Dept., Univ. of ela as are, 'i?ewark, DE Approximately 130 low specific gravity ((2.601, high silica
|
|
- Easter Hawkins
- 6 years ago
- Views:
Transcription
1 HIGH (760%) SiO LUNAR GLASS%. ir.f. Glass, Geoloey Dept., Univ. of ela as are, 'i?ewark, DE Approximately 130 low specific gravity ((2.601, high silica p602) glass particles recovered from a 4.88 gm sample of lunar fines (14259,20) using heavy liquids.?he major element compositions of-90 of the high silica glass particles were determined by electron microprobe analyses. Silica contents range from-60% to nearly 100%. Approximately 70 of the particles were homogeneous. Histograms and oxide variation diagrams were used to divide the homogeneous glasses into several groups (Table 1). Pifty-seven (-81%) of the homogeneous glasses fall into a group with SiO content ranging between 72 and 78%. The rest have somewhat gigher or lower silica ccntents (groups A, B and Y,?able I), and generally do not contain vesicles or crystalline inclusions. The glasses with silica contents between 72 and 78% fall into three well-defined groups based on their FeO contents. The glasses in the largest group (group E) have FeO contents clustering around 2.65%. The glasses in this group do not contain vesicles or crystalline inclusions. The glasses in the second largest group (group C) have FeO contents clustering around 0.5%. The third group (group D) contains glasses with intermediate Fee contents (1 to %). The group C and D glasses, in contrast to the group E glasses, contain abundant crystalline inclusions. The crystalline phases identified are, in order of their abundance t pyroxene, Si02, Ili-F e, apatite, ilmenite, K- feldspar, plagioclase, metallic iron and troilite. The range and modal composition of the glasses reported here are similar to those previously reported for high silica glasses from lunar fines. Two possible origins of the high silica glasses seem most reasonable8 1) they are fragments of interstitial or residual glass from mare basalts; or 2) they are impact-produced glasses from a "graniticw source rock. liumerous authors have reported the presence of high silica interstitial or residual glass up to 150 across in the mare basalts, The size, shape, abundance, mineralogy and major element composition of the glasses (except those of group E) reported here are consistent with their being fragments of interstitial glass from mare basalts. The fact that high silica glass fragments have not been reported in Apollo 16 (highland) soils also supports their being fragments of interstitial glass from mare basalts.?he group E glasses also have major element compositions similar to the high silica interstitial glasses found in mare basalts. However, they seem to have slightly higher Na20 ( %) and slightly lower Cab ( %) contents than interstitial glasses with the same Si02 and FeO contents, which generally have less than 1% Na20and often have more than 1.5% CaO.
2 High Si02 Lunar Glasses B.P. Glass '?he lack of crystalline inclusions in the group E glasses also suggests that they are not fragments oe interstitial glass. It 1s tempting, therefore, to suggest that these glass particles were derived by shock melting from a "graniticv source rock. However, there are two problems with such an origin. First of all, the group E glasses do not contain any shocked crystalline inclusions or Ni-f e spherules of meteoritic composition that would support such an origin. Secondly, all of the group E glasses are fragments; none are splash forms (spheres, teardrops, dumbbells, etc.). An alternative origin is that these glasses are the products of lunar acidic volcanism. This hypothesis is supported by their homogeneity not only within a single particle, but from particle to particle. I Table 1. Average Composition of High Silica Glass Groups S i02 T i0 A1 a, F e8 MgO C a0 Na2C K2 R.I. Analysis #72 f Range Ave. Group A Group B Group C (3) (2) (18) Group D Group E Group F Analys is (10) (30) (2) #80 * S i G 'l ic z ~l , F e big 0 0, CaO PJa K R.I (4) (15) (2) Ave e ( ) = number of analyses f Homogeneous glass particle with lowest Si02 content. - + = one stand.ard deviation * The only high silica spherule found.
3 ELECTRICAL PROPERTIES OF APOLLO 17 ROCK AND SOIL SAMPLES AND A SUMMARY OF THE ELECTRICAL PROPERTIES OF LUNAR MATERIAL AT 450 MHz FREQUENCY. T. Gold, E. Bilson and R. L. Baron, Center for Radiophysics and Space Res., Cornell University, Ithaca, N.Y., Figure 1 shows the average dielectric constant vs. density Rayleigh curve for Apollo 17 soil samples-4 samples from different locations, including the orange soil, and data points for two Apollo 17 rock samples. This curve lies very close to the Apollo 11 and 12 curve, see Figure 2, which is included for comparison. The data points for the solid samples seem to be approximately on the extension to higher density of the powder Rayleigh curve. This is interesting because the Apollo 17 dust and rock samples display a great variety of chemical composition but for each rock type there is a corresponding dust type. This was not the case for example with the Apollo 11 and 12 samples and data points for the solid rocks did not fit the Rayleigh curve for dust. Figure 3 shows the voltage absorption vs. density Rayleigh curves for Apollo 17 soil samples and data points for the rock samples. Again the solid data points lie close to the extension of Rayleigh curves representing dust of similar chemical composition as the rock. (Actually soil sample and rock sample are not as close mineralogically as indicated by the absorption curve ) Rock is an example of a very lossy solid material whereas the absorption in is less than in any terrestrial rock examined (1). Figure 4 shows, for comparison, voltage absorption vs. density Rayleigh curves for Apollo 11, 12, 14, 15 and 16 samples. The Apollo 17 samples display a greater range of absorbency than samples from any other Apollo missions. In Figure 5 absorption lengths, measured in rock samples from all the Apollo missions, are shown as a function of the iron + titanium concentration in these samples. The density of each rock sample is - 3 indicated in parenthesis, the density range being g cm. At these densities the absorption length vs. density curve is rather flat, so that a small change in density does not effect the absorption significantly. The absorption length in rocks seems to be clearly related to the iron+titanium content. A similar finding was reported by Olhoeft and Strangway (2). Figure 6 relates the albedo (which in turn was also related to the Fe + Ti content (3)) and the absorption length in soil samples. Again a clear correlation seems to exist. Samples and are somewhat outstanding. It is very interesting that in the albedo vs. surface (Fe + Ti) concentration curve and are also outstanding(3). These samples have probablyahigh albedo because they contain a few percent of very
