Structure, stability and evolution of Saturn's rings
Recent data obtained from the Voyager spacecrafts and ground-based measurements indicate: (1) the rings have a thickness of at most 150 m (ref. 1) and probably several times less 2,3 ; (2) the rings are mostly composed of ice particles ranging from centimetres to metres in size 4 ; (3) the rings are...
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| Veröffentlicht in: | Nature (London) 1984-01, Vol.309 (5966), p.333-335 |
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| creator | Bridges, Frank G. Hatzes, A. Lin, D. N. C. |
| description | Recent data obtained from the Voyager spacecrafts and ground-based measurements indicate: (1) the rings have a thickness of at most 150 m (ref. 1) and probably several times less
2,3
; (2) the rings are mostly composed of ice particles ranging from centimetres to metres in size
4
; (3) the rings are subdivided into a large number of ringlets with a radial dimension ranging from 10-km down to the several metres resolution of the Voyager spacecraft's camera
5
; (4) the B ring contains very many optical depth variations (0.6–3)
3
. This behaviour is essentially determined by the collisional properties of the rings' ice particles. Here we report some preliminary results from an experiment designed to measure the coefficient of restitution of ice particles colliding at impact velocities relevant to Saturn's rings. We apply these results to simple dynamical models for Saturn's rings and deduce the rings' thickness to be ≺5 m. We also show that regions with optical depth |
| doi_str_mv | 10.1038/309333a0 |
| format | Article |
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2,3
; (2) the rings are mostly composed of ice particles ranging from centimetres to metres in size
4
; (3) the rings are subdivided into a large number of ringlets with a radial dimension ranging from 10-km down to the several metres resolution of the Voyager spacecraft's camera
5
; (4) the B ring contains very many optical depth variations (0.6–3)
3
. This behaviour is essentially determined by the collisional properties of the rings' ice particles. Here we report some preliminary results from an experiment designed to measure the coefficient of restitution of ice particles colliding at impact velocities relevant to Saturn's rings. We apply these results to simple dynamical models for Saturn's rings and deduce the rings' thickness to be ≺5 m. We also show that regions with optical depth <0.5, such as the B ring, are unstable to viscous diffusion. Such an instability may be the cause of optical depth variations in the B ring.</description><identifier>ISSN: 0028-0836</identifier><identifier>EISSN: 1476-4687</identifier><identifier>DOI: 10.1038/309333a0</identifier><identifier>CODEN: NATUAS</identifier><language>eng</language><publisher>London: Nature Publishing Group UK</publisher><subject>Astronomy ; Earth, ocean, space ; Exact sciences and technology ; Humanities and Social Sciences ; letter ; multidisciplinary ; Planets, their satellites and rings. Asteroids ; Saturn ; Science ; Science (multidisciplinary) ; Solar system</subject><ispartof>Nature (London), 1984-01, Vol.309 (5966), p.333-335</ispartof><rights>Springer Nature Limited 1984</rights><rights>1985 INIST-CNRS</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-a408t-46ae1ebce577caec069b0c7ca8b4c31dd7f02995dc7c283e0b0c1aacb1f929283</citedby><cites>FETCH-LOGICAL-a408t-46ae1ebce577caec069b0c7ca8b4c31dd7f02995dc7c283e0b0c1aacb1f929283</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.1038/309333a0$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1038/309333a0$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>314,776,780,27901,27902,41464,42533,51294</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&idt=8883684$$DView record in Pascal Francis$$Hfree_for_read</backlink></links><search><creatorcontrib>Bridges, Frank G.</creatorcontrib><creatorcontrib>Hatzes, A.</creatorcontrib><creatorcontrib>Lin, D. N. C.</creatorcontrib><title>Structure, stability and evolution of Saturn's rings</title><title>Nature (London)</title><addtitle>Nature</addtitle><description>Recent data obtained from the Voyager spacecrafts and ground-based measurements indicate: (1) the rings have a thickness of at most 150 m (ref. 1) and probably several times less
2,3
; (2) the rings are mostly composed of ice particles ranging from centimetres to metres in size
4
; (3) the rings are subdivided into a large number of ringlets with a radial dimension ranging from 10-km down to the several metres resolution of the Voyager spacecraft's camera
5
; (4) the B ring contains very many optical depth variations (0.6–3)
3
