We investigate the properties of hydrodynamic flow around eccentric protoplanets and compare them with often assumed case a circular orbit. To this end, we perform set 3D simulations small eccentricities ($e\leq 0.1$). adopt an isothermal equation state concentrate resolution on protoplanet to flows down scale protoplanet's circumplanetary disk (CPD). find enhanced prograde rotation exterior CP...

Curves in a family derived from powers of the polar coordinate formula for ellipses are found to provide good fits to bound orbits in a range of power-law potentials. This range includes the well-known 1/r (Keplerian) and logarithmic potentials. These approximate orbits, called p-ellipses, retain some of the basic geometric properties of ellipses. They satisfy and generalize Newton’s apsidal pr...

Abstract The climate of a terrestrial exoplanet is controlled by the type host star, orbital configuration and characteristics atmosphere surface. Many rocky exoplanets have higher eccentricities than those in Solar System, about 18% planets with masses <10 M⊕ e > 0.1. Underexplored are implications such high on atmosphere, climate, potential habitability planets. We use WACCM6, s...

An episode of dynamical instability is thought to have sculpted the orbital structure outer solar system. When modeling this instability, a key constraint comes from Jupiter's fifth eccentric mode (quantified by its amplitude M55), which an important driver system's secular evolution. Starting commonly-assumed near-circular orbits, present-day giant planets' architecture lies at limit numerical...