4 ELECTRICAL PROPERTIES... T. Gold et al. light, iron poor material. Olhoeft et a1 (4) demonstrated the effects of short- and long- period exposure of lunar dust samples to moisture, particularly significant was the short-term exposure effect on the absorption properties. Our samples were baked at 150 C in high vacuum for two days prior to the measurement (made in air). It is possible though that short-term exposure effects altered our results, the magnitude of these effects at high frequencies has not been determined yet. However our results show no clustering of data obtained with samples from the early missions (Apollo 11, 12, 14) vs. data representing samples from later missions, thus we see no obvious long-term exposure effects due to sample handling. The high absorption in Apollo 11 and 12 samples seem to be related to the low albedo (high Fe + Ti content) in these samples and similarly high absorption is found in a low albedo Apollo 17 dust sample. In summary: absorption lengths of wavelengths at 1.6 gati3 density are not unusual on the Moon for compacted powders and the absorption range in lunar rocks is wavelengths at 450 MHz frequency. In terrestrial samples the absorption length range at 450 MHz is wavelengths (1). The existence of these great absorption lengths on the Moon is very important for the interpretation of radar results. In the future perhaps depths of several kilometers in the lunar surface could be investigated by suitable radar systems. References: (1) Campbell, M.J., and Ulrichs, J., 1969, Journal of Geophys. Res., 74, p (2) Olhoeft, G.R., and Strangway, D.W., 1975, Earth and Planetary Science Letters, 24, p (3) Gold, T., Bilson, E., And Baron, R.L., 1976, The Correlation Between the Albedo and the Surface Chemical Composition in Lunar Soil Samples in "Lunar Science VII", The Lunar Science Institute, Houston. (4) Olhoeft, G.R., Strangway, D.W., and Pearce, G.W., 1975, Proc. Lunar. Sci. Conf. 6th, p Figure 1. Figure 2.
5 ELECTRICAL PROPERTIES... T. Gold et al. Figure 3. Figure ,7w1 1207c The A~SD~P~IM Length is the Colculoled Volue far 12 g ~ r n Densty - ~ Figure 5. Figure 6.
6 THE CORRELATION BETWEEN THE ALBEDO AND THE SURFACE CHEMICAL COMPOSITION IN LUNAR SOIL SAMPLES. T. Gold, E. Bilson, and R. L. Baron, Center for Radiophysics and Space Res., Cornell University, Ithaca, N.Y., The correlation of the albedo and the iron + titanium concentration in numerous ground-up lunar rock and soil samples from all the Apollo landing sites has been investigated in detail. In Figure 1 the data points (with the exception of that of the iron poor, very high albedo soil samples 73241, 67601,.63501) are fitted to the exponential law: A=A e -na where A is the observed albedo, A. is the hypothetical aybedo at n=o (the law does not seem to be valid for soil samples at very low n values), n is the iron + titanium concentration (surface or bulk) observed and o is the absorption coefficient. The concentration error bars indicate the Auger concentration.extremes obtained with taking spectra on various spots of the same sample, the albedo error Qars refer to the lowest and highest albedo mea- sured at 5500A wavelength at 8' illumination angle and was normalized at MgO. There seems to be three distinct curves. 1. Albedo of soil samples vs. bulk iron + titanium concentration (the latter obtained from the literature). 2. Albedo of soil samples vs. surface iron + titanium concentration (determined by Auger electron spectroscopy) (1, 3). 3. Albedo of ground-up rock samples vs. surface (approximately same as the bulk) iron + titanium concentration. In our first publication on this subject (1) we includ-ed similar curves but the albedo was plotted as a function of iron concentration alone. Recently we have analyzed titanium rich rock and soil samples from the Apollo 11 and 17 missions and discovered that the data fits the exponential law best when n includes both the iron and titanium concentrations. This is to be expected on the basis that both iron and titanium provide absorption centers. From these curves the following deductions can be made: a. The albedo of the soil samples is approximately three times lower than that of ground-up rock samples having the same bulk iron + titanium concentration, see curves 1 and 3. At the same time the soil samples have higher (2-3times) iron + titanium concentration on their surface than bulk concentration in these elements, see curves 1 and 2. The soil therefore must have suffered a treatment that affected both the albedo and the surface iron and titanium. b. The fact that curves 2 and 3 are clearly separate suggests that a different mechanism must be responsible for light absorption on the surface of soil samples and on the surface of freshly ground-up rock samples. Our Auger results and recent ESCA information (2) suggest
