TY - JOUR A1 - Krüger, Harald A1 - Krivov, Alexander V. A1 - Grün, Eberhard T1 - A dust cloud around Ganymede Maintained by hypervelocity impacts of interplanetary micrometeoroids Y1 - 2000 SN - 0032-0633 ER - TY - JOUR A1 - Thiessenhusen, Kai-Uwe A1 - Krivov, Alexander V. A1 - Krüger, Harald A1 - Grün, Eberhard T1 - A dust cloud around Pluto and Charon Y1 - 2002 SN - 0032-0633 ER - TY - JOUR A1 - Krivov, Alexander V. A1 - Krüger, Harald A1 - Grün, Eberhard A1 - Thiessenhusen, Kai-Uwe A1 - Hamilton, Douglas P. T1 - A tenuous dust ring of Jupiter formed by escaping ejecta from the Galilean satellites Y1 - 2002 SN - 0148-0227 ER - TY - JOUR A1 - Spahn, Frank A1 - Schmidt, Jürgen A1 - Albers, Nicole A1 - Hörning, Marcel A1 - Makuch, Martin A1 - Seiß, Martin A1 - Kempf, Sascha A1 - Srama, Ralf A1 - Dikarev, Valeri A1 - Helfert, Stefan A1 - Moragas-Klostermeyer, Georg A1 - Krivov, Alexander V. A1 - Sremcevic, Miodrag A1 - Tuzzolino, Anthony J. A1 - Economou, Thanasis A1 - Grün, Eberhard T1 - Cassini dust measurements at Enceladus and implications for the origin of the E ring Y1 - 2006 UR - http://www.sciencemag.org/content/311/5766/1416.full U6 - https://doi.org/10.1126/science.1121375 ER - TY - JOUR A1 - Grün, Eberhard A1 - Krivov, Alexander V. T1 - Dust astronomy : new venues in interplanetary and interstellar dust research Y1 - 2002 SN - 1-58381-113-3 ER - TY - JOUR A1 - Mann, Ingrid A1 - Krivov, Alexander V. A1 - Kimura, Hiroshi T1 - Dust cloud near the sun Y1 - 2000 ER - TY - JOUR A1 - Krivov, Alexander V. A1 - Banaszkiewicz, Marek T1 - Dust Influx to Titan from Hyperion Y1 - 2001 SN - 0-7923-6946-7 ER - TY - JOUR A1 - Krivov, Alexander V. A1 - Sremcevic, Miodrag A1 - Spahn, Frank T1 - Evolution of a Keplerian disk of colliding and fragmenting particles: a kinetic model with application to the Edgeworth-Kuiper belt N2 - We present a kinetic model of a disk of solid particles, orbiting a primary and experiencing inelastic collisions. In distinction to other collisional models that use a 2D (mass-sernimajor axis) binning and perform a separate analysis of the velocity (eccentricity, inclination) evolution, we choose mass and orbital elements as independent variables of a phase space. The distribution function in this space contains full information on the combined mass, spatial, and velocity distributions of particles. A general kinetic equation for the distribution function is derived, valid for any set of orbital elements and for any collisional outcome, specified by a single kernel function. The first implementation of the model utilizes a 3D phase space (mass-semimajor axis-eccentricity) and involves averages over the inclination and all angular elements. We assume collisions to be destructive, simulate them with available material- and size-dependent scaling laws, and include collisional damping. A closed set of kinetic equations for a mass-semimajor axis-eccentricity distribution is written and transformation rules to usual mass and spatial distributions of the disk material are obtained. The kinetic "core" of our approach is generic. It is possible to add inclination as an additional phase space variable, to include cratering collisions and agglomeration, dynamical friction and viscous stirring, gravity of large perturbers, drag forces, and other effects into the model. As a specific application, we address the collisional evolution of the classical population in the Edgeworth-Kuiper belt (EKB). We run the model for different initial disk's masses and radial profiles and different impact strengths of objects. Our results for the size distribution, collisional timescales, and mass loss are in agreement with previous studies. In particular, collisional evolution is found to be most substantial in the inner part of the EKB, where the separation size between the survivors over EKB ' s age and fragments of earlier collisions lies between a few and several tens of km. The size distribution in the EKB is not a single Dohnanyi-type power