Space weathering simulation of micrometeorite bombardment on silicates and their mixture for space application

Weber, I.; Böttger, Ute; Hanke, Franziska; Reitze, Max P.; Heeger, Marcel; Adolphs, Thorsten; Arlinghaus, Heinrich F.

doi:10.1002/jrs.6162

Cited by 6 publications

(18 citation statements)

References 30 publications

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“…After laser irradiation, the wavenumber, shape, and FWHM of the doublet peaks did not change substantially (Table A.3). The newly formed np-Fe 0 particles are pure metallic iron that have no Raman effects, and the potential reduction of the fluorescence-dominated background due to the formation of np-Fe 0 may facilitate a better interpretation of the individual mineral peaks by the Raman spectrometer (Weber et al 2021(Weber et al , 2022. Amorphization of the olivine surface may cause local disorder and result in the broadening of Raman peaks, as suggested in previous studies (Rouquette et al 2008;Santamaria-Perez et al 2016); however, the amorphous layer showed no substantial influence in our experiments.…”

Section: Raman Spectral Characteristics Of Altered Olivinementioning

confidence: 99%

Space weathering effects and potential spectral alteration on Phobos and the Moon: Clues from the Fe content of olivine

et al. 2023

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Context. Olivine responds to space weathering in the fastest and most profound way, which results in significant space weathering spectral alteration effects (SWSAEs) on airless silicate bodies. Although Mg-rich olivine (Fa10) has been subjected to extensive studies, SWSAEs of Fe-rich (Fa# > 20) or Fa-dominant (Fa# ⩾ 50) olivine are still poorly understood. Aims. We aim to systematically characterize the space weathering effects and the associated spectral alterations of Fe-rich olivine on the surface of Phobos and the Moon. Methods. We conducted nanosecond pulsed laser irradiation experiments on a set of synthetic Fe-rich olivine (Fa29, Fa50, Fa71, and Fa100) with energy levels simulated for Phobos and the Moon and analyzed the irradiated olivine for microscopic characteristics and near-infrared (NIR) and Raman spectroscopy. Results. Micron-level thick alteration layers are found in Fa100 compared to those hundreds of nanometers thick in Fa29, Fa50, and Fa71. With increasing irradiation energy levels and Fa# values, nanophase iron (np-Fe0) particles increase in size but decrease in quantity. The np-Fe0 formed via in situ decomposition are ubiquitously present, while those formed via vapor deposition are primarily found in Fa29 but rarely in Fa# ⩾ 50. The size fraction of intermediate (10–40 nm) and large (40–60 nm) np-Fe0 proportionally increases with Fa# values. The NIR spectra of weathered olivine show darkening over reddening in most cases, but Fa100 under the most irradiated condition shows brightening-reddening spectral effects. The Raman spectra of weathered olivine show a reduction in intensity without peak shifts. Conclusions. The Fa# values of olivine are a more critical factor in controlling the SWSAEs on Phobos than those on the Moon. If Phobos and Deimos contain substantial Fe-rich or Fa-dominant olivine, similar to Mars, thick alteration rims and large np-Fe0 formed via space weathering may cause darkening-reddening and potentially brightening-reddening spectral effects on the Martian moons.

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Section: Raman Spectral Characteristics Of Altered Olivinementioning

confidence: 99%

Space weathering effects and potential spectral alteration on Phobos and the Moon: Clues from the Fe content of olivine

et al. 2023

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“…As it has been mentioned before, the development of the science for the preparation of the mentioned missions is a hard but very important task. In this sense, Weber et al [ 6 ] emphasized that missions to planetary bodies require innovative techniques for the in situ investigation of their surfaces, especially when landings are planned, and state that Raman spectroscopy as an excellent laboratory tool for rapid mineralogical analysis of both terrestrial and extraterrestrial rocks. However, when preparing such space missions, it is essential to be prepared for all possible outcomes, such as samples exhibiting space weathering (SW).…”

