@article{GordonKrivovSchmidtetal.2002,
  author    = {Gordon, M. K. and Krivov, Alexander V. and Schmidt, J{\"u}rgen and Spahn, Frank},
  title     = {Planetary rings},
  year      = {2002},
  language  = {en}
}
@article{GruenKrivov2002,
  author    = {Gr{\"u}n, Eberhard and Krivov, Alexander V.},
  title     = {Dust astronomy : new venues in interplanetary and interstellar dust research},
  isbn      = {1-58381-113-3},
  year      = {2002},
  language  = {en}
}
@article{KrivovBanaszkiewicz2001,
  author    = {Krivov, Alexander V. and Banaszkiewicz, Marek},
  title     = {Unusual origin, evolution and fate of icy ejecta from Hyperion},
  issn      = {0032-0633},
  year      = {2001},
  language  = {en}
}
@article{KrivovBanaszkiewicz2001,
  author    = {Krivov, Alexander V. and Banaszkiewicz, Marek},
  title     = {Dust Influx to Titan from Hyperion},
  isbn      = {0-7923-6946-7},
  year      = {2001},
  language  = {en}
}
@article{KrivovKrivovaSolankietal.2004,
  author    = {Krivov, Alexander V. and Krivova, Natalia A. and Solanki, S. K. and Titov, V. B.},
  title     = {Towards understanding the beta Pictoris dust stream},
  issn      = {0004-6361},
  year      = {2004},
  abstract  = {The recent radar detection by Baggaley (2000) of a collimated stream of interstellar meteoroids postulated to be sourced at beta Pictoris, a nearby star with a prominent dust disk. presents a challenge to theoreticians. Two mechanisms of possible dust ejection from beta Pic have been proposed: ejection of dust by radiation pressure from comets in eccentric orbits and by gravity of a hypothetical planet in the disk. Here we re-examine observational data and reconsider theoretical scenarios, substantiating them with detailed modeling to test whether they can explain quantitatively and simultaneously the masses, speeds, and fluxes. Our analysis of the stream geometry and kinematics confirms that beta Pic is the most likely source of the stream and suggests that an intensive dust ejection phase took place similar to0.7 Myr ago. Our dynamical simulations show that high ejection speeds retrieved from the observations can be explained by both planetary ejection and radiation pressure mechanisms, providing, however, several important constraints. In the planetary ejection scenario, only a "hot Jupiter"-type planet with a semimajor axis of less than 1 AU can be responsible for the stream, and only if the disk was dynamically "heated" by a more distant massive planet. The radiation pressure scenario also requires the presence of a relatively massive planet at several AU or more, that had heated the cometesimal disk before the ejection occurred. Finally, the dust flux measured at Earth can be brought into reasonable agreement with both scenarios, provided that beta Pic's protoplanetary disk recently passed through an intensive short-lasting (similar to0.1 Myr) clearance stage by nascent giant planets, similar to what took place in the early solar system},
  language  = {en}
}
@article{KrivovKruegerGruenetal.2002,
  author    = {Krivov, Alexander V. and Kr{\"u}ger, Harald and Gr{\"u}n, Eberhard and Thiessenhusen, Kai-Uwe and Hamilton, Douglas P.},
  title     = {A tenuous dust ring of Jupiter formed by escaping ejecta from the Galilean satellites},
  issn      = {0148-0227},
  year      = {2002},
  language  = {en}
}
@article{KrivovMannKrivova2000,
  author    = {Krivov, Alexander V. and Mann, Ingrid and Krivova, Natalia A.},
  title     = {Size distributions of dust in circumstellar debris discs},
  issn      = {0935-4956},
  year      = {2000},
  language  = {en}
}
@article{KrivovSremcevicSpahn2005,
  author    = {Krivov, Alexander V. and Sremcevic, Miodrag and Spahn, Frank},
  title     = {Evolution of a Keplerian disk of colliding and fragmenting particles: a kinetic model with application to the Edgeworth-Kuiper belt},
  issn      = {0019-1035},
  year      = {2005},
  abstract  = {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},
  language  = {en}
}
@article{KrivovaKrivovMann2000,
  author    = {Krivova, Natalia A. and Krivov, Alexander V. and Mann, Ingrid},
  title     = {The disk of beta pictoris in the light of polarimetric data},
  issn      = {0004-637x},
  year      = {2000},
  language  = {en}
}
@article{KrivovaKrivovMann2000,
  author    = {Krivova, Natalia A. and Krivov, Alexander V. and Mann, Ingrid},
  title     = {Size distribution of dust in the disk of Beta Pictoris},
  isbn      = {1-58381-051-X},
  year      = {2000},
  language  = {en}
}