The profile of Saturn's ring a as derived from stellar occultations
- 15 Downloads
Stellar occultations behind Saturn's ring A reveal sharp-edged gaps in its outer parts. Observed fluctuations in stellar brightness during one observation can be interpreted as Fresnel's diffraction zones. According to this the sharpness of the edges of the gap are estimated to be under 700 m, which also means that the thickness of ring A in that part cannot exceed a few hundred metres. A further conclusion is that particle size must be a lot less than a few hundred metres.
KeywordsParticle Size Outer Part Stellar Occultation Diffraction Zone Stellar Brightness
Unable to display preview. Download preview PDF.
- Ainslie, M. A.: 1971a,Monthly Notices Roy. Astron. Soc. 77, 456–459.Google Scholar
- Ainslie, M. A. and Knight, J.: 1917b,J. Brit. Astron. Assoc. 27, 212–217.Google Scholar
- Alexander, A. F. O'D.: 1962,The Planet Saturn, Faber and Faber, London, pp. 340–344, 425 and 442–443.Google Scholar
- Alfvén, H. and Arrhenius, G.: 1977,Evolution of the Solar System, NASA SP-345, pp. 140–141.Google Scholar
- Allen, C. W.: 1973,Astrophysical Quantities. Althone Press, London.Google Scholar
- Bobrov, M. A.: 1970, ‘Physical Properties of Saturn's Rings’, inSurfaces and Interiors of Planets and Satellites (A. Dollfus, ed.), Academic Press, New York, pp. 376–461.Google Scholar
- Dollfus, A.: 1970, ‘Diamètres des planètes et Satellites’, inSurfaces and Interiors of Planets and Satellites A. Dollfus, ed.), Academic Press, New York, pp. 98–110.Google Scholar
- Evans, D. S.: 1977,Sky Telesc. 54, 164–166 and 289–292.Google Scholar
- Hämeen-Anttila, K. A.: 1977,Tcarus 31, 385–400.Google Scholar
- Heath, M. B. B.: 1958,J. Brit. Astron. Assoc. 68, 57.Google Scholar