Cryogenic flow features on Ceres: Implications for crater-related cryovolcanism

K. Krohn; R. Jaumann; K. Stephan; K. A. Otto; N. Schmedemann; R. J. Wagner; K. D. Matz; F. Tosi; F. Zambon; I. von der Gathen; F. Schulzeck; S. E. Schröder; D. L. Buczkowski; H. Hiesinger; H. Y. McSween; C. M. Pieters; F. Preusker; T. Roatsch; C. A. Raymond; C. T. Russell; David Williams

doi:10.1002/2016GL070370

Cryogenic flow features on Ceres: Implications for crater-related cryovolcanism

K. Krohn, R. Jaumann, K. Stephan, K. A. Otto, N. Schmedemann, R. J. Wagner, K. D. Matz, F. Tosi, F. Zambon, I. von der Gathen, F. Schulzeck, S. E. Schröder, D. L. Buczkowski, H. Hiesinger, H. Y. McSween, C. M. Pieters, F. Preusker, T. Roatsch, C. A. Raymond, C. T. RussellDavid Williams

Earth and Space Exploration, School of (SESE)

Research output: Contribution to journal › Article › peer-review

46 Scopus citations

Abstract

Craters on Ceres, such as Haulani, Kupalo, Ikapati, and Occator show postimpact modification by the deposition of extended plains material with pits, multiple lobate flows, and widely dispersed deposits that form a diffuse veneer on the preexisting surface. Bright material units in these features have a negative spectral slope in the visible range, making it appear bluish with respect to the grey-toned overall surface of Ceres. We calculate the drop height-to-runout length ratio of several flow features and obtain a coefficient of friction of < 0.1: The results imply higher flow efficiency for flow features on Ceres than for similar features on other planetary bodies with similar gravity, suggesting low-viscosity material. The special association of flow features with impact craters could either point to an impact melt origin or to an exogenic triggering of cryovolcanic processes.

Original language	English (US)
Pages (from-to)	11,994-12,003
Journal	Geophysical Research Letters
Volume	43
Issue number	23
DOIs	https://doi.org/10.1002/2016GL070370
State	Published - Dec 16 2016

Keywords

coefficient of friction
cryovolcanism
dwarf planet Ceres
flow features
impact melt
subsurface materials

ASJC Scopus subject areas

Geophysics
General Earth and Planetary Sciences

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10.1002/2016GL070370

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Krohn, K., Jaumann, R., Stephan, K., Otto, K. A., Schmedemann, N., Wagner, R. J., Matz, K. D., Tosi, F., Zambon, F., von der Gathen, I., Schulzeck, F., Schröder, S. E., Buczkowski, D. L., Hiesinger, H., McSween, H. Y., Pieters, C. M., Preusker, F., Roatsch, T., Raymond, C. A., ... Williams, D. (2016). Cryogenic flow features on Ceres: Implications for crater-related cryovolcanism. Geophysical Research Letters, 43(23), 11,994-12,003. https://doi.org/10.1002/2016GL070370

Krohn, K, Jaumann, R, Stephan, K, Otto, KA, Schmedemann, N, Wagner, RJ, Matz, KD, Tosi, F, Zambon, F, von der Gathen, I, Schulzeck, F, Schröder, SE, Buczkowski, DL, Hiesinger, H, McSween, HY, Pieters, CM, Preusker, F, Roatsch, T, Raymond, CA, Russell, CT & Williams, D 2016, 'Cryogenic flow features on Ceres: Implications for crater-related cryovolcanism', Geophysical Research Letters, vol. 43, no. 23, pp. 11,994-12,003. https://doi.org/10.1002/2016GL070370

@article{e9d3bc8d030445ee96cee719f688de85,

title = "Cryogenic flow features on Ceres: Implications for crater-related cryovolcanism",

abstract = "Craters on Ceres, such as Haulani, Kupalo, Ikapati, and Occator show postimpact modification by the deposition of extended plains material with pits, multiple lobate flows, and widely dispersed deposits that form a diffuse veneer on the preexisting surface. Bright material units in these features have a negative spectral slope in the visible range, making it appear bluish with respect to the grey-toned overall surface of Ceres. We calculate the drop height-to-runout length ratio of several flow features and obtain a coefficient of friction of < 0.1: The results imply higher flow efficiency for flow features on Ceres than for similar features on other planetary bodies with similar gravity, suggesting low-viscosity material. The special association of flow features with impact craters could either point to an impact melt origin or to an exogenic triggering of cryovolcanic processes.",

keywords = "coefficient of friction, cryovolcanism, dwarf planet Ceres, flow features, impact melt, subsurface materials",

