Particle sizes of the Uranus delta ring's inner diffuse companion through comparison of RSS and PPS voyager occultation data
| ISSN: |
0019-1035
|
|---|---|
| Source: |
Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
|
| Topics: |
Physics
|
| Type of Medium: |
Electronic Resource
|
| URL: |
| _version_ | 1798290862216577025 |
|---|---|
| autor | Hui, J. Horn, L.J. Lane, A.L. |
| autorsonst | Hui, J. Horn, L.J. Lane, A.L. |
| book_url | http://dx.doi.org/10.1016/0019-1035(91)90217-H |
| datenlieferant | nat_lic_papers |
| fussnote | The Voyager 2 spacecraft encountered the Uranian system in January 1986. Several occultations of the Uranian rings were observed including a radio science (RSS) earth occultation and two stellar occultations. The photopolarimeter (PPS) and ultraviolet spectrometer (UVS) observed the stars σ Sagitarii and β Persei as they were occulted by the δ ring. An inner diffuse companion of the δ ring was detected in the RSS data taken at λ = 3.6 cm and in both the PPS and the UVS σ Sagitarii occultation data taken at λ = 0.26 and λ = 0.11 μm, respectively. The diffuse companion was not observable above the background noise level in the PPS β Persei data because of low signal to noise ratio nor in the UVS β Persei data because of high magnetospheric background. The companion has also been observed in Earth-based stellar occultation observations. Using the PPS σ Sagitarii and RSS data, we found the inner diffuse companion of the δ ring to have an average width of 12 km with an average RSS equivalent depth of 0.60 +/- 0.080 km and an average PPS equivalent depth of 0.36 +/- 0.054 km. The RSS opacity is roughly twice that of the PPS opacity because the RSS extinction coefficient is twice that of PPS, which accounts for the factor of two. From comparing the widths and equivalent depth between the two sets of data, we found that the particles that contribute the most to the integrated opacities of the companion are particles which have sizes in the several centimeter or greater regime. These particles seem to be located away from the PPS edges, where there may be particles that have sizes smaller than a few centimeters. This would account for the higher equivalent depths and larger widths seen in the PPS data. |
| hauptsatz | hsatz_simple |
| identnr | NLZ180443828 |
| issn | 0019-1035 |
| journal_name | Icarus |
| materialart | 1 |
| package_name | Elsevier |
| publikationsort | Amsterdam |
| publisher | Elsevier |
| reference | 93 (1991), S. 347-353 |
| search_space | articles |
| shingle_author_1 | Hui, J. Horn, L.J. Lane, A.L. |
| shingle_author_2 | Hui, J. Horn, L.J. Lane, A.L. |
| shingle_author_3 | Hui, J. Horn, L.J. Lane, A.L. |
| shingle_author_4 | Hui, J. Horn, L.J. Lane, A.L. |
| shingle_catch_all_1 | Hui, J. Horn, L.J. Lane, A.L. Particle sizes of the Uranus delta ring's inner diffuse companion through comparison of RSS and PPS voyager occultation data 0019-1035 00191035 Elsevier |
| shingle_catch_all_2 | Hui, J. Horn, L.J. Lane, A.L. Particle sizes of the Uranus delta ring's inner diffuse companion through comparison of RSS and PPS voyager occultation data 0019-1035 00191035 Elsevier |
| shingle_catch_all_3 | Hui, J. Horn, L.J. Lane, A.L. Particle sizes of the Uranus delta ring's inner diffuse companion through comparison of RSS and PPS voyager occultation data 0019-1035 00191035 Elsevier |
| shingle_catch_all_4 | Hui, J. Horn, L.J. Lane, A.L. Particle sizes of the Uranus delta ring's inner diffuse companion through comparison of RSS and PPS voyager occultation data 0019-1035 00191035 Elsevier |
| shingle_title_1 | Particle sizes of the Uranus delta ring's inner diffuse companion through comparison of RSS and PPS voyager occultation data |
| shingle_title_2 | Particle sizes of the Uranus delta ring's inner diffuse companion through comparison of RSS and PPS voyager occultation data |
| shingle_title_3 | Particle sizes of the Uranus delta ring's inner diffuse companion through comparison of RSS and PPS voyager occultation data |
| shingle_title_4 | Particle sizes of the Uranus delta ring's inner diffuse companion through comparison of RSS and PPS voyager occultation data |
| sigel_instance_filter | dkfz geomar wilbert ipn albert fhp |
| source_archive | Elsevier Journal Backfiles on ScienceDirect 1907 - 2002 |
| timestamp | 2024-05-06T08:23:28.003Z |
| titel | Particle sizes of the Uranus delta ring's inner diffuse companion through comparison of RSS and PPS voyager occultation data |
| titel_suche | Particle sizes of the Uranus delta ring's inner diffuse companion through comparison of RSS and PPS voyager occultation data The Voyager 2 spacecraft encountered the Uranian system in January 1986. Several occultations of the Uranian rings were observed including a radio science (RSS) earth occultation and two stellar occultations. The photopolarimeter (PPS) and ultraviolet spectrometer (UVS) observed the stars σ Sagitarii and β Persei as they were occulted by the δ ring. An inner diffuse companion of the δ ring was detected in the RSS data taken at λ = 3.6 cm and in both the PPS and the UVS σ Sagitarii occultation data taken at λ = 0.26 and λ = 0.11 μm, respectively. The diffuse companion was not observable above the background noise level in the PPS β Persei data because of low signal to noise ratio nor in the UVS β Persei data because of high magnetospheric background. The companion has also been observed in Earth-based stellar occultation observations. Using the PPS σ Sagitarii and RSS data, we found the inner diffuse companion of the δ ring to have an average width of 12 km with an average RSS equivalent depth of 0.60 +/- 0.080 km and an average PPS equivalent depth of 0.36 +/- 0.054 km. The RSS opacity is roughly twice that of the PPS opacity because the RSS extinction coefficient is twice that of PPS, which accounts for the factor of two. From comparing the widths and equivalent depth between the two sets of data, we found that the particles that contribute the most to the integrated opacities of the companion are particles which have sizes in the several centimeter or greater regime. These particles seem to be located away from the PPS edges, where there may be particles that have sizes smaller than a few centimeters. This would account for the higher equivalent depths and larger widths seen in the PPS data. |
| topic | U |
| uid | nat_lic_papers_NLZ180443828 |