Section: The Importance Of Mars and Space Exploration By Raman Spectr...mentioning

confidence: 99%

GeoRaman

Castro

Ling

2022

J Raman Spectroscopy

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was the 14th edition of the international biennial meeting devoted to the application of Raman spectroscopy to mineralogy, geology and earth sciences in broad sense. However, this edition was marked by the COVID19 pandemic. Initially, it should have been held in spring in Weihai (China), but the circumstances, with a worldwide confinement and strong travel restrictions, in what was the first wave of the pandemic focused on Asia, led to the hard decision to be made to move the meeting to Bilbao (Spain) and hold the conference in the fall. Unfortunately, the successive waves of the pandemic and the global uncertainty prevented the formal celebration of said meeting.Far from being discouraged, it was decided to keep the spirit of GeoRaman open a call for abstracts and publish a book of abstracts after the pertinent scrutiny of the scientific committee. The 2020 edition of the conference gathered around 90 research works. GeoRaman 2020 focused on topics, which can be summarized as follows:1. Mineralogy, gemmology and provenance studies 2. Planetary analysis and space exploration 3. Astrobiology and biomineralization 4. Petrology, field and experimental volcanology 5. Geothermobarometry and fluid geochemistry 6. Carbonaceous materials 7. Cultural heritage and archaeometry This special issue of the Journal of Raman Spectroscopy is dedicated to the 14th International GeoRaman Conference and comprises 27 papers covering some of the topics listed above.

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“…13,14 PL is generally expected to be inherent for various planetary surfaces and can be affected at those with dilute atmospheres, that is, strong space weathering. 15 Different spectroscopic techniques were explored in order to suppress PL in Raman spectra; see for detailed description the review 16 : time-resolved, shifted excitation wavelength difference, surface enhanced, photobleaching, and many other techniques. All these approaches have their critical limitations and are addressed to an attempt to resolve RS at the presence of strong PL rather than to avoid PL excitation/detection.…”

Section: Introductionmentioning

confidence: 99%

“…PL has a pure electronic nature, resulting from radiative transitions between electronic states, representing both a material matrix and also abundant impurities; some of those are strong luminescent centers: for instance, ions of transition metals or rare earth elements 13,14 . PL is generally expected to be inherent for various planetary surfaces and can be affected at those with dilute atmospheres, that is, strong space weathering 15 . Different spectroscopic techniques were explored in order to suppress PL in Raman spectra; see for detailed description the review 16 : time‐resolved, shifted excitation wavelength difference, surface enhanced, photobleaching, and many other techniques.…”

Section: Introductionmentioning

confidence: 99%

Comparative Raman spectroscopy of astrobiology relevant bio‐samples and planetary surface analogs under UV–VIS–IR excitation

Hanke,

Böttger,

Pohl

et al. 2023

J Raman Spectroscopy

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We investigated the potential of a laser selection in the broad optical range, from ultraviolet through visible to infrared (excitation wavelengths of 325, 532, 785, and 1064 nm) for combined analysis of Earth‐relevant extremophiles (Xanthoria elegans, Buellia frigida, and green alga of Circinaria gyrosa), carbohydrate molecules, as well as Mars and Moon surface regolith simulants as analog mineral mixtures (P‐MRS, S‐MRS, LRS, and JSC‐1). We show that the optimization of the laser photon energy provides (for at least one of the chosen excitation wavelengths) high‐end quality Raman spectra for each examined sample. In most cases, the infrared spectral range is advanced for biological samples, while an excitation in the visible and ultraviolet spectral range is often favorable or at least sufficient for accurate identification/resolution of mineral phases under the illuminated laser spot on the planetary surface simulants. Ultraviolet excitation does not always deliver significant contrast of the Raman Stokes responses to the induced photoluminescence in the studied biomolecules. Most prominent features in the Raman spectra of the biological samples are assigned to their specific pigments, also considered as biomolecular signatures of the extremophiles. The critical issue of specific advantages and limitations of each particular excitation source implies study for gaining scientific return from Raman spectroscopy for exobiological prospecting, for instance, the best trade between a single or dual excitation wavelength(s) for both biological and geological spectral data.

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Space weathering simulation of micrometeorite bombardment on silicates and their mixture for space application

Cited by 6 publications

References 30 publications

Space weathering effects and potential spectral alteration on Phobos and the Moon: Clues from the Fe content of olivine

Space weathering effects and potential spectral alteration on Phobos and the Moon: Clues from the Fe content of olivine

GeoRaman

Comparative Raman spectroscopy of astrobiology relevant bio‐samples and planetary surface analogs under UV–VIS–IR excitation

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