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43 results for “regolith”
Water content in the upper 1 meter of the Martian regolith, estimated from FREND experiment data
<p>This dataset contains a raw map of neutron suppression and a smoothed map of water content in the upper meter of the Martian subsurface derived from FREND instrument data, between latitudes 50° north and south. FREND is a high resolution neutron telescope onboard ExoMars’ TGO orbiter (see Mitrofanov, I. et al. Fine Resolution Epithermal Neutron Detector (FREND) Onboard the ExoMars Trace Gas Orbiter. Space Sci Rev 214, 86 (2018). <a href="https://doi.org/10.1007/s11214-018-0522-5">https://doi.org/10.1007/s11214-018-0522-5</a>).</p> <p>Neutron Suppression is defined as ratio between neutron count rate (counts per second) at each pixel and a reference count rate (average count rate over Solis Planum area between -115° and -65° longitude and -55° and -15° latitude). It is a dimensionless parameter, showing how much the neutron flux is suppressed relative to the reference Solis Planum area, known to be one of the driest on Mars with water equivalent hydrogen (WEH) estimated as 2.78 weight percent (wt%, see Boynton, W.V. et al. Concentration of H, Si, Cl, K, Fe, and Th in the low- and mid-latitude regions of Mars. Journal of Geophysical Research 112, (2007) E12S99. <a href="https://doi.org/10.1029/2007JE002887">https://doi.org/10.1029/2007JE002887</a>). Statistical errors are given in each pixel. Map of neutron suppression can be used to locate regions of high or low water content.</p> <p>Map of water is derived from the neutron suppression map in the following way: neutron suppression map is smoothed with a gaussian 12° (full width half maximum) filter, considering statistical errors in each pixel. Transition from smoothed neutron suppression values to WEH values is done through numerical modeling of all physical process from neutron emission from the Martian regolith to detection of neutrons by FREND instrument, depending on the WEH content in the regolith. Map of water contains three values for each pixel: minimum, mean and maximum WEH in wt%: mean values are derived from neutron suppression map, maximum and minimum values correspond to plus and minus error of the neutron suppression. These three values represent the range of WEH in each pixel within 1 error margin of neutron suppression values.</p>
Dataset from "Constraining Martian regolith and vortex parameters from combined seismic and meteorological measurements"
<p>The table provided below (in CSV format) includes derived data obtained from the raw data of the InSight SEIS and APSS experiments. For the raw data, we acknowledge:</p> <p>InSight Mars SEIS Data Service. (2019). SEIS raw data, Insight Mission. IPGP, JPL, CNES, ETHZ, ICL, MPS, ISAE-Supaero, LPG, MFSC. https://doi.org/10.18715/SEIS.INSIGHT.XB_2016</p> <p>The dataset in this table was used to produce Figures 6, 7, 11 and 12 of the following paper:</p> <p>N. Murdoch, A. Spiga, R. Lorenz, R.F. Garcia, C. Perrin, R. Widmer-Schnidrig, S. Rodriguez, N. Compaire, N. H. Warner, D. Mimoun, D. Banfield, P. Lognonné and W.B. Banerdt. Constraining Martian regolith and vortex parameters from combined seismic and meteorological measurements. Journal of Geophysical Research: Planets.</p> <p>The table provides derived vortex parameters of all vortices studied in this paper. The columns of the table contain the following properties of every vortex event: Sol, UTC date and time, Local Mean Solar Time (LMST), Observed pressure deficit <span class="math-tex">\(\Delta P_{obs}\)</span> (determined from the fit to the Ellehoj et al. (2010) model after filtering in the 0.02 - 0.3 Hz frequency band), Observed pressure drop encounter duration <span class="math-tex">\(\tau\)</span> (FWHM determined from the fit to the Ellehoj et al. (2010) model after filtering in the 0.02 - 0.3 Hz frequency band), the Ellehoj et al. (2010) model goodness of fit to the vortex pressure data (after filtering in the 0.02 - 