7 ALBEDO AND SURFACE CHEMISTRY CORRELATION. T. Gold et al. that at least some of the iron and titanium is reduced on the surface of soil grains to a lower oxidation state than their state in the bulk. In the case of iron this is the metallic state. Research is under progress for the determination of the thickness of the chemically altered skin on soil grains and its optical significance. The possibility exists that the above skin proves to be too thin to be optically significant and the increased light absorption in soil samples is due to a crystallographic change in the lattice. This change then seemingly goes in step with a chemical change on the outer surface and is very probably due to the same weathering agent. We reported recently (3) on solar wind simulation experiments with 2 kev protons. A dose of protons, equivalent to a few thousand years of solar wind rendered the Auger spectrum of an Apollo 14 ground-up rock sample identical (within experimental uncertainty) to that of the Apollo 14 soil of the same bulk composition. The principal change induced by the ion bombardment was the increased iron concentration on the surface of the rock powder. The albedo of the powder decreased however only slightly by the above dose. Since then we repeated the above experiment with 2 kev a-particles using much higher irradiation doses. We found that an approximate equivalent of 25,000 years of solar wind was needed to darken the ground-up rock to the albedo of the soil. At this stage we suppose that this much higher dose, necessary to darken the rock to lunar soil albedo, corresponds to the dose needed to alter the chemistry down to a thick enough layer on the grains to cause the required optical effect. Comparison and correlation of the surface and bulk concentrations of different elements is important for the understanding of the origin and the formation mechanism of the chemically altered skin on soil grains (3). Previously we reported data on the Fe, Ti and Ca concentrations calculated from Auger Fe/O, Ti/O and Ca/O data (3). With the help of recent improvements on our Auger system we have preliminary results on Si concentrations. Sample \- 1 rock zoil Si (surface) in atomic percent Si (bulk) in atomic percent The above data indicate no systematic change of the surface Si concentration from the bulk Si concentration in soil samples. Housley and Grant (2) reported somewhat different findings concerning Si on one sample using ESCA. Clearly more data is needed for good statistical significance. It is very likely however
8 ALBEDO AND SURFACE CHEMISTRY CORRELATION. T. Gold et al. that the concentration of Ca and that of all the other elements lighter than Ca is decreased on the surface whereas the concentration of Fe and Ti is increased. The mass dependence of the chemical change on the surface can be most readily explained by a sputtering process by solar wind ions. References: (1) Gold, T., Bilson, E., and Baron, R.L., 1974, Proc. Lunar Sci. Conf. 5th, p (2) Housley, R.M., and Grant, R.W., 1975, Proc. Lunar Sci. Conf. 6th, p (3) Gold, T., Bilson, E., and Baron, R.L., Sci. Conf. 6th, p , Proc. Lunar L l l i i l l l,, l l ( 1, 1 1, 1, IS 19 Alomfc Percent (Fe+ TI ) Figure 1
The Surprising Lunar Maria
1 of 5 posted June 23, 2000 The Surprising Lunar Maria Written by G. Jeffrey Taylor Hawai'i Institute of Geophysics and Planetology The lunar maria, the dark, smooth areas on the Moon, formed when lava
More informationUV-V-NIR Reflectance Spectroscopy
UV-V-NIR Reflectance Spectroscopy Methods and Results A. Nathues Naturally-occurring inorganic substances with a definite and predictable chemical composition and physical properties Major groups: Silicates
More informationComposition of the Moon's Crust
1 of 7 posted December 10, 2004 Composition of the Moon's Crust --- New empirical calibrations of Lunar Prospector and Clementine data yield improved global maps of Th, K, and FeO. The movie of the Moon,
More informationLunar Glossary. Note to the User: Glossary
Lunar Glossary Note to the User: A number of terms are unique to lunar science or are at least used in a specialized sense. The following brief glossary is an attempt to define these unique terms plus
More informationIron and Titanium: Important Elements. posted October 20, References:
1 of 6 posted October 20, 1997 Moonbeams and Elements Written by G. Jeffrey Taylor Hawai'i Institute of Geophysics and Planetology To determine how a planetary body formed and evolved, we must determine
More informationStatistical Analysis of the Links among Lunar Mare Soil Mineralogy, Chemistry, and Reflectance Spectra
Icarus 155, 285 298 (2002) doi:10.1006/icar.2001.6749, available online at http://www.idealibrary.com on Statistical Analysis of the Links among Lunar Mare Soil Mineralogy, Chemistry, and Reflectance Spectra
More informationESR APPLICATIONS TO METEORITE SAMPLES. Chihiro y AMANAKA, Shin TOYODA and Motoji IKEY A
Proc. NIPR Symp. Antarct. Meteorites, 6, 417-422, 1993 ESR APPLICATIONS TO METEORITE SAMPLES Chihiro y AMANAKA, Shin TOYODA and Motoji IKEY A Osaka University, Department of Earth and Space Science, J
More informationhttp://eps.mcgill.ca/~courses/c201_winter/ http://eps.mcgill.ca/~courses/c201_winter/ Neutron Proton Nucleosynthesis neutron!! electron!+!proton!!=!!é!!+!h +!! t 1/2 =!12!minutes H + +!neutron!! Deuterium!(D)
More informationAstronomy 101 The Solar System Tuesday, Thursday 2:30-3:45 pm Hasbrouck 20. Tom Burbine
Astronomy 101 The Solar System Tuesday, Thursday 2:30-3:45 pm Hasbrouck 20 Tom Burbine tomburbine@astro.umass.edu Course Course Website: http://blogs.umass.edu/astron101-tburbine/ Textbook: Pathways to
More informationSupplementary Figure 1 Panoramic view of four sites (CE-0005, CE-0006, CE-0007, and CE-0008) measured by APXS and VNIS. Images (a), (b), and (d) were
Supplementary Figure 1 Panoramic view of four sites (CE-0005, CE-0006, CE-0007, and CE-0008) measured by APXS and VNIS. Images (a), (b), and (d) were acquired by the Panoramic Camera at the CE3-0007 site,
More informationSilicate Atmospheres, Clouds, and Fractional Vaporization of Hot Earth-like Exoplanets
Silicate Atmospheres, Clouds, and Fractional Vaporization of Hot Earth-like Exoplanets Laura Schaefer and Bruce Fegley, Jr. Planetary Chemistry Laboratory Department of Earth and Planetary Sciences Washington
More informationEPMA IMAGES. Figure 9. Energy-dispersive spectra of spot mineral analyses in sample 89GGR-33A for locations 1-5 in Figure 8.
