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Model Calculations of Near Solar Dust Properties

Published online by Cambridge University Press:  27 February 2018

I. Mann ,
H. Ishimoto ,
H. Okamoto  and
T. Mukai
I. Mann
Affiliation:
Max-Planck-Institut für Aeronornie, Postfach 20, D-37189 Katlenburg-Lindau, Germany
H. Ishimoto
Affiliation:
Max-Planck-Institut für Aeronornie, Postfach 20, D-37189 Katlenburg-Lindau, Germany
H. Okamoto
Affiliation:
Department of Earth and Planetary Sciences, Faculty of Science, Kobe University, Nada 657, Kobe, Japan
T. Mukai
Affiliation:
Department of Earth and Planetary Sciences, Faculty of Science, Kobe University, Nada 657, Kobe, Japan

Abstract

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We discuss efforts to explain the dust distribution, as it was derived from the F-coronal brightness, mainly how to explain a constant number density near the Sun. It is shown that silicate particles have temperatures below the blackbody temperature if the impurity from absorbing material amounts to less than 0.1% in volume. This effect is especially significant for porous particles and may explain why particles can approach to less than 3 R⊙ from the Sun. Another effect may arise from particles on high eccentricity orbits and from the influence of collisional fragments. Whereas on the one hand heat resistant silicate particles may cause a stable dust cloud in the solar vicinity, on the other hand dynamical effects may cause a variation of the number density in the corona in short time scales.

Type
IX. Zodiacal Light and Thermal Emission
Information
International Astronomical Union Colloquium , Volume 150: Physics, Chemistry and Dynamics of Interplanetary Dust , 1996 , pp. 357 - 360
Copyright
Copyright © Astronomical Society of the Pacific 1996

References

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