Comets have three known reservoirs: the roughly spherical Oort Cloud (for long-period
comets), the flattened Kuiper Belt (for ecliptic comets), and, surprisingly, the asteroid belt (for …

Objects in the Kuiper belt are difficult to study in detail, even with the best telescopes
available. Therefore, for many years, studies of the compositions of these objects were …

How big were the first planetesimals? We attempt to answer this question by conducting
coagulation simulations in which the planetesimals grow by mutual collisions and form …

Collisions are the core agent of planet formation. In this work, we derive an analytic
description of the dynamical outcome for any collision between gravity-dominated bodies …

We present a model of near-Earth asteroid (NEA) rotational fission and ensuing dynamics
that describes the creation of synchronous binaries and all other observed NEA systems …

ABSTRACT A large fraction of∼ 100 km class low-inclination objects in the classical Kuiper
Belt (KB) are binaries with comparable masses and a wide separation of components. A …

The disaster area is a constantly changing environment, which can make it challenging to
distribute supplies effectively. The lack of accurate information about the required goods and …

Radial velocity and transit surveys indicate that solar-type stars bear super-Earths, with
masses up to∼ 20 M⊕ and periods up to a few months, that are more common than those …

Debris disks are optically thin, almost gas-free dusty disks observed around a significant
fraction of main-sequence stars older than about 10 Myr. Since the circumstellar dust is short …

Numerical simulations of the stochastic end stage of planet formation typically begin with a
population of embryos and planetesimals that grow into planets by merging. We analyzed …