0.3 Hz frequency band), Mean background wind speed <span class="math-tex">\(v\)</span>, Standard deviation of background wind speed <span class="math-tex">\(\sigma_v\)</span>, Maximum radial tilt <span class="math-tex">\(\theta_{obs}\)</span>, Azimuth at maximum radial tilt (i.e. at closest approach) <span class="math-tex">\(\alpha_{obs}\)</span>, Mean miss distance <span class="math-tex">\(x\)</span> (i.e. when <span class="math-tex">\(S = v\)</span>), <span class="math-tex">\(\eta \)</span> (defined as <span class="math-tex">\(E/(1-\nu^2) \)</span>), Mean <span class="math-tex">\(\zeta\)</span> (i.e. when <span class="math-tex">\(S = v\)</span>). For further details about these parameters please see the paper cited above.</p>
Far-Ultraviolet Photometric Characteristics of JSC-1A and LMS-1 Lunar Regolith Simulants: Comparative Investigations with Apollo 10084
<p>The .txt files listed here contain the data used for Figure 3 and Supplemental Figure S3 of the paper titled "Far-Ultraviolet Photometric Characteristics of JSC-1A and LMS-1 Lunar Regolith Simulants: Comparative Investigations with Apollo 10084." The experimentally derived phase curves are contained in the files which have the material name (JSC-1A, LMS-1, or Apollo 10084) followed by the wavelength alone (Lyman-a, 140 nm, 160 nm) in the file name. All files with "Hapke" in the file name are the Hapke photometric model (Hapke, 2012) fitted phase curves for the associated experimental data. Two of the JSC-1A files have either "LT38" or "GT150" included in the file name; these are the sieved grain size category data referenced in S3.</p> <p>Also included are .txt files of the data points used in Figure 4 for the JSC-1A and LMS-1 simulants. These each have "Fig4" in the file name.</p>
Datasets for Morphological and Spectral Characterization of Lunar Regolith Breakdown due to Water Ice
<p>Remote sensing observations of the Moon suggest that the lunar polar regolith environment is affected by several natural processes that may cause the regolith in these regions to become more porous and fine particulate. One of these processes may be the mechanical breakdown of regolith particles through the interaction of water ice and regolith by frost wedging. We present morphological and spectral analyses of high-fidelity lunar regolith simulants LHS-1 (lunar highlands simulant-1) and LMS-1 (lunar mare simulant-1) that have been exposed to varying concentrations of water ice (1, 10, and 30 wt%) over extended periods of time (1, 3, and 6 months) to evaluate the extent at which lunar regolith may be weathered by ice-regolith interactions in the Moon’s polar regions. To characterize changes in regolith particle morphology, we explored grain size and shape parameters with the CILAS ExpertShape suite and characterized the abundance and evolution of clinging fines with scanning electron microscopy (SEM) and energy dispersive x-ray spectroscopy (EDS). Reflectance spectra were taken from 1.0 – 22.5 µm (444.4 - 10,000 cm<sup>-1</sup>) to characterize any differences in spectral features that may occur as a result of regolith breakdown. Both the morphological and spectral investigations display trends that show simulant particle degradation as a function of composition, increasing water concentration, and freezing time. Our study demonstrates that the lunar regolith is susceptible to mechanical breakdown in the presence of water ice and that water ice is likely a contributor to the weathering environment within permanently shadowed regions on the lunar surface.</p> <p>This dataset contains all spectra, SEM images, and ExpertShape images/results used to conduct this work.</p>
Ultrasonic velocity measurements of lunar regolith simulant at low confining pressures with variable ice content
