Abstract
AbstractYielding the inner continuation of the interplanetary dust cloud, the dust at about 0.3 AU and closer to the Sun is studied under observing conditions different from those of the Zodiacal light. The F-coronal brightness indicates its optical particle properties as well as its overall spatial distribution. The present knowledge is based on visible and near infrared F-coronal observations and may be improved from data of the SOHO satellite in the near future. Some dynamical effects become particulary important for sub-μm particles in the solar vicinity. However, these particles seem to have only a small effect on the observable corona brightness, but are more accessible to in-situ experiments.
Publisher
Cambridge University Press (CUP)
Reference47 articles.
1. Tsurutani B. T. , & Randolph J.E. 1991, in Origin & Evolution of Interplanetary Dust, A.-C. Levasseur-Regourd & H. Hasegawa, Dordrecht: Kluwer, 29
2. Tollestrup E. V. , Fazio G. G. , Woolaway J. , Blackwell J. , & Brecher K. 1994, in Infrared Solar Physics, D. Rabin J. T. Jefferies , & C. Lindsey , Dordrecht: Kluwer, 179
3. The path and surviving tail of a comet that fell into the sun
4. Scherer K. , Fahr H. J. , & Banaszkiewicz M. , Icarus, submitted.