A Photometric Model of the Inclined F Ring of Saturn
| dc.contributor.author | Scharringhausen, Britt Rebecca | |
| dc.date.accessioned | 2006-10-31T14:15:00Z | |
| dc.date.available | 2006-10-31T14:15:00Z | |
| dc.date.issued | 2006-10-31T14:15:00Z | |
| dc.description | Philip Nicholson Joseph Burns Riccardo Giovanelli Peter Gierasch | en_US |
| dc.description.abstract | Observations by Hubble Space Telescope (HST) of the rings of Saturn during the 1995 ring-plane crossing revealed a surprising asymmetry in the brightness of the east and west ansae. As in historical observations, the ring brightness was nonzero at the time that the rings are observed edge-on. We create a photometric model of the ring system with the F ring inclined to the main ring plane which re- produces the observed brightness of the rings and the asymmetry in ring brightness after the ring-plane crossing. The F ring is modeled as "ribbon" 60 km tall, of indeterminate radial width, with a gaussian profile of optical depth as a function of height with an equivalent depth of D=10+/-4 km and a full width at half maximum of 13+/-7 km. This is the first estimate of the physical vertical thickness of the F ring, which we find is approximately 1000 times greater than the main ring thickness. The model shows that as the Earth crosses the main ring plane, the F ring dominates the brightness of the system, and that the asymmetry in ring brightness after the ring-plane crossing is caused by asymmetric absorption of light from the main rings by the front of the F ring. The model gives post-crossing asymmetries in good agreement with the HST data, but fails to reproduce the small asymmetries in ring brightness observed before the ring-plane crossing. The model profiles of ring brightness plotted vs. horizontal distance from the center of Saturn show many of the features observed in the HST profiles. However, the F ring in this model is longitudinally symmetric, and does not include the many clumps or arcs that have been observed in the real F ring. It therefore cannot reproduce many of the small-scale variations seen in the HST profiles. It may be that these small features are responsible for the asymmetries observed before the ring-plane crossing. | en_US |
| dc.format.extent | 1483301 bytes | |
| dc.format.mimetype | application/pdf | |
| dc.identifier.uri | https://hdl.handle.net/1813/3707 | |
| dc.language.iso | en_US | en_US |
| dc.relation.isformatof | bibid: 6475875 | |
| dc.subject | saturnshine | en_US |
| dc.subject | reflectance | en_US |
| dc.subject | Saturn | en_US |
| dc.subject | rings | en_US |
| dc.subject | F ring | en_US |
| dc.subject | photometry | en_US |
| dc.subject | ring-plane crossing | en_US |
| dc.title | A Photometric Model of the Inclined F Ring of Saturn | en_US |
| dc.type | dissertation or thesis | en_US |
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