. This behaviour is essentially determined by the collisional properties of the rings' ice particles. Here we report some preliminary results from an experiment designed to measure the coefficient of restitution of ice particles colliding at impact velocities relevant to Saturn's rings. We apply these results to simple dynamical models for Saturn's rings and deduce the rings' thickness to be ≺5 m. We also show that regions with optical depth <0.5, such as the B ring, are unstable to viscous diffusion. Such an instability may be the cause of optical depth variations in the B ring.</description><subject>Astronomy</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>Humanities and Social Sciences</subject><subject>letter</subject><subject>multidisciplinary</subject><subject>Planets, their satellites and rings. Asteroids</subject><subject>Saturn</subject><subject>Science</subject><subject>Science (multidisciplinary)</subject><subject>Solar system</subject><issn>0028-0836</issn><issn>1476-4687</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1984</creationdate><recordtype>article</recordtype><recordid>eNplkM1LxDAQxYMouK6Cf0IP4gdYnTTZNj3K4hcseFg9h2maSpdus2ZSYf97U3b14mmGNz_e8B5j5xzuOAh1L6AUQiAcsAmXRZ7KXBWHbAKQqRSUyI_ZCdEKAGa8kBMml8EPJgze3iYUsGq7NmwT7OvEfrtuCK3rE9ckS4xIf0WJb_tPOmVHDXZkz_Zzyj6eHt_nL-ni7fl1_rBIUYIK8TVabitjZ0Vh0BrIywpMXFUljeB1XTSQleWsjlqmhIV45Yim4k2ZlVGZssud78a7r8FS0OuWjO067K0bSGdSZgJyGcHrHWi8I_K20RvfrtFvNQc91qJ_a4noxd4TyWDXeOxNS3-8UrEjNTre7DDajJGt1ysXG4hp_1v-AJb6bog</recordid><startdate>19840101</startdate><enddate>19840101</enddate><creator>Bridges, Frank G.</creator><creator>Hatzes, A.</creator><creator>Lin, D. N. C.</creator><general>Nature Publishing Group UK</general><general>Nature Publishing</general><scope>IQODW</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope></search><sort><creationdate>19840101</creationdate><title>Structure, stability and evolution of Saturn's rings</title><author>Bridges, Frank G. ; Hatzes, A. ; Lin, D. N. C.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a408t-46ae1ebce577caec069b0c7ca8b4c31dd7f02995dc7c283e0b0c1aacb1f929283</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>1984</creationdate><topic>Astronomy</topic><topic>Earth, ocean, space</topic><topic>Exact sciences and technology</topic><topic>Humanities and Social Sciences</topic><topic>letter</topic><topic>multidisciplinary</topic><topic>Planets, their satellites and rings. Asteroids</topic><topic>Saturn</topic><topic>Science</topic><topic>Science (multidisciplinary)</topic><topic>Solar system</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Bridges, Frank G.</creatorcontrib><creatorcontrib>Hatzes, A.</creatorcontrib><creatorcontrib>Lin, D. N. C.</creatorcontrib><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Nature (London)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Bridges, Frank G.</au><au>Hatzes, A.</au><au>Lin, D. N. C.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Structure, stability and evolution of Saturn's rings</atitle><jtitle>Nature (London)</jtitle><stitle>Nature</stitle><date>1984-01-01</date><risdate>1984</risdate><volume>309</volume><issue>5966</issue><spage>333</spage><epage>335</epage><pages>333-335</pages><issn>0028-0836</issn><eissn>1476-4687</eissn><coden>NATUAS</coden><abstract>Recent data obtained from the Voyager spacecrafts and ground-based measurements indicate: (1) the rings have a thickness of at most 150 m (ref. 1) and probably several times less
2,3
; (2) the rings are mostly composed of ice particles ranging from centimetres to metres in size
4
; (3) the rings are subdivided into a large number of ringlets with a radial dimension ranging from 10-km down to the several metres resolution of the Voyager spacecraft's camera
5
; (4) the B ring contains very many optical depth variations (0.6–3)
3
. This behaviour is essentially determined by the collisional properties of the rings' ice particles. Here we report some preliminary results from an experiment designed to measure the coefficient of restitution of ice particles colliding at impact velocities relevant to Saturn's rings. We apply these results to simple dynamical models for Saturn's rings and deduce the rings' thickness to be ≺5 m. We also show that regions with optical depth <0.5, such as the B ring, are unstable to viscous diffusion. Such an instability may be the cause of optical depth variations in the B ring.</abstract><cop>London</cop><pub>Nature Publishing Group UK</pub><doi>10.1038/309333a0</doi><tpages>3</tpages></addata></record> |
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| ispartof | Nature (London), 1984-01, Vol.309 (5966), p.333-335 |
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| language | eng |
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| source | Springer Nature - Complete Springer Journals; Nature |
| subjects | Astronomy Earth, ocean, space Exact sciences and technology Humanities and Social Sciences letter multidisciplinary Planets, their satellites and rings. Asteroids Saturn Science Science (multidisciplinary) Solar system |
| title | Structure, stability and evolution of Saturn's rings |
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