EPMA IMAGES The attached images and mineral data can be used to supplement an instrument-based lab, or serve as the basis for lab that can be completed without an instrument. Please provide credit for
More informationMössbauer mineralogy on the Moon: The lunar regolith
Hyperfine Interactions 117 (1998) 405 432 405 Mössbauer mineralogy on the Moon: The lunar regolith Richard V. Morris a,göstar Klingelhöfer b, Randy L. Korotev c and Tad D. Shelfer d a Code SN3 NASA Johnson
More informationGeos 306, Mineralogy Final Exam, Dec 12, pts
Name: Geos 306, Mineralogy Final Exam, Dec 12, 2014 200 pts 1. (9 pts) What are the 4 most abundant elements found in the Earth and what are their atomic abundances? Create a reasonable hypothetical charge-balanced
More informationOrigin of Earth's moon Short Course Notes
Origin of Earth's moon Short Course Notes I gave this short course several times to groups of high school earth science teachers, 1994-1998. The information herein was derived from many sources, some of
More informationThe Moon: Internal Structure & Magma Ocean
The Moon: Internal Structure & Magma Ocean 1 Lunar Magma Ocean & Lunar Interior 2 Two possible views of the Moon s interior: The Moon: Internal Structure 3 Like Earth, the Moon is a differentiated body.
More informationSignature: GEOLOGICAL SCIENCES 0050
GEOLOGICAL SCIENCES 0050 I am aware of the Brown University Honor Code [see the Student Handbook, which can be accessed through the Geo0050 web site], understand that this exercise falls under that code,
More informationEFFECTS OF LASER SPACE WEATHERING ON DERIVED IRON OXIDE CONTENT IN SAN CARLOS OLIVINE, PYROXENE, AND ANORTHOSITE
EFFECTS OF LASER SPACE WEATHERING ON DERIVED IRON OXIDE CONTENT IN SAN CARLOS OLIVINE, PYROXENE, AND ANORTHOSITE Logan K. Magad-Weiss Department of Geology and Geophysics University of Hawai`i at Mānoa
More informationMoon Formation. Capture Hypothesis Many Hypothesis Fission Hypothesis Double Impact Hypothesis Giant Impact Hypothesis
Moon Formation Capture Hypothesis Many Hypothesis Fission Hypothesis Double Impact Hypothesis Giant Impact Hypothesis Capture Hypothesis Earth seized a pre-formed moon Disproved when lunar samples showed
More informationAgenda. Chapter 7. The Earth s Moon. The Moon. Surface Features. Magnificent Desolation. The Moon
Chapter 7 The 1 Agenda Announce: Project Part II due Tue No class next Thursday...Tgiving break! No class 12/14 (last day) Spectral Lines Lab due Pass Back Test 2 Discuss grades NYT article on gamma ray
More informationDRAFT Coarse-fines 569 grams
10085 Coarse-fines 569 grams DRAFT Figure 1: Selected coarse fines from 10085. Scale is in mm. Photo from Wood et al. 1969. Introduction!0085 and 10084 were created during the Apollo 11 preliminary examination
More informationUsing the modified Gaussian model to extract quantitative data from lunar soils
Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 111,, doi:10.1029/2006je002721, 2006 Using the modified Gaussian model to extract quantitative data from lunar soils Sarah K. Noble, 1,2
More information15009 Single Drive Tube Station 6
15009 Single Drive Tube Station 6 Figure 2: Location of soil samples, trench and drive tube at station 6, Apollo 15. Figure 1: Photo of drive tube 15009 driven in all the way. AS15-86-11565. Introduction
More informationLunar Oxygen Production and Metals Extraction Using Ionic Liquids
Lunar Oxygen Production and Metals Extraction Using Ionic Liquids Matthew Marone, Mercer University, Macon, GA Mark Steven Paley, AZ Technology, Huntsville, AL David N. Donovan Marshall Space Flight Center
More informationLab 5: An Investigation of Meteorites Geology 202: Earth s Interior
Lab 5: An Investigation of Meteorites Geology 202: Earth s Interior Asteroids and Meteorites: What is the difference between asteroids and meteorites? Asteroids are rocky and metallic objects that orbit
More informationMinerals. Atoms, Elements, and Chemical Bonding. Definition of a Mineral 2-1
Minerals In order to define a what we mean by a mineral we must first make some definitions: 2-1 Most of the Earth s surface is composed of rocky material. An element is a substance which cannot be broken
More informationgrams grams Poikilitic Impact Melt Breccia
