both suffered giant collisions during their
Tilting Ice Giants with a Spin–Orbit Resonance
Giant collisions can account for Uranus’s and Neptune’s large obliquities, yet generating two planets with widely different tilts and strikingly similar spin rates is a low-probability event.
The Origin of Neptune’s Unusual Satellites from a Planetary Encounter
The Neptunian satellite system is unusual, comprising Triton, a large (∼2700 km) moon on a close-in, circular, yet retrograde orbit, flanked by Nereid, the largest irregular satellite (∼300 km) on a
Tilting Uranus: Collisions versus Spin–Orbit Resonance
In this paper, we investigate whether Uranus’s 98° obliquity was a by-product of a secular spin–orbit resonance assuming that the planet originated closer to the Sun. In this position, Uranus’s spin
Formation of Regular Satellites from Ancient Massive Rings in the Solar System
It is shown that most regular satellites in the solar system probably formed in this way, and predicts that Uranus and Neptune once had massive, Saturn-like rings, which gave birth to moons and then disappeared.


The origin of the high inclination of Uranus’ spin-axis (Uranus’ obliquity) is one of the great unanswered questions about the solar system. Giant planets are believed to form with nearly zero
Constraints to Uranus' Great Collision. IV. The Origin of Prospero
Context. It is widely accepted that the large obliquity of Uranus is the result of a great tangential collision (GC) with an Earth size proto-planet at the end of the accretion process. The impulse
The recent formation of Saturn's moonlets from viscous spreading of the main rings
A hybrid simulation is reported in which the viscous spreading of Saturn’s rings beyond the Roche limit (the distance beyond which the rings are gravitationally unstable) gives rise to the small moons.
Formation of the Galilean Satellites: Conditions of Accretion
We examine formation conditions for the Galilean satellites in the context of models of late-stage giant planet accretion and satellite-disk interactions. We first reevaluate the current standard, in
Giant impacts on a primitive Uranus
The Secular Evolution of the Primordial Kuiper Belt
A model that rapidly computes the secular evolution of a gravitating disk-planet system is developed. The disk is treated as a nested set of gravitating rings, with the rings'/planets' time evolution
Solar system dynamics
The Solar System is a complex and fascinating dynamical system. This is the first textbook to describe comprehensively the dynamical features of the Solar System and to provide students with all the
A Multiple Time Step Symplectic Algorithm for Integrating Close Encounters
We present a new symplectic algorithm that has the desirable properties of the sophisticated but highly efficient numerical algorithms known as mixed variable symplectic (MVS) methods and that, in