<p>This dataset was created by Christopher Chance Amos during completion of a PhD degree in Space Resources</p><p>at Colorado School of Mines. This data was collected during Spring 2023.</p><p> </p><p>This dataset includes compressional and shear raw collected waveforms as well as interpreted velocities</p><p>from first-break picking. See the README files in subdirectories for explanations of individual files.</p><p> </p><p>The purpose of this dataset is to serve as a foundation and calibration for seismic modeling of the lunar</p><p>near-surface. These models will be used to determine if seismic methods are feasible for characterizing</p><p>the quantity and form of lunar subsurface ice deposits.</p>
Data for Abiotic Origin of Organics in the Martian Regolith
<p>This is the supplemental data for the muscript (submitted): "Abiotic Origin of Organics in the Martian Regolith", and comprises the following: </p> <p><strong>_FTIR hyperspectral map </strong></p> <blockquote> <p><strong>↪</strong> FTIR hyperspectral data [combined into single .xlsx file]</p> <p><strong>↪ </strong>FTIR pixel location map</p> <p><strong>↪ </strong>Raman IFORS fitting results</p> </blockquote> <p><strong>_micro-Raman hyperspectral maps</strong></p> <blockquote> <p><strong>↪ </strong>Raman hyperspectral data [per region]</p> <p><strong>↪ </strong>Raman pixel location map [per region]</p> </blockquote> <p><strong>_microscopy</strong></p> <blockquote> <p><strong>↪ </strong>Reflected Light (RL) image of entire sample</p> <p><strong>↪ </strong>Reflected Light (RL) [per region]</p> </blockquote> <p><strong>_mossbauer results</strong></p> <p><strong>_NanoSIMS</strong></p> <blockquote> <p><strong>↪ </strong>NanoSIMS data [per region]</p> <p><strong>↪ </strong>NanoSIMS data images [per region]</p> <p><strong>↪ </strong>NanoSIMS processed data</p> <p><strong>↪ </strong>NanoSIMS standards</p> </blockquote> <p><strong>_SEM BSE&EDS images</strong></p> <blockquote> <p><strong>↪ </strong>BSE and EDS images [per region]</p> </blockquote> <p> </p> <p><strong>ABSTRACT</strong></p> <p>The martian meteorite Northwest Africa (NWA) 11220 and paired stones (notably NWA 7034) are the only group of meteorites that sample a clastic near-surface lithology from Mars. The stones have been recognized as an impact-reworked lithology subjected to an impact-induced hydrothermal system — comparable to the postulated history of Jezero Crater, currently being explored by the NASA Perseverance rover. By applying Mössbauer spectroscopy in combination with several <em>in situ</em> analytical techniques including Raman spectroscopy, FTIR spectroscopy, and NanoSIMS, we show that aliphatic carbon compounds dominate the inventory of insoluble indigenous carbon compounds within NWA 11220. Disordered carbon — present in ~5 μm heterogeneous masses — is preferentially found within porosity where it adjoins the mineral surface of titano-magnetite. This relationship suggests catalytic surfaces have enabled Fischer–Tropsch (FT) synthesis of hydrocarbons. Our <em>in situ</em> micron-scale analytical study indicates that such methods can successfully determine the origin of organic material and, therefore, differentiate abiotic martian organics that exist in the near-surface martian regolith. The multimodal approach will be a key methodology for searching for traces of past life in future samples returned from Mars.</p> <p> </p>
Regolith-landform map of the Tanami Region, Australia
<p>Images used for mapping and modelling the regolith-landform of the Tanami Region, Australia.</p> <p>Zip file: Temporally mergered Landsat TM; RGB, DS754 and Gozzard ratios (ECW)</p> <p><span><span>Zip file: Relief imagess (PNG, PGW); </span></span><span>Slope images (PNG, PGW); </span><span>TWI images (PNG, PGW); </span><span>Flow accumulation images (PNG, PGW)</span></p>
Regolith-landform map of the Tanami Region, Australia
<p>Figure 10 in "Geochemical pathways defined by predictive regolith-landform models using TanDEM-X data in the Tanami Region, Australia". Mapped and modelled for reproduction at 1:25,000-scale.</p>
Data archive for "Rock abundance on the lunar mare on surfaces of different age: Implications for regolith evolution and thickness"