64567 13.8 grams 64569-14.3 grams Poikilitic Impact Melt Breccia Figure 1: Photo of 64567. Scale in mm. S72-55386 Mineralogical Mode by Simonds et al. (1973) 64567 64569 Plagioclase 69% 57 Pyroxene 10
More informationWORKING WITH ELECTRON MICROPROBE DATA FROM A HIGH PRESSURE EXPERIMENT CALCULATING MINERAL FORMULAS, UNIT CELL CONTENT, AND GEOTHERMOMETRY
WORKING WITH ELECTRON MICROPROBE DATA FROM A HIGH PRESSURE EXPERIMENT CALCULATING MINERAL FORMULAS, UNIT CELL CONTENT, AND GEOTHERMOMETRY Brandon E. Schwab Department of Geology Humboldt State University
More informationThermal, Thermophysical, and Compositional Properties of the Moon Revealed by the Diviner Lunar Radiometer
Thermal, Thermophysical, and Compositional Properties of the Moon Revealed by the Diviner Lunar Radiometer Benjamin T. Greenhagen Jet Propulsion Laboratory David A. Paige and the Diviner Science Team LEAG
More informationDifferentiation 2: mantle, crust OUTLINE
Differentiation 2: mantle, crust OUTLINE Reading this week: Should have been White Ch 10 and 11!! 7- Nov Differentiation of the Earth, Core formation W 10.6.6, 11.4 9- Nov Moon, crust, mantle, atmosphere
More informationMeteorites free samples from the solar system
Meteorites free samples from the solar system It is easier to believe that Yankee professors would lie, than that stones would fall from heaven [Thomas Jefferson, 3rd president of the USA] 2.1 Collection
More informationgrams grams Double Drive tube 61 cm
68002 583.5 grams 68001 840.7 grams Double Drive tube 61 cm Figure 1a: Surface photo for double drive tube 68001-2. AS16-108-17684. Introduction Station 8 was the closest to South Ray Crater so premission
More information65055 Basaltic Impact Melt grams
65055 Basaltic Impact Melt 500.8 grams Figure 1: Photo of 65055 showing large zap pit. Cube is 1 cm. S72-43869. Introduction According to the Apollo 16 Catalog by Ryder and Norman, 65055 is an aluminous,
More informationSupporting Information
Supporting Information Bindi et al. 10.1073/pnas.1111115109 Fig. S1. Electron microprobe X-ray elemental maps for the grain reported in Fig. 1B. Experimental details are given in Experimental Methods.
More informationBackground Image: SPA Basin Interior; LRO WAC, NASA/GSFC/ASU
B. L. Jolliff1, C. K. Shearer2, N. E. Petro3, D. A. Papanastassiou,4 Y. Liu,4 and L. Alkalai4 1Dept. of Earth & Planetary Sciences, Washington University, St. Louis, MO 2Institute of Meteoritics, University
More information72335 Impact melt Breccia grams
Impact melt Breccia 108.9 grams Figure 1: Location of on boulder #2 on landslide off of South Massif. Boulder is ~ 2-3 meters high. AS17-137-20918. Transcript Hey, that s a different rock, Gene (station
More informationLecture 3 Rocks and the Rock Cycle Dr. Shwan Omar
Rocks A naturally occurring aggregate of one or more minerals (e.g., granite), or a body of non-crystalline material (e.g., obsidian glass), or of solid organic material (e.g., coal). Rock Cycle A sequence
More informationAN INTRODUCTION TO COSMOCHEMISTRY
AN INTRODUCTION TO COSMOCHEMISTRY CHARLES R. COWLEY Professor of Astronomy, University of Michigan CAMBRIDGE UNIVERSITY PRESS Foreword V a % e x i 1 Overview 1 1.1 The Scope of Cosmochemistry 1 1.2 Cosmochemistry
More informationSupporting Information Appendix
Supporting Information Appendix 1. Supporting Text. Silica-rich terrestrial deposits without tridymite. 2. Table S1. Chemical compositions from Rietveld analysis and chemical composition of minerals used
More informationEinfluss von Mineralstäuben auf keramische Solarabsorber
15. Kölner Sonnenkolloquium Einfluss von Mineralstäuben auf keramische Solarabsorber Martin Schmücker Deutsches Zentrum für Luft- und Raumfahrt Institut für Werkstoff-Forschung 51147 Köln Honeycomb SiC
More informationThe Moon. Part II: Solar System. The Moon. A. Orbital Motion. The Moon s Orbit. Earth-Moon is a Binary Planet
Part II: Solar System The Moon Audio update: 2014Feb23 The Moon A. Orbital Stuff B. The Surface C. Composition and Interior D. Formation E. Notes 2 A. Orbital Motion 3 Earth-Moon is a Binary Planet 4 1.
More informationDirected Reading. Section: Rocks and the Rock Cycle. made of a. inorganic matter. b. solid organic matter. c. liquid organic matter. d. chemicals.
