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• W1654728492 abstract "Since the dark “holes” in the Milky Way were discovered to be caused by cosmic dust [1], it’s been established that dust is a ubiquitous component in the cosmic environment. Within the solar system, dust grains are exposed to the solar photon flux, electrons and ions in the solar wind, as well as highly energetic particles. As a result, these dust grains are charged and influenced by electric and magnetic fields [2]. The grain charge plays an important role in many dynamical and physical processes such as coagulation in dust clouds, levitation and dynamics in the interplanetary medium and on planetary surfaces and in rings [3]. The coagulation of cosmic dust grains is a fundamental process which can take place in many astrophysical environments, such as presolar nebulae, circumstellar disks, proplanetary disks and cometary tails. Since most cosmic dust grains are charged, the electrostatic force between dust grains can strongly affect the coagulation rate. There have been experimental and numerical studies on the charging processes and coagulation of dust grains [4-8]. Meyer-Vernet [4] first proposed that identical grains with different charging histories could achieve opposite charges, even though they are immersed in the same environment. This is due to the fact that the equilibrium equation for the charge on a single sphere due to the ambient plasma and secondary electron emission can have multiple roots. The surface potentials on two grains could therefore be of opposite sign, depending on the charging history. Meyer-Vernet also pointed out that a small disturbance in the environment may induce large and rapid charge variations on the grain surface. This idea was further developed by Horanyi & Goertz [5], who showed that fluctuations in the plasma temperature allowed different sized dust grains to acquire opposite charges, which greatly enhances the coagulation rate. This process is one of the most efficient mechanisms for the growth of aggregates, leading to onset of “gelation” or runaway growth [7, 8]. However, most of the previous related work has been based on the assumption that the dust grains are isolated spherical grains. Since colliding grains produce irregular aggregates, a detailed understanding of charging of aggregates has profound significance in terms of understanding many astrophysical phenomena. We consider silicates within a size range 5 nm ≤ a ≤ 2 μm to be representative of interplanetary dust. Aggregates consisting of monomers of different sizes are built using “Aggregate Builder” [9]. The algorithm takes both monopole and dipole interactions of the grain’s electrostatic potential into account. The dipoledipole interaction can cause the aggregates to rotate as they approach one another. Only true collisions between the aggregates are detected. A sample aggregate is shown in Fig. 1." @default.
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• W1654728492 date "2011-03-01" @default.
• W1654728492 modified "2023-09-26" @default.
• W1654728492 title "Charging of Interplanetary Dust Grains and Consequences for Aggregation" @default.
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