Distribution of the Resonant Particles in the Zodiacal Cloud: a New Approach

Details Distribution of the Resonant Particles in the Zodiacal Cloud: a New Approach Distribution of the Resonant Particles in the Zodiacal Cloud: a New Approach

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aas...190.0501g&link_type=abstract

American Astronomical Society, 190th AAS Meeting, #05.01; Bulletin of the American Astronomical Society, Vol. 29, p.782

Astronomy and Astrophysics

Astronomy

1

Scientific paper

As we have shown earlier, the interplanetary dust flow evolution can be conveniently described by the continuity equation written in the space of orbital coordinates such as semimajor axis a, eccentricity e, inclination i, etc. (Gor'kavyi, Ozernoy, & Mather 1997). Having accounted for the Poynting-Robertson (P-R) drag as the leading effect for dynamics of small dust particles, we have computed a `reference model' for the 3-D structure of the zodiacal cloud produced by 217 comets and 5000 asteroids (Gor'kavyi, Ozernoy, Mather & Taidakova 1997 equiv GOMT). In order to make our reference model complete, one needs to include in it those ~ 10% of particles which are subjected to resonant effects. For a resonant line a=const in the (a,e)-space, we solve analytically a new 1-D transport equation (see GOMT) and then find the distribution of resonant particles in the zodiacal cloud. This enables us to compute the (a,e)-distribution of resonant particles in the zodiacal cloud for about two dozen different resonances near Earth. Using our transformation equations, we make a transition from the space of orbital coordinates to the r,z-space, which completes the finding of the resonant ring near the Earth averaged over the direction of particle's perihelion. We calculate the number densities and masses of the asteroidal and cometary components of the resonant and non resonant populations of the zodiacal cloud near the Earth. A substantial advantage of this approach is that, as opposed to previous work on resonant particles, it enables us to compute the particle's distribution in eccentricity in the vicinity of every resonant orbit. References: {Gor'kavyi, N., Ozernoy, L. & Mather, J. 1997, ApJ 474, 496. Gor'kavyi, N., Ozernoy, L., Mather, J. & Taidakova, T. 1996, Bull. AAS 28, 1300; ApJ 1997 (submitted) (equiv GOMT)}

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