Skills Worksheet Directed Reading Section: Rocks and the Rock Cycle 1. The solid part of Earth is made up of material called a. glacial ice. b. lava. c. rock. d. wood. 2. Rock can be a collection of one
More informationASTRO 120 Sample Exam
ASTRO 120 Sample Exam 1) If a planet has a reasonably strong magnetic field, we know that a. It is made entirely of iron b. There is liquid nitrogen below the surface c. It can harbor life d. It has a
More informationTreatment of Data. Methods of determining analytical error -Counting statistics -Reproducibility of reference materials -Homogeneity of sample
Treatment of Data Methods of determining analytical error -Counting statistics -Reproducibility of reference materials -Homogeneity of sample Detection Limits Assessment of analytical quality -Analytical
More information1 st shell holds 2 electrons. 2 nd shell holds 8 electrons
ATOM INDIVISIBLE ELEMENTS - Nucleus = protons (+ charge) & neutrons (no charge ) - Electrons (- charge) orbit the nucleus in shells of 2, 8, 8 electrons (inner orbit outward) - Atomic number = number of
More informationLecture 36. Igneous geochemistry
Lecture 36 Igneous geochemistry Reading - White Chapter 7 Today 1. Overview 2. solid-melt distribution coefficients Igneous geochemistry The chemistry of igneous systems provides clues to a number of important
More informationgrams grams Crystalline matrix Breccia
14069 24.87 grams 14070-36.56 grams Crystalline matrix Breccia Figure 1: Photo of 14069,0. Scale in cm and mm. S78-28808. 14070 Figure 2: Photo of 14070. Scale is in cm. S71-22168. Introduction 14069 and
More informationShocked Carbonates May Spell in Martian Meteorite ALH84001
1 of 5 posted May 22, 1997 Shocked Carbonates May Spell in Martian Meteorite ALH84001 Written by Edward R.D. Scott Hawai'i Institute of Geophysics and Planetology, SOEST, University of Hawai'i In an electrifying
More informationpage - Lab 13 - Introduction to the Geology of the Terrestrial Planets
page - Lab 13 - Introduction to the Geology of the Terrestrial Planets Introduction There are two main families of planets in our solar system: the inner Terrestrial planets (Earth, Mercury, Venus, and
More informationAMHERST COLLEGE Department of Geology Geology 41: Environmental and Solid Earth Geophysics
AMHERST COLLEGE Department of Geology Geology 41: Environmental and Solid Earth Geophysics Lab 1: Meteorites EQUIPMENT: notebook and pen only In this lab, we will examine thin sections and hand samples
More informationMoon 101. Bellaire High School Team: Rachel Fisher, Clint Wu, Omkar Joshi
Moon 101 Bellaire High School Team: Rachel Fisher, Clint Wu, Omkar Joshi Part I Formation of the Moon Planetary Formation In the solar nebula, dust particles coalesced to form smaller planetesimals and
More informationTrinitite the Atomic Rock
Trinitite the Atomic Rock Nelson Eby, EEAS, University of Massachusetts, Lowell, MA Norman Charnley, Earth Sciences, University of Oxford, Oxford, UK John Smoliga, Roxbury, CT Special thanks to Robert
More informationChapter 7. The Moon. Copyright (c) The McGraw-Hill Companies, Inc. Permission required for reproduction or display.
Chapter 7 The Moon Copyright (c) The McGraw-Hill Companies, Inc. Permission required for reproduction or display. The Earth s Moon Earth s nearest neighbor is space Once the frontier of direct human exploration
More informationCERAMIC GLAZING as an IGNEOUS PROCESS
GEOL 640: Geology through Global Arts and Artifacts CERAMIC GLAZING as an IGNEOUS PROCESS GLAZE COMPONENTS A glaze is a waterproof silica glass on the surface of a ceramic pot, and was first produced by
More informationXUV 773: X-Ray Fluorescence Analysis of Gemstones
Fischer Application report vr118 HELM UT FISCHER GMBH + CO. KG Institut für Elektronik und Messtechnik Industriestrasse 21-7169 Sindelfingen, Germany Tel.: (+49) 731 33- - Fax: (+49) 731 33-79 E-Mail:
More informationWed. Oct. 04, Makeup lecture time? Will Friday noon work for everyone? No class Oct. 16, 18, 20?
Wed. Oct. 04, 2017 Reading: For Friday: Bugiolacchi et al. 2008 Laurence et al. 1998" Makeup lecture time? Will Friday noon work for everyone? No class Oct. 16, 18, 20? Today: Finish Lunar overview (from
More informationBasalt-Atmosphere Interactions on Venus - The Rocks Perspective. Allan Treiman Susanne Schwenzer LPI
Basalt-Atmosphere Interactions on Venus - The Rocks Perspective Allan Treiman Susanne Schwenzer LPI Plan of Talk Hoped to have more results - sorry! So, a selection of research problems on Venus rock-atmosphere
More informationMESSENGER: Exploring New Views of Mercury s Exosphere and Surface
MESSENGER: Exploring New Views of Mercury s Exosphere and Surface Ann L. Sprague 1, Ronald J. Vervack, Jr. 2, Rosemary M. Killen 3, William E. McClintock 4, Richard D. Starr 5, David Schriver 6, Pavel
More informationNew evidence for lunar basalt metasomatism by underlying regolith.
1 2 3 4 5 New evidence for lunar basalt metasomatism by underlying regolith. John F. Pernet-Fisher* School of Earth, Atmospheric, and Environmental Sciences, University of Manchester, Manchester, M13 2PL,
More informationMeteors. Meteors Comet dust particles entering our atmosphere and burning up from the friction. The Peekskill, NY Meteorite Fall.
Meteors Meteors Comet dust particles entering our atmosphere and burning up from the friction. 2 Updated july 19, 2009 Every year about Nov. 18 the Earth goes through the path of an old comet. Meteorites
More informationThe chemistry of exo-terrestrial material in evolved planetary systems. Boris Gänsicke
The chemistry of exo-terrestrial material in evolved planetary systems Boris Gänsicke Transiting planets M & R bulk densities What is the bulk composition of exo-planets? large degeneracy How to measure
More informationOUR SOLAR SYSTEM. James Martin. Facebook.com/groups/AstroLSSC Twitter.com/AstroLSSC
OUR SOLAR SYSTEM James Martin Facebook.com/groups/AstroLSSC Twitter.com/AstroLSSC It s time for the human race to enter the solar system. -Dan Quayle Structure of the Solar System Our Solar System contains
More informationReport on samples from the Great Basin Science Sample and Records Library
Jonathan G. Price, Ph.D. State Geologist and Director Nevada Bureau of Mines and Geology Office telephone: 775-784-6691 extension 5 1664 North Virginia Street Home telephone: 775-329-8011 University of
More informationA Rock is a solid aggregate of minerals.
