Crater modification and geologic activity in Enceladus' heavily cratered plains: Evidence from the impact crater distribution

Kirchoff, M. R.; Schenk, P.

doi:10.1016/j.icarus.2009.03.034

Cited by 71 publications

(130 citation statements)

References 32 publications

(51 reference statements)

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“…Zahnle et al (2003) Smith et al (1982) from the Voyager observations are between our values of the current cratering rates for s 2 = 2.5 and s 2 = 3.5. Kirchoff & Schenk (2009, 2010, presented the cumulative number of craters of different sizes (N o (>D)) per 10 6 km 2 for selected areas on each satellite. We take the data from their Figs.…”

Section: Resultsmentioning

confidence: 99%

“…This suggests that any possible geologic activity at Mimas, if there is any, is at a low level. Kirchoff & Schenk (2009, 2010 present counts of craters on Mimas. In Fig.…”

Section: Mimasmentioning

confidence: 99%

“…The number of craters for s 2 = 2.5 is much less than the observed values. Kirchoff & Schenk (2009) obtained the cumulative crater size-frequency distribution for certain diameter ranges. For 4 km < D < 10 km the cumulative slope is −1.548, for 10 km < D < 20 km it is −2.12, and for 20 km < D < 70 km it is −3.0.…”

Section: Mimasmentioning

confidence: 99%

“…Cassini observations of the Saturnian system provide high-resolution images that allowed the Cassini team to obtain impact cratering records on their surfaces. Kirchoff & Schenk (2009) and (2010) (KS09 and KS10 in the following) analyzed Cassini images and obtained the number and sizefrequency distribution of craters for the mid-sized icy satellites. Although the counts are not from the complete surface (Kirchoff, priv.…”

Section: Introductionmentioning

confidence: 99%

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The production of craters on the mid-sized saturnian satellites by Centaur objects

Sisto

Zanardi

2013

A&A

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Context. The Saturnian satellite system has been observed in detail by the Cassini-Huygens mission. These satellites present different surface features, including impact craters caused by small objects probably coming from the trans-Neptunian region. Aims. In this paper we calculate the production of craters on the mid-sized Saturnian satellites produced by Centaurs from the scattered disk (SD) and plutinos in order to determine this contribution, and we compare our estimations with the Cassini observations. Methods. We used a method developed in a previous paper that uses a numerical investigation of the dynamical evolution of Centaur objects to calculate the production of craters. We used a size-frequency distribution (SFD) of scattered disk objects (SDOs) as a power law with a break at diameters d = 60 km considering two cases for the differential power-law index: s 2 = 2.5 and s 2 = 3.5 for d < 60 km. Results. We calculated the number of craters, the greatest crater produced by Centaurs from the SD and plutinos, and the present cratering rate on each of the mid-sized satellites, for both cases of the SFD of SDOs considered. The contribution of plutinos is negligible compared to SDOs. From our calculations and the comparison with observations we note that the calculated number of craters for s 2 = 3.5 is in general nearer the observed number. However, in general for smaller craters, the observed number is less than the calculated one. This trend can be explained by at least two mechanisms. On the one hand, this could be caused by an erasing process that gradually buries the craters, which does not affect large craters. On the other hand, the comparison of the calculated and observed crater size-frequency distribution for different size ranges implies that for d < 60 km, the SFD of SDOs is consistent with the assumed index s 2 = 3.5, for d 0.2−1.4 km and for d 0.2−1.4 km, it is consistent with s 2 = 2.5. Then in the range d ∼ 0.2−1.4 km, the SFD of SDOs could have a new break. This change of slope could explain the reduction of small craters, at least for some cases. Conclusions. We found a good agreement when comparing our results with observations. However, independent determination of surface ages and geological processes are needed to determine if there is a new break on the SFD of SDOs, if there is a planetocentric source of craters in the Saturnian system, and which craters are primordial.

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Section: Resultsmentioning

confidence: 99%

“…This suggests that any possible geologic activity at Mimas, if there is any, is at a low level. Kirchoff & Schenk (2009, 2010 present counts of craters on Mimas. In Fig.…”

Section: Mimasmentioning

confidence: 99%

Section: Mimasmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The production of craters on the mid-sized saturnian satellites by Centaur objects

Sisto

Zanardi

2013

A&A

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“…2.18 where b ∼ 0.9−1.2 [Dones et al, 2009]. Likewise, taking either the cumulative number density slopes or the differential slopes gives regolith overturn timescales that are all negative Kirchoff and Schenk [2009].…”

Section: B Cratering Studies On the Icy Saturnian Satellitesmentioning

confidence: 99%

Radiation Effects on Airless Bodies in Space: Radiolysis, Sputtering, and Sintering in Regoliths

Schaible¹

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Particle deposition on the saturnian satellites from ephemeral cryovolcanism on Enceladus

Hirata

Miyamoto

Showman

2014

Geophysical Research Letters

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The geologically active south pole of Enceladus generates a plume of micron-sized particles, which likely form Saturn's tenuous E-ring extending from the orbit of Mimas to Titan. Interactions between these particles and satellites have been suggested, though only as very thin surficial phenomena. We scrutinize high-resolution images with a newly developed numerical shape model of Helene and find that the leading hemisphere of Helene is covered by thick deposits of E-ring particles, which occasionally collapse to form gully-like depressions. The depths of the resultant gullies and near-absence of small craters on the leading hemisphere indicate that the deposit is tens to hundreds of meters thick. The ages of the deposits are less than several tens of My, which coincides well with similar deposits found on Telesto and Calypso. Our findings as well as previous theoretical work collectively indicate that the cryovolcanic activity currently occurring on Enceladus is ephemeral.

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Crater modification and geologic activity in Enceladus' heavily cratered plains: Evidence from the impact crater distribution

Cited by 71 publications

References 32 publications

The production of craters on the mid-sized saturnian satellites by Centaur objects

The production of craters on the mid-sized saturnian satellites by Centaur objects

Radiation Effects on Airless Bodies in Space: Radiolysis, Sputtering, and Sintering in Regoliths

Particle deposition on the saturnian satellites from ephemeral cryovolcanism on Enceladus

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