<p>This is associated data for the study "<strong>Rock abundance on the lunar mare on surfaces of different age: Implications for regolith evolution and thickness </strong>" in GRL.</p> <p>The zipfile FT2014-Dense50kmN-n800mto5km.tif.zip is a raster of neighborhood crater frequencies from Fassett and Thomson 2014 (JGR) that are used for the age information in this paper. </p> <p>The csv file is the extracted rock abundance for every frequency pixel in this dataset. </p> <p>A github software release associated with the paper is also available on <a href="https://zenodo.org/badge/latestdoi/417542233">as a Zenodo software repository</a>, as well as on <a href="https://github.com/cfassett/MareRockAbundances">Github</a>.</p>
Geochemistry and chronology of lunar KREEP-rich regolith breccia meteorite Northwest Africa 4485: Implications for the Imbrium impact event and high alkali suite
<p>The dataset includes chemical composition, chronology, and spectral data of lunar meteorite Northwest Africa 4485 (Table 1 and Table 2, Table S1 to S4) for the manuscript "Geochemistry and chronology of lunar KREEP-rich regolith breccia meteorite Northwest Africa 4485: Implications for the Imbrium impact event and high alkali suite".</p>
Spectral effects of regolith porosity in the mid-IR - Forsteritic olivine
<p>This dataset contains laboratory spectra of olivine in the mid-Infrared (MIR; 5-35 micron) wavelength region as described in Martin et al., 2022. </p> <p>Files are labeled accordingly: mineral_largest particle size_regolith porosity</p> <p>Example: The file labeled OLV1_45_10.txt contains spectra of olivine (OLV1 in the paper), with 20-45 micron particle sizes, has 10% regolith porosity. </p>
Spectral effects of regolith porosity in the Mid-IR - Pyroxene [part 2]
<p>This dataset is one of three that contains laboratory spectra of pyroxene in the mid-Infrared (MIR; 5-35 micron) wavelength region as described in Martin et al., 2023. Specifically, this dataset (part 2) has .txt files of HEN1, HEN2, and AEG spectra.</p> <p>Dataset part 1 (10.5281/zenodo.11398016) contains spectra of ENS, DIOP1, and DIOP2.</p> <p>Dataset part 3 (10.5281/zenodo.11402393) contains spectra of AUG and MXT.</p> <p>Files are labeled accordingly: mineral_largest particle size_regolith porosity</p> <p>Example: The file labeled AEG_45_10.txt contains spectra of aegirine (AEG in the paper), with 20-45 micron particle sizes, has 10% regolith porosity. </p>
Spectral effects of regolith porosity in the Mid-IR - Pyroxene [part 1]
<p>This dataset is one of three that contains laboratory spectra of pyroxene in the mid-Infrared (MIR; 5-35 micron) wavelength region as described in Martin et al., 2023. Specifically, this dataset (part 1) has .txt files of ENS, DIOP1, and DIOP2 spectra.</p> <p>Dataset part 2 (10.5281/zenodo.11402380) contains spectra of HEN1, HEN2, and AEG.</p> <p>Dataset part 3 (10.5281/zenodo.11402393) contains spectra of AUG and MXT.</p> <p>Files are labeled accordingly: mineral_largest particle size_regolith porosity</p> <p>Example: The file labeled DIOP1_45_10.txt contains spectra of diopside (DIOP1 in the paper), with 20-45 micron particle sizes, has 10% regolith porosity. </p>
Spectral effects of regolith porosity in the Mid-IR - Pyroxene [part 3]
<p>This dataset is one of three that contains laboratory spectra of pyroxene in the mid-Infrared (MIR; 5-35 micron) wavelength region as described in Martin et al., 2023. Specifically, this dataset (part 3) has .txt files of AUG and MXT spectra.</p> <p>Dataset part 1 (10.5281/zenodo.11398016) contains spectra of ENS, DIOP1, and DIOP2.</p> <p>Dataset part 2 (10.5281/zenodo.11402380) contains spectra of HEN1, HEN2, and AEG.</p> <p>Files are labeled accordingly: mineral_largest particle size_regolith porosity</p> <p>Example: The file labeled AUG_45_10.txt contains spectra of augite (AUG in the paper), with 20-45 micron particle sizes, has 10% regolith porosity. </p>
Analysis of thermal and dielectric loss features of lunar regolith considering real-time effect solar irradiance
