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The effect of solar or stellar radiation on dust particles' trajectories (thePoynting-Robertson drag) has been studied by a number of authors and applied tointerplanetary dust dynamics in numerical computations. Meanwhile someimportant features of dust flows can be studied analytically by implementingour novel hydrodynamical approach to use the continuity equation written in theparticle's orbital elements as coordinates (Gor'kavyi, Ozernoy, & Mather 1997).By employing this approach and integrating the continuity equation, we are ableto find two integrals of motion when the Poynting-Robertson drag dominates thedissipative forces in the dust flow. These integrals of motion enable us toexplore basic characteristics of dust flows from any sources in the Solarsystem (such as asteroids, comets, Kuiper belt, etc.) or in another planetarysystem. In particular, we have reproduced the classical solution $n(r)\proptor^{-1}$ that approximately represents the overall distribution of dust in theSolar system. We have also investigated various factors that could beresponsible for the deviations of the power law index in $n(r)\proptor^{\delta}$ from $\delta=-1$, including the influences of the orbitalcharacteristics of dust sources, the evaporation of dust particles, as well asmixtures of dust particles of both asteroidal and cometary origin. We havecalculated the masses and number densities of asteroidal and cometarycomponents of the zodiacal cloud at different distances from the Sun.Comment: Accepted for publication in ApJ, v. 488, Oct. 10, 1997; 22 pages,  Latex, 12 Postscript figure

Quasi‐Stationary States of Dust Flows under Poynting‐Robertson Drag: New Analytical and Numerical Solutions