Quartz A Rock is a solid aggregate of minerals. Orthoclase Feldspar Plagioclase Feldspar Biotite Four different minerals are obvious in this piece of Granite. The average automobile contains: Minerals
More informationSpace weathering of asteroidal surfaces
Space weathering of asteroidal surfaces Giovanni Strazzulla 1 & Rosario Brunetto 2 1 INAF Osservatorio Astrofisico di Catania, Italy gianni@oact.inaf.it 2 Institut d'astrophysique Spatiale, UMR 8617, Orsay,
More informationMoon and Mercury 3/8/07
The Reading Assignment Chapter 12 Announcements 4 th homework due March 20 (first class after spring break) Reminder about term paper due April 17. Next study-group session is Monday, March 19, from 10:30AM-12:00Noon
More informationSupplementary Materials for
advances.sciencemag.org/cgi/content/full/2/3/e1501725/dc1 Supplementary Materials for Discovery of natural MgSiO3 tetragonal garnet in a shocked chondritic meteorite The PDF file includes: Naotaka Tomioka,
More information23/9/2013 ENGINEERING GEOLOGY. Chapter 2: Rock classification:
ENGINEERING GEOLOGY Chapter 2: Rock classification: ENGINEERING GEOLOGY Chapter 1.0: Introduction to engineering geology Chapter 2.0: Rock classification Igneous rocks Sedimentary rocks Metamorphic rocks
More informationThe Moon. Tidal Coupling Surface Features Impact Cratering Moon Rocks History and Origin of the Moon
The Moon Tidal Coupling Surface Features Impact Cratering Moon Rocks History and Origin of the Moon Earth Moon Semi-major Axis 1 A.U. 384 x 10 3 km Inclination 0 Orbital period 1.000 tropical year 27.32
More informationWhat is the Moon? A natural satellite One of more than 96 moons in our Solar System The only moon of the planet Earth
The Moon What is the Moon? A natural satellite One of more than 96 moons in our Solar System The only moon of the planet Earth Location, location, location! About 384,000 km (240,000 miles) from Earth
More informationEarth Materials II Review Optical Mineralogy and Igneous Minerals
Earth Materials II Review Optical Mineralogy and Igneous Minerals Refractive Index and Angle of Refraction Refractive Index(R. I. ) = velocity of light in a vacuum velocity of light in a medium The refractive
More informationThe Periodic Table: Atoms, Elements, and Isotopes
Cosmic Chemistry: Understanding Elements The Periodic Table: Atoms, Elements, and Isotopes TEACHER TEXT The following is teacher background information and should only be used with students after they
More informationVOLCANIC STRATIGRAPHY AND PETROLOGY OF THE NORTHERN SNAEFELLSNES RIFT, SOUTHERN LAXÁRDALSFJÖLL, ICELAND
VOLCANIC STRATIGRAPHY AND PETROLOGY OF THE NORTHERN SNAEFELLSNES RIFT, SOUTHERN LAXÁRDALSFJÖLL, ICELAND LEBN SCHUYLER Whitman College Sponsor: John Winter INTRODUCTION Iceland is exposed above sea level
More informationrinds for 8 Loihi rocks. Sample spectra, fits and model compounds are shown in Figure S5. All
SUPPLEMENTARY INFORMATION Supplementary Table 1 Sample Location %Mats (M34, M39) 2L-FH (III)- smectite Vivianite Basalt glass red chi 2 J2-369-R2 Marker 17a 30% 21% - 11% 38% 0.06 J2-369-R5 Marker 17a
More informationRotated Magnets. posted May 22, 1997
1 of 6 posted May 22, 1997 Low-temperature Origin of Carbonates Consistent with Life in ALH84001 Written by G. Jeffrey Taylor Hawai'i Institute of Geophysics and Planetology, SOEST, University of Hawai'i
More informationSoil Mechanics/Geotechnical Engineering I Prof. Dilip Kumar Baidya Department of Civil Engineering Indian Institute of Technology, Kharagpur
Soil Mechanics/Geotechnical Engineering I Prof. Dilip Kumar Baidya Department of Civil Engineering Indian Institute of Technology, Kharagpur Lecture - 01 Rock Cycle Good morning. I welcome you to this
More informationTerramechanics. Origin and nature of lunar soil Soil mechanics Rigid wheel mechanics MARYLAND U N I V E R S I T Y O F
Terramechanics Origin and nature of lunar soil Soil mechanics Rigid wheel mechanics 1 2010 David L. Akin - All rights reserved http://spacecraft.ssl.umd.edu Lunar Regolith Broken down from larger pieces
More informationDifferentiation of planetary interiors. Rocky Planets Interiors and surface geophysics
Differentiation of planetary interiors Rocky Planets Interiors and surface geophysics Process of separation of internal planetary layers that takes place as a result of the physical and chemical properties
More informationWritten by G. Jeffrey Taylor Hawai i Institute of Geophysics and Planetology. A Plethera of Geochemical Data. May 8, 2009.
