Properties of the dust cloud caused by the Deep Impact experiment

Jordá, L.; Lamy, P.; Faury, G.; Keller, H. U.; Hviid, S. F.; Küppers, M.; Koschny, D.; Lecacheux, J.; Gutiérrez, P. J.; Lara, L. M.

doi:10.1016/j.icarus.2006.10.004

Cited by 39 publications

(59 citation statements)

References 19 publications

(1 reference statement)

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“…Schleicher et al (2006) (8), we find n g ∼ 1 × 10 18 for particles of radius a ∼ 0:3 μm, roughly half the observational wavelength, and n g ∼ 7 × 10 16 for a ∼ 0:85 μm from the NIR data, so that the dust produced by the impact consists of considerably larger grains. Converting these values to dust masses, M c ðaÞ ∼ 4 × 10 6 kg, on the order of the Jorda et al (2007) a As derived from the listed reference using the method outlined in Bauer et al 2003b and in the text, assuming a grain density of ρ ∼ 1:0 g=cm 3 . The Q dust value is for a dust ejection velocity v ej ∼ 200 m s À1 .…”

Section: Discussionmentioning

confidence: 99%

The Large-Grained Dust Coma of 174P/Echeclus

Bauer

Choi²,

Weissman³

et al. 2008

PUBL ASTRON SOC PAC

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ABSTRACT. On 2005 December 30, Y.-J. Choi and P. R. Weissman discovered that the formerly dormant Centaur 2000 EC98 was in strong outburst. Previous observations by P. Rousselot et al. spanning a 3-year period indicated a lack of coma down to the 27 mag arcsec À2 level. We present Spitzer Space Telescope MIPS observations of this newly active Centaur-now known as 174P/Echeclus (2000 EC98)-or 60558 Echeclus-taken in 2006 late February. The images show strong signal at both the 24 and 70 μm bands and reveal an extended coma about 2′ in diameter. Analyses yield estimates of the coma signal contribution that are in excess of 90% of the total signal in the 24 μm band. Dust production estimates ranging from 1:7-4 × 10 2 kg s À1 are on the order of 30 times that seen in other Centaurs. Simultaneous visible-wavelength observations were also obtained with Palomar Observatory's 200-inch telescope, the 1.8-m Vatican Advanced Technology Telescope, the Bohyunsan Optical Astronomy Observatory (BOAO) 1.8-m telescope, and Table Mountain Observatory's 0.6-m telescope, revealing a coma morphology nearly identical to the mid-IR observations. The grain size distribution derived from the data yields a log particle mass power-law with slope parameter α ¼ À0:87 AE 0:07, and is consistent with steady cometary activity, such as that observed during the Stardust spacecraft's encounter at 81P/Wild 2, and not with an impactdriven event, such as that caused by the Deep Impact experiment.

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Section: Discussionmentioning

confidence: 99%

The Large-Grained Dust Coma of 174P/Echeclus

Bauer

Choi²,

Weissman³

et al. 2008

PUBL ASTRON SOC PAC

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“…The ejecta fragmentation (via the slope of the cumulative size distribution of the ejected fragments) in a cratering event in a geological material seems not to strongly depend on the impact incident angle, the projectile speed or the projectile material and shape, even when the fragmentation has been observed and analysed using different techniques, such as the Deep Impact event (Jorda et al, 2007). Jorda et al (2007) acquired the ejecta fragmentation result from the data gathered by the OSIRIS narrow angle camera onboard Rosetta spacecraft during an encounter with the comet 9P/Tempel-1.…”

Section: Comparison With Previous Workmentioning

confidence: 98%

“…Jorda et al (2007) acquired the ejecta fragmentation result from the data gathered by the OSIRIS narrow angle camera onboard Rosetta spacecraft during an encounter with the comet 9P/Tempel-1.…”

Section: Comparison With Previous Workmentioning

confidence: 99%

Ejecta fragmentation in impacts into gypsum and water ice

Miljković

Mason

Zarnecki

2011

Icarus

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Please cite this article as: Miljković, K., Mason, N.J., Zarnecki, J.C., Ejecta fragmentation in impacts into gypsum and water ice, Icarus (2011Icarus ( ), doi: 10.1016Icarus ( /j.icarus.2011 This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain. Ejecta fragmentation in impacts into AbstractUsing the light gas gun at the Open University's hypervelocity impact facility, a series of impact experiments exploring impacts into water ice and gypsum have been performed. Fragmentation of solid ejecta was recorded using two different methods, analysed and compared with the total ejecta. Preliminary results show that the size distribution of the ejecta fragments from water ice is very similar to those from gypsum. These results also represent a step towards a better understanding of ejecta fragmentation in geological materials, including icy surfaces in the Solar system.

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“…Comets outgas heavily as they pass through the inner solar system and are known, from spectroscopy and space missions e.g. [49][50][51], to contain a great deal of dusty material. The polar caps of Mars are also known to be rich in dust [52] with up to 6% by weight on the surface, as determined by the OMEGA instrument on Mars Express [53] and potentially more at depth.…”

Section: General Implicationsmentioning

confidence: 99%

Experimental and theoretical simulation of sublimating dusty water ice with implications for D/H ratios of water ice on Comets and Mars

et al. 2012

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Sublimation experiments have been carried out to determine the effect of the mineral dust content of porous ices on the isotopic composition of the sublimate gas over medium (days to weeks) timescales. Whenever mineral dust of any kind was present, the D/H ratio of the sublimated gas was seen to decrease with time from the bulk ratio. Fractionations of up to 2.5 were observed for dust mixing ratios of 9 wt% and higher of JSC MARS-1 regolith simulant 1-10 μm crushed and sieved fraction. These favored the presence of the light isotope, H 2 O, in the gas phase. The more dust was added to the mixture, the more pronounced was this effect. Theoretical modeling of gas migration within the porous samples and adsorption on the excavated dust grains was undertaken to explain the results. Adsorption onto the dust grains is able to explain the low D/H ratios in the sublimate gas if adsorption favors retention of HDO over H 2 O. This leads to significant isotopic enrichment of HDO on the dust over time and depletion in the amount of HDO escaping the system as sublimate gas. This effect is significant for planetary bodies on which water moves mainly through the gas phase and a significant surface reservoir of dust may be found, such as on Comets and Mars. For each of these, inferences about the bulk water D/H ratio as inferred from gas phase measurements needs to be reassessed in light of the volatile cycling history of each body.

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Properties of the dust cloud caused by the Deep Impact experiment

Cited by 39 publications

References 19 publications

The Large-Grained Dust Coma of 174P/Echeclus

The Large-Grained Dust Coma of 174P/Echeclus

Ejecta fragmentation in impacts into gypsum and water ice

Experimental and theoretical simulation of sublimating dusty water ice with implications for D/H ratios of water ice on Comets and Mars

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