Calibration of relative sensitivity factors for impact ionization detectors with high-velocity silicate microparticles

Fiege, K.; Trieloff, M.; Hillier, Jon K.; Guglielmino, M.; Postberg, F.; Srama, R.; Kempf, S.; Blum, Jürgen

doi:10.1016/j.icarus.2014.07.015

Cited by 24 publications

(25 citation statements)

References 30 publications

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“…[H] + , [H 2 ] + , [H 3 ] + , [O] + , [O 2 ] + , [OH] + and [H 2 O] + , species dominating CDA spectra above approximately 18 km/s. It is indeed typical that the generation of such ions only occurs above specific speed thresholds in impact ionization at which the localized energy density at the impact site becomes high enough . At the lower impact speeds the slow expansion speed, and hence longer impact cloud lifetime, increase the likelihood of any minor [H] + component clustering, potentially resulting in the same lack of [H] + that would be seen if fragmentation dominated.…”

Section: Discussionmentioning

confidence: 99%

“…The impact speeds of the ice grains may be determined not only by the rise times of the charge signals on the target and/or the ion grids of CDA, and/or via spectral appearance (i.e. a decrease in cluster size, appearance of target material ions, production of ions with high ionization energies), but also through dynamical considerations. In this latter technique, the known position of the spacecraft when individual E ring ice grains are detected can be used to estimate the speed of the particle in a circular orbit passing through this point.…”

Section: Methodsmentioning

confidence: 99%

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Analogue spectra for impact ionization mass spectra of water ice grains obtained at different impact speeds in space

Klenner

Postberg

Hillier

et al. 2019

Rapid Comm Mass Spectrometry

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Rationale:Detecting ice grains with impact ionization mass spectrometers in space provides information about the compositions of ice grains and their sources.Depending on the impact speeds of the ice grains onto the metal target of a mass spectrometer, ionization conditions can vary substantially, resulting in changes to the appearance of the resulting mass spectra. Methods:Here we accurately reproduce mass spectra of water ice grains, recorded with the Cosmic Dust Analyzer (CDA) on board the Cassini spacecraft at typical impact speeds ranging between 4 km/s to 21 km/s, with a laboratory analogue experiment. In this Laser-Induced Liquid Beam Ion Desorption (LILBID) approach, a μm-sized liquid water beam is irradiated with a pulsed infrared laser, desorbing charged analyte and solvent aggregates and isolated ions, which are subsequently analyzed in a time-of-flight (TOF) mass spectrometer. Results:We show that our analogue experiment can reproduce impact ionization mass spectra of ice grains obtained over a wide range of impact speeds, aiding the quantitative analyses of mass spectra from space. Conclusions:Spectra libraries created with the LILBID experiment will be a vital tool for inferring the composition of ice grains from mass spectra recorded by both past and future impact ionization mass spectrometers (e.g. the SUrface Dust Analyzer (SUDA) onboard NASA's Europa Clipper Mission or detectors on a future Enceladus Mission).

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Section: Discussionmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

Analogue spectra for impact ionization mass spectra of water ice grains obtained at different impact speeds in space

Klenner

Postberg

Hillier

et al. 2019

Rapid Comm Mass Spectrometry

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“…Dust analyzer instruments are capable of measuring time-of-flight (TOF) mass spectra from impact ionized dust particles (e.g., Srama et al, 2005;Sternovsky et al, 2007Sternovsky et al, , 2015. Laboratory experiments showed the relation between the measured mass spectra and the elemental composition of the dust particles, potentially allowing identification of mineralogical information from in situ TOF spectra (e.g., Fiege et al, 2014). At…”

Section: Detectability Of Water In Impact Ejecta Spectramentioning

confidence: 99%

Impact Ejecta and Gardening in the Lunar Polar Regions

et al. 2019

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The Moon is continually bombarded by interplanetary meteoroids. While many of the meteoroid sources are near the ecliptic plane, a significant population of high‐inclination meteoroids exists at 1 au that bombards the lunar polar regions. Building on previous measurements of the response of the lunar impact ejecta cloud to known meteoroid sources, we develop an ejecta model for the entire lunar surface by incorporating the high‐inclination sources. We find that the polar regions of the Moon experience similar quantities of impact ejecta production as the equator. Due to the enhanced impactor fluxes near the equator and at high latitudes on the dawn side, lunar regolith is preferentially distributed to the mid to high‐latitude regions over long timescales, providing a pathway to mix regolith from different regions. We find impact ejecta yields at the Moon to be significantly lower than the Galilean moons, suggesting meteoroids deliver more energy to the local regolith and can be an important driver in the evolution of volatiles near the lunar surface. Additionally, we find that a polar orbiting spacecraft equipped with a dust analyzer can measure appreciable quantities of lunar ejecta near the poles to constrain the water content in the polar regions.

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“…Since the plasma formation, as well as chemical processes, molecule formation and destruction, are determined by physical properties of the plasma plume such as temperatures, densities, collision rates, and the expansion velocity the resulting chemical composition varies with the particle impact or laser conditions, respectively (e.g. Mocker et al, 2012;Fiege et al, 2014).…”

Section: Introductionmentioning

confidence: 99%

Excess of l-alanine in amino acids synthesized in a plasma torch generated by a hypervelocity meteorite impact reproduced in the laboratory

Managadze

Engel

Getty

et al. 2016

Planetary and Space Science

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We present a laboratory reproduction of hypervelocity impacts of a carbon containing meteorite on a mineral substance representative of planetary surfaces. The physical conditions of the resulting impact plasma torch provide favourable conditions for abiogenic synthesis of protein amino acids: We identified glycine and alanine, and in smaller quantities serine, in the produced material. Moreover, we observe breaking of alanine mirror symmetry with L excess, which coincides with the bioorganic world. Therefore the selection of L-amino acids for the formation of proteins for living matter could have been the result from plasma processes occurring during the impact meteorites on the surface. This indicates that the plasma torch from meteorite impacts could play an important role in the formation of biomolecular homochirality. Thus, meteorite impacts possibly were the initial stage of this process and promoted conditions for the emergence of a living matter.

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Calibration of relative sensitivity factors for impact ionization detectors with high-velocity silicate microparticles

Cited by 24 publications

References 30 publications

Analogue spectra for impact ionization mass spectra of water ice grains obtained at different impact speeds in space

Analogue spectra for impact ionization mass spectra of water ice grains obtained at different impact speeds in space

Impact Ejecta and Gardening in the Lunar Polar Regions

Excess of l-alanine in amino acids synthesized in a plasma torch generated by a hypervelocity meteorite impact reproduced in the laboratory

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