Anorthite sputtering by H+ and Arq+ (q = 1–9) at solar wind velocities

Hijazi, Hussein; Bannister, M. E.; Meyer, Harry M.; Rouleau, Christopher M.; Barghouty, A. F.; Rickman, Doug; Meyer, F. W.

doi:10.1002/2014ja020140

Cited by 14 publications

(25 citation statements)

References 28 publications

(54 reference statements)

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“…Furthermore, a static surface composition is often assumed even though it is known that composition changes as a function of irradiation fluence. However, experiments at solar wind energies (∼1 keV/amu) have been carried out giving the total sputtering yields for several simple oxides (Hijazi et al, 2014;Roth et al, 1979) as well as the relative secondary ion yields from a small number of Apollo lunar soils (Dukes & Baragiola, 2015;Schaible, 2014) and soil simulants (Elphic et al, 1991;Meyer et al, 2011), thus allowing for some comparison with computational results.…”

Section: Solar Wind Sputteringmentioning

confidence: 99%

Solar Wind Sputtering Rates of Small Bodies and Ion Mass Spectrometry Detection of Secondary Ions

et al. 2017

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Solar wind interactions with the surfaces of asteroids and small moons eject atoms and molecules from the uppermost several nanometers of regolith grains through a process called sputtering. A small fraction of the sputtered species, called secondary ions, leave the surface in an ionized state, and these are diagnostic of the surface composition. Detection of secondary ions using ion mass spectrometry (IMS) provides a powerful method of analysis due to low backgrounds and high instrument sensitivities. However, the sputtered secondary ion yield and the atomic composition of the surface are not 1‐to‐1 correlated. Thus, relative yield fractions based on experimental measurements are needed to convert measured spectra to surface composition. Here available experimental results are combined with computationally derived solar wind sputtering yields to estimate secondary ion fluxes from asteroid‐sized bodies in the solar system. The Monte Carlo simulation code SDTrimSP is used to estimate the total sputtering yield due to solar wind ion bombardment for a diverse suite of meteorite and lunar soil compositions. Experimentally measured relative secondary ion yields are analyzed to determine the abundance of refractory species (Mg+, Al+, Ca+, and Fe+) relative to Si+, and it is shown that relative abundances indicate whether a body is primitive or has undergone significant geologic reprocessing. Finally, estimates of the sputtered secondary ion fluxes are used to determine the IMS sensitivity required to adequately resolve major element ratios for nominal orbital geometries.

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Section: Solar Wind Sputteringmentioning

confidence: 99%

Solar Wind Sputtering Rates of Small Bodies and Ion Mass Spectrometry Detection of Secondary Ions

et al. 2017

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“…TRIM provides the total sputter yield for a species and does not specify the fraction of ions in the sputtered flux. TRIM has been used for decades to simulate sputtering and related phenomena and gives good quantitative results on sputter yields, even for samples with relevance to planetology (e.g., Hijazi et al 2014). Table 1 lists the calculated relative sputter yields for mineral grains for the species of interest for solar wind speeds of 440 km s −1 and assuming 95% protons and 5% alpha particles.…”

Section: Solar Wind Sputteringmentioning

confidence: 99%

Solar wind sputtering of dust on the surface of 67P/Churyumov-Gerasimenko

Würz

Rubin

Altwegg

et al. 2015

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Aims. Far away from the Sun, at around 3 AU, the activity of comet 67P/Churyumov-Gerasimenko is low and changes with local time (solar insolation), with location (chemical heterogeneity of the surface), and with season. When the activity is very low because the total cross section of the comet against the Sun is small, the solar wind has access to the surface of the comet and causes ion-induced sputtering of surface material, which we wish to observe. Methods. We used the Double Focussing Mass Spectrometer (DFMS) of the ROSINA experiment on ESA's Rosetta mission to search for mass spectrometric evidence of sputtered refractory species. In high-resolution mode, DFMS can separate some of the mass peaks of refractory elements from the many volatile species present in the coma. Results. At present, the locations of solar wind surface access are in the southern hemisphere of the comet (the local winter). Of particular interest is sputtering of dust grains on the surface. We observe global averages over the winter hemisphere of the refractory elements Na, K, Si, and Ca, presumably sputtered from grains residing on the surface. Compared to carbonaceous chondrites, the comet has the same Na abundance, is depleted in Ca, and has an excess of K. In addition, for Si the signal strength is strong enough to compile a coarse compositional map of the southern hemisphere. Most, perhaps all, of the observed variation can be explained by the solar wind being affected by the atmosphere of the comet.

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“…A similar increase due to potential sputtering by the multicharged solar wind species, based on measurements of absolute sputtering yields for multicharged Ar ions impacting anorthite, using a quartz crystal microbalance (QCM), was reported in Hijazi et al . []. In the latter publication, the dependence of potential sputtering on the multicharged Ar ion's neutralization potential energy was directly determined, which permitted an improved estimation of the potential sputtering contributions of the remaining multicharged solar wind ions.…”

Section: Introductionmentioning

confidence: 99%

“…The reported He +q ion yields, together with a reanalysis of the low charge state Ar +q sputtering yields reported in Hijazi et al . [] are used to obtain a revised scaling of the potential sputtering yield with neutralization potential energy, which is subsequently used in the analysis of section 3.…”

Section: Introductionmentioning

confidence: 99%

Kinetic and potential sputtering of an anorthite‐like glassy thin film

et al. 2017

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In this paper, we present measurements of He+ and He+2 ion‐induced sputtering of an anorthite‐like thin film at a fixed solar wind‐relevant impact energy of ~0.5 keV/amu using a quartz crystal microbalance approach (QCM) for determination of total absolute sputtering yields. He+2 ions are the most abundant multicharged ions in the solar wind, and increased sputtering by these ions in comparison to equivelocity He+ ions is expected to have the biggest effect on the overall sputtering efficiency of solar wind impact on the Moon. Our measurements indicate an almost 70% increase of the sputtering yield for doubly charged incident He ions compared to that for same velocity He+ impact (14.6 amu/ion for He+2 vs. 8.7 amu/ion for He+). Using a selective sputtering model, the new QCM results presented here, together with previously published results for Ar+q ions and SRIM results for the relevant kinetic‐sputtering yields, the effect due to multicharged‐solar‐wind‐ion impact on local near‐surface modification of lunar anorthite‐like soil is explored. It is shown that the multicharged‐solar‐wind component leads to a more pronounced and significant differentiation of depleted and enriched surface elements as well as a shortening of the timescale over which such surface‐compositional modifications might occur in astrophysical settings. In addition, to validate previous and future determinations of multicharged‐ion‐induced sputtering enhancement for those cases where the QCM approach cannot be used, relative quadrupole mass spectrometry (QMS)‐based measurements are presented for the same anorthite‐like thin film as were investigated by QCM, and their suitability and limitations for charge state‐enhanced yield measurements are discussed.

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Anorthite sputtering by H⁺ and Ar^q+ (q = 1–9) at solar wind velocities

Cited by 14 publications

References 28 publications

Solar Wind Sputtering Rates of Small Bodies and Ion Mass Spectrometry Detection of Secondary Ions

Solar Wind Sputtering Rates of Small Bodies and Ion Mass Spectrometry Detection of Secondary Ions

Solar wind sputtering of dust on the surface of 67P/Churyumov-Gerasimenko

Kinetic and potential sputtering of an anorthite‐like glassy thin film

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