author = "K. Krohn and R. Jaumann and K. Stephan and Otto, {K. A.} and N. Schmedemann and Wagner, {R. J.} and Matz, {K. D.} and F. Tosi and F. Zambon and {von der Gathen}, I. and F. Schulzeck and Schr{\"o}der, {S. E.} and Buczkowski, {D. L.} and H. Hiesinger and McSween, {H. Y.} and Pieters, {C. M.} and F. Preusker and T. Roatsch and Raymond, {C. A.} and Russell, {C. T.} and David Williams",

note = "Funding Information: We thank the Dawn team for the development, cruise, orbital insertion, and operations of the Dawn spacecraft at Ceres. Portions of this work were performed at the DLR Institute of Planetary Research, at the Jet Propulsion Laboratory (JPL) under contract with NASA. Dawn data are archived with the NASA Planetary Data System (http://sbn.pds.nasa.gov/). K. Krohn is supported by the Helmholtz Association (HGF) through the research Helmholtz Postdoc Program. Publisher Copyright: {\textcopyright}2016. American Geophysical Union. All Rights Reserved.",

year = "2016",

month = dec,

day = "16",

doi = "10.1002/2016GL070370",

language = "English (US)",

volume = "43",

pages = "11,994--12,003",

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TY - JOUR

T1 - Cryogenic flow features on Ceres

T2 - Implications for crater-related cryovolcanism

AU - Krohn, K.

AU - Jaumann, R.

AU - Stephan, K.

AU - Otto, K. A.

AU - Schmedemann, N.

AU - Wagner, R. J.

AU - Matz, K. D.

AU - Tosi, F.

AU - Zambon, F.

AU - von der Gathen, I.

AU - Schulzeck, F.

AU - Schröder, S. E.

AU - Buczkowski, D. L.

AU - Hiesinger, H.

AU - McSween, H. Y.

AU - Pieters, C. M.

AU - Preusker, F.

AU - Roatsch, T.

AU - Raymond, C. A.

AU - Russell, C. T.

AU - Williams, David

N1 - Funding Information: We thank the Dawn team for the development, cruise, orbital insertion, and operations of the Dawn spacecraft at Ceres. Portions of this work were performed at the DLR Institute of Planetary Research, at the Jet Propulsion Laboratory (JPL) under contract with NASA. Dawn data are archived with the NASA Planetary Data System (http://sbn.pds.nasa.gov/). K. Krohn is supported by the Helmholtz Association (HGF) through the research Helmholtz Postdoc Program. Publisher Copyright: ©2016. American Geophysical Union. All Rights Reserved.

PY - 2016/12/16

Y1 - 2016/12/16

N2 - Craters on Ceres, such as Haulani, Kupalo, Ikapati, and Occator show postimpact modification by the deposition of extended plains material with pits, multiple lobate flows, and widely dispersed deposits that form a diffuse veneer on the preexisting surface. Bright material units in these features have a negative spectral slope in the visible range, making it appear bluish with respect to the grey-toned overall surface of Ceres. We calculate the drop height-to-runout length ratio of several flow features and obtain a coefficient of friction of < 0.1: The results imply higher flow efficiency for flow features on Ceres than for similar features on other planetary bodies with similar gravity, suggesting low-viscosity material. The special association of flow features with impact craters could either point to an impact melt origin or to an exogenic triggering of cryovolcanic processes.

AB - Craters on Ceres, such as Haulani, Kupalo, Ikapati, and Occator show postimpact modification by the deposition of extended plains material with pits, multiple lobate flows, and widely dispersed deposits that form a diffuse veneer on the preexisting surface. Bright material units in these features have a negative spectral slope in the visible range, making it appear bluish with respect to the grey-toned overall surface of Ceres. We calculate the drop height-to-runout length ratio of several flow features and obtain a coefficient of friction of < 0.1: The results imply higher flow efficiency for flow features on Ceres than for similar features on other planetary bodies with similar gravity, suggesting low-viscosity material. The special association of flow features with impact craters could either point to an impact melt origin or to an exogenic triggering of cryovolcanic processes.

KW - coefficient of friction

KW - cryovolcanism

KW - dwarf planet Ceres

KW - flow features

KW - impact melt

KW - subsurface materials

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U2 - 10.1002/2016GL070370

DO - 10.1002/2016GL070370

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VL - 43

SP - 11,994-12,003

JO - Geophysical Research Letters

JF - Geophysical Research Letters

IS - 23

ER -

Cryogenic flow features on Ceres: Implications for crater-related cryovolcanism

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