<p>ESI data for "Analysis of thermal and dielectric loss features of lunar regolith considering real-time effect solar irradiance".</p>
Measuring the effects of regolith porosity on mid-IR spectra of the Allende meteorite
<p>This dataset contains three types of data: 1) Mid-Infrared (MIR; 5-35 micron) laboratory spectra of the Allende meteorite, 2) Measured parameters of the MIR Allende spectra, and 3) MIR spectra from the Spitzer Space Telescope of asteroids (85989) 1999 JD6, (234) Barbara, (5261) Eureka, and (114) Kassandra as described in Dausend et al., (in rev). </p> <p>Allende meteorite spectra files are labeled accordingly: Allende_[largest particle size]_[Allende ratio]</p> <p>Example: The file labeled Allende_63_70.txt contains spectra of Allende powder with 45-63 micron particle size, and an Allende:KBr ratio of 70:30.</p> <div>Additional information regarding Allende spectra feature parameters: </div> <div>We combined some features together for band parameter analyses to form ‘composite features’. A composite feature is made of two or more individual features that, together, form a larger spectral feature. In the spreadsheet these features are labeled with a ‘c’ prefix. The composite feature definitions are:</div> <div>cP_1 = P_1-2 (primary Christiansen Feature)</div> <div>cP_2 = P_3-4</div> <div>cP_3 = P_5-7</div> <div>cP_4 = P_3-7 (10 μm feature)</div> <div>cD_1 = D_2-6</div> <div> </div> <div>Corrections: </div> <ul> <li> <div>In the ‘Allende_peak_parameter’ and ‘Allende_dip_parameter’ spreadsheets, the ‘Area’ unit should be labeled as ‘μm’, not ‘μm^2’. </div> </li> </ul> <ul> <li>The last column of the ‘Wavenumbers’ sheet in “Allende_dip_parameters.xlsx” is labeled as ‘cP1 error’, but it should be ‘cD1 error’.</li> </ul>
Solar wind access to grains in the upper layer of regolith
<p>The directory contains the scripts and output files from running COUPI DEM for determining the distribution of protons in upper layer of regolith. This is the model data for the paper "Solar wind access to grains in the upper layer of regolith" accepted to JGR Planets.</p> <p>Each case represents different packing density. The cases are described by Paul Duvoy in file Cases_paul_duvoy.xlsx.</p> <p>Most scripts to extract and process modeled data are located in utils and<br> gnuplot directory.</p> <p> </p>
Comparison of Dielectric Properties and Structure of Lunar Regolith at Chang'e-3 and Chang'e-4 Landing Sites Revealed by Ground Penetrating Radar
<p><strong>Fig 2(d) dataset.</strong> Signal Power profile and after R<sup>2</sup>, R<sup>3</sup>, R<sup>4 </sup>backscatter/spreading correction. The first column is depth in meter, second column is original data, third, forth, fifth column is original data after R<sup>2</sup>, R<sup>3</sup>, R<sup>4</sup> correction,respectively.</p> <p><strong>Fig 3(b) dataset. </strong>The first five days of Lunar penetrating radar (LPR) of CE-4 site with Auto Gain Control (AGC) method. Each column represents a single sample of data.</p> <p><strong>Fig 3(c) dataset. </strong>LPR dataset of CE-4 site using an exponential equation gain function for amplitude compensation. Each column represents a single sample of data.</p>
Mid-Infrared Reflectance and Emissivity Spectra of High Porosity Regoliths
<p>This dataset contains laboratory spectra of olivine and pyroxene in the mid-Infrared (MIR; 5-35 micron) wavelength region as described in Martin et al., (in rev). </p> <p>Files are labeled accordingly: mineral_smallest particle size_largest particle size_regolith porosity_measurement type</p> <p>OLV = olivine, PYX=pyroxene</p> <p>r = ambient reflectance, a = ambient emissivity, sae = simulated asteroid environment</p> <p>Example: The file labeled OLV_45_63_10_a.txt contains spectra of olivine, with 45-63 micron particle sizes, has 10% regolith porosity, and was measured in ambient emissivity. </p>
Production and evolution of granitic regolith under cold temperate climate in northeast China: a perspective from 238U-234U-230Th disequilibrium
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