Naor Movshovitz

TL;DR: In this paper, a selection of interior models based on ab initio computer simulations of hydrogen-helium mixtures is presented. But, the model predictions are strongly affected by the chosen equation of state, the prediction of an enrichment of Z in the deep, metallic envelope over that in the shallow, molecular envelope holds.

TL;DR: In this article, Hubickyj et al. presented numerical simulations for the formation of Jupiter at 5.2 AU in three primordial disks with three different assumed values of the surface density of solid particles.

TL;DR: In this paper, the authors explore the idea that most chondrules formed as a consequence of inefficient pairwise accretion, when molten or partly molten planetesimals ~ 30-100 km diameter, similar in size, collided at velocities comparable to their two-body escape velocity ~ 100 m/s.

TL;DR: In this article, the size distribution of silicate grains in the outer radiative region of the envelope of a protoplanet evolving according to the scenario of Pollack et al. was computed.

TL;DR: In this paper, the authors construct a family of Saturn interior models constrained by the gravity field and compute their adiabatic mode eigenfrequencies and corresponding Lindblad and vertical resonances in Saturn's C ring, where more than twenty waves with pattern speeds faster than the ring mean motion have been detected and characterized using high resolution Cassini Visual and Infrared Mapping Spectrometer (VIMS) stellar occultation data.