law, reflecting the size dependence of the critical specific energy in both strength and gravity regimes. The net mass loss rate of an evolved disk is nearly constant and is dominated by disruption of larger objects. Finally, assuming an initially uniform distribution of orbital eccentricities, we show that an evolved disk contains more objects in orbits with intermediate eccentricities than in nearly circular or more eccentric orbits. This property holds for objects of any size and is explained in terms of collisional probabilities. The effect should modulate the eccentricity distribution shaped by dynamical mechanisms, such as resonances and truncation of perihelia by Neptune. (c) 2004 Elsevier Inc. All rights reserved Y1 - 2005 SN - 0019-1035 ER - TY - JOUR A1 - Sremcevic, Miodrag A1 - Krivov, Alexander V. A1 - Krüger, Harald A1 - Spahn, Frank T1 - Impact-generated dust clouds around planetary satellites : model versus Galileo N2 - This paper focuses on tenuous dust clouds of Jupiter's Galilean moons Europa, Ganymede and Callisto. In a companion paper (Sremcevic et al., Planet. Space Sci. 51 (2003) 455-471) an analytical model of impact-generated ejecta dust clouds surrounding planetary satellites has been developed. The main aim of the model is to predict the asymmetries in the dust clouds which may arise from the orbital motion of the parent body through a field of impactors. The Galileo dust detector data from flybys at Europa, Ganymede and Callisto are compatible with the model, assuming projectiles to be interplanetary micrometeoroids. The analysis of the data suggests that two interplanetary impactor populations are most likely the source of the measured dust clouds: impactors with isotropically distributed velocities and micrometeoroids in retrograde orbits. Other impactor populations, namely those originating in the Jovian system, or interplanetary projectiles with low orbital eccentricities and inclinations, or interstellar stream particles, can be ruled out by the statistical analysis of the data. The data analysis also suggests that the mean ejecta velocity angle to the normal at the satellite surface is around 30°, which is in agreement with laboratory studies of the hypervelocity impacts. © 2004 Elsevier Ltd. All rights reserved Y1 - 2005 SN - 0032-0633 ER - TY - JOUR A1 - Makuch, Martin A1 - Krivov, Alexander V. A1 - Spahn, Frank T1 - Long-term dynamical evolution of dusty ejecta from Deimos N2 - We re-assess expected properties of the presumed dust belt of Mars formed by impact ejecta from Deimos. Previous studies have shown that dynamics of Deimos particles are dominated by two perturbing forces: radiation pressure (RP) and Mars' oblateness (J2). At the same time, they have demonstrated that lifetimes of particles, especially of grains about ten of micrometers in size, may reach more than 10(4) years. On such timescales, the Poynting-Robertson drag (PR) becomes important. Here we provide a study of the dynamics under the combined action of all three perturbing forces. We show that a PR decay of the semimajor axes leads to an adiabatic decrease of amplitudes and periods of oscillations in orbital inclinations predicted in the framework of the underlying RP+J2 problem. Furthermore, we show that smallest of the long-lived Deimos grains (radius approximate to 5-10 mum) may reach a chaotic regime, resulting in unpredictable and abrupt changes of their dynamics. The particles just above that size (approximate to 10- 15 mum) should be the most abundant in the Deimos torus. Our dynamical analysis, combined with a more accurate study of the particle lifetimes, provides corrections to earlier predictions about the dimensions and geometry of the Deimos torus. In addition to a population, appreciably inclined and shifted towards the Sun, the torus should contain a more contracted, less asymmetric, and less tilted component between the orbits of Phobos and Deimos. (C) 2004 Elsevier Ltd. All rights reserved Y1 - 2005 SN - 0032-0633 ER -