Other
Scientific paper
Sep 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999jqsrt..63....1k&link_type=abstract
Journal of Quantitative Spectroscopy and Radiative Transfer, vol. 63, issue 1, pp. 1-14
Other
8
Cosmic Dust: Chemical Composition, Cosmic Dust: Density, Cosmic Dust: Scattering, Cosmic Dust: Radiation Pressure, Cosmic Dust: Extinction
Scientific paper
The radiation effects of nonspherical really shaped cosmic dust particles are studied. A correlation between particle shape and estimated lifetime of a particle in the solar system was studied also. The discrete dipole approximation is utilized to calculate efficiency factors for scattering, absorption, extinction and radiation pressure, respectively, and scattering phase functions. Chemical and physical properties of the sample particle U2015 B10 are obtained by laboratory analyses. The model of particle constructed using computer techniques is compared with the real photos. Results of calculations showing that Poyinting-Robertson drag used to simulate the particle motion in interplanetary space leads to incorrect results (because of the spherical shape of particle) are proposed. Therefore, for instance, a stability of zodiacal cloud cannot be explained in this manner. On the other hand, any asphericity or irregularities in particle shape will be reflected in the increase of energy scattered in the nonradial (non-forward) direction. This fact is directly connected with the lifetime of the particle in solar system - i.e. the smaller the energy scattered forwardly the greater possibility of increasing the particle lifetime. The stability of the zodiacal cloud could be then explained also by particle shape - e.g. if the zodiacal cloud consists mainly of particles similar to the authors' sample. The mean bulk density of the authors' particle (about 1.83 g cm-3) correlates well with material of carboneous chondrites of density about 2.1 g cm-3 (from asteroids or comets, too). This particle could belong also to the debris (remnants) of Population I, i.e. to large grains with density approx. 2-3 g cm-3.
Kapisinsky I.
Kocifaj Miroslav
Kundracik F.
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