Abstract
The density of the Galactic meteoroid background formed by the loss of large dust grains escaped from circumstellar disks during the formation of a star is estimated. This density is shown to be substantially higher than the local density of meteoroids that escaped from dusty stellar disks as a result of two-star collisions. The flux of meteors of the Galactic background near the Earth is calculated for a given latitude of the observing site taking into account the velocity distribution of dust particles and the motion of particles in the solar gravity field. The expected rate of the Galactic background meteor events at the AMOR radar latitude is lower by at least a factor of 30 than the reported frequency of interstellar meteor events that are supposedly registered in the AMOR experiment.
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