dc.contributor.author
Parekh, Rutu
dc.contributor.author
Otto, K. A.
dc.contributor.author
Matz, K. D.
dc.contributor.author
Jaumann, Ralf
dc.contributor.author
Krohn, K.
dc.contributor.author
Roatsch, T.
dc.contributor.author
Kersten, E.
dc.contributor.author
Elgner, S.
dc.contributor.author
Russell, C. T.
dc.contributor.author
Raymond, C. A.
dc.date.accessioned
2022-01-11T10:52:13Z
dc.date.available
2022-01-11T10:52:13Z
dc.identifier.uri
https://refubium.fu-berlin.de/handle/fub188/33442
dc.identifier.uri
http://dx.doi.org/10.17169/refubium-33163
dc.description.abstract
Dust and melt ponds have been studied on planetary bodies including Eros, Itokawa, and the Moon. However, depending on the nature of the regolith material properties and the location of the planetary body, the formation mechanism of the ponded features varies. On Eros and Itokawa, ponded features are formed from dry regolith materials whereas on the Moon similar features are thought to be produced by ejecta melt. On the surface of Vesta, we have identified type 1, ejecta ponds, and type 2, dust ponds. On Vesta type 1 pond are located in the vicinity of ejecta melt of large impact craters. The material is uniformly distributed across the crater floor producing smooth pond surfaces which have a constant slope and shallow depth. The hosting crater of melt-like ponds has a low raised rim and is located on relatively low elevated regions. Whereas, the type 2 ponds on Vesta reveal an undulating surface that is frequently displaced from the crater center or extends toward the crater wall with an abruptly changing slope. We suggested that for the production of the type 2 ponds, localized seismic diffusion and volatile-induced fluidization may be responsible for Vesta. Due to Vesta's large size (in comparison to Eros and Itokawa), the surface may have experienced local-scale rare high-amplitude seismic diffusion which was sufficient to drift fine material. Similarly, short-lived volatile activities were capable to transfer dusty material on to the surface. Segregation and smoothing of transferred material lack further surface activities, hindering the formation of smooth morphology.
en
dc.format.extent
17 Seiten
dc.rights.uri
https://creativecommons.org/licenses/by-nc/4.0/
dc.subject
fine-grained
en
dc.subject.ddc
500 Naturwissenschaften und Mathematik::520 Astronomie::520 Astronomie und zugeordnete Wissenschaften
dc.title
Formation of Ejecta and Dust Pond Deposits on Asteroid Vesta
dc.type
Wissenschaftlicher Artikel
dcterms.bibliographicCitation.articlenumber
e2021JE006873
dcterms.bibliographicCitation.doi
10.1029/2021JE006873
dcterms.bibliographicCitation.journaltitle
JGR: Planets
dcterms.bibliographicCitation.number
11
dcterms.bibliographicCitation.volume
126
dcterms.bibliographicCitation.url
https://doi.org/10.1029/2021JE006873
refubium.affiliation
Geowissenschaften
refubium.affiliation.other
Institut für Geologische Wissenschaften / Fachrichtung Planetologie und Fernerkundung
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refubium.resourceType.isindependentpub
no
dcterms.accessRights.openaire
open access
dcterms.isPartOf.eissn
2169-9100
refubium.resourceType.provider
WoS-Alert