1 of 8 May 8, 2009 --- Chemical analyses of rocks on the Martian surface indicate that the Martian crust was built of basalt lava flows not much different from those on Earth. Written by G. Jeffrey Taylor
More information*Corresponding author. (Received 02 October 2015; revision accepted 06 June 2016)
Meteoritics & Planetary Science 1 24 (2016) doi: 10.1111/maps.12689 An analysis of Apollo lunar soil samples 12070,889, 12030,187, and 12070,891: Basaltic diversity at the Apollo 12 landing site and implications
More informationThe mathematics of scattering and absorption and emission
The mathematics of scattering and absorption and emission The transmittance of an layer depends on its optical depth, which in turn depends on how much of the substance the radiation has to pass through,
More informationLunar Geology ASTR 2120 Sarazin
Lunar Geology ASTR 2120 Sarazin Interior of the Moon Density low (3.3 gm/cc), very little iron No iron core Very small heat flow out of interior Little radioactive heating No magnetic field No molten iron
More informationTime to Solidify an Ocean of Magma
1 of 6 March 25, 2009 Time to Solidify an Ocean of Magma --- A small mineral grain places limits on how long it took the lunar magma ocean to solidify. Written by G. Jeffrey Taylor Hawai i Institute of
More informationgrams g g g g Regolith Breccia
15306 134.2 grams 15315 35.6 g 15324 32.3 g 15325 57.8 g 15330 57.8 g Regolith Breccia Figure 1a,b: Photo of dust-covered 15306. Sample is 7 cm across. S71-43064 and 067. Introduction 15306 is a regolith
More informationDiffusion in minerals and melts
Diffusion in minerals and melts There are three types of diffusion in a rock Surface diffusion essentially over a 2 dimensional area Grain-boundary diffusion along grain boundaries, slower than surface
More informationFinding Basalt Chips from Distant Maria
Page 1 of 12 posted April 30, 2006 Finding Basalt Chips from Distant Maria --- Tossed chips of lava help fill in blanks in our knowledge of lunar basalts. Written by G. Jeffrey Taylor Hawai'i Institute
More informationStudent Guide to Moon 101
Student Guide to Moon 101 LINKS TO WEBSITES AND DOCUMENTS NECESSARY TO COMPLETE MOON 101 CAN BE FOUND AT: 1) Read the following articles: PART 1 - FORMATION OF THE MOON a) The Scientific Legacy of Apollo,
More informationXM1/331 XM1/331 BLFX-3 XM1/331
a b AkC AkC strontian fluoro-apatite clinopyroxene phlogopite K-richterite XM1/331 clinopyroxene XM1/331 Fe-Ti ox c d clinopyroxene kric AkC ilmenite Sr-barite AkC XM1/331 BLFX-3 Supplementary Figure 1.
More informationAstronomy. physics.wm.edu/~hancock/171/ A. Dayle Hancock. Small 239. Office hours: MTWR 10-11am
Astronomy A. Dayle Hancock adhancock@wm.edu Small 239 Office hours: MTWR 10-11am The Moon The Moon's surface Humans on the Moon The Moon's interior The difference between Moon and Earth rocks The collision
More informationMian Abbas, Jim Spann, Andre LeClair NASA Marshall Space Flight Center, Huntsville, AL
Lunar Dust Distributions From So Infrared Absorption Measurement With a Fourier Transform Spectrometer Mian Abbas, Jim Spann, Andre LeClair NASA Marshall Space Flight Center, Huntsville, AL John Brasunas,
More informationPhys 214. Planets and Life
Phys 214. Planets and Life Dr. Cristina Buzea Department of Physics Room 259 E-mail: cristi@physics.queensu.ca (Please use PHYS214 in e-mail subject) Lecture 10. Geology and life. Part 1 (Page 99-123)
More informationTeachersʼ Guide. Creating Craters. Down to Earth KS3
Teachersʼ Guide Creating Craters Creating Craters! Creating Craters - Teachersʼ Guide - 2 Overview This lesson allows pupils to create impact craters in layered dry materials. Pupils can perform controlled
More informationAt the beginning. Matter + antimatter. Matter has the advantage. baryons quarks, leptons, electrons, photons (no protons or neutrons)
At the beginning Matter + antimatter Matter has the advantage baryons quarks, leptons, electrons, photons (no protons or neutrons) Hadrons protons, neutrons Hydrogen, helium (:0 H:He) Origin of the Universe
More informationAstro 210 Lecture 19 October 8, 2010
Astro 210 Lecture 19 October 8, 2010 Announcements Remember me? HW 5 due HW 6 available, due in class next Friday Night Observing continues next week Last time: The Moon Q: from Earth we only see one side
More informationTwo types of Terrain Highlands Maria This picture of the moon was taken with a telescope at Lick Observatory, CA
Two types of Terrain Highlands Maria This picture of the moon was taken with a telescope at Lick Observatory, CA A view seen by Apollo 17 astronauts as they orbited the Moon The Maria are smoother, lower,
More informationBreeding et al., Data Repository Material Figure DR1. Athens. Study Area
Breeding, Ague, and Brocker 1 Figure DR1 21 o 24 Greece o A 38 o Athens Tinos 37 o Syros Attic-Cycladic Blueschist Belt Syros Kampos B Study Area Ermoupoli N Vari Unit Cycladic HP-LT Unit Marble horizons
More information9/4/2015. Feldspars White, pink, variable Clays White perfect Quartz Colourless, white, red, None
ENGINEERING GEOLOGY Chapter 1.0: Introduction to engineering geology Chapter 2.0: Rock classification Igneous rocks Sedimentary rocks Metamorphic rocks Chapter 3.0: Weathering & soils Chapter 4.0: Geological
More informationA Model of Spectral Albedo of Particulate Surfaces: Implications for Optical Properties of the Moon
Icarus 137, 235 246 (1999) Article ID icar.1998.635, available online at http://www.idealibrary.com on A Model of Spectral Albedo of Particulate Surfaces: Implications for Optical Properties of the Moon
More information2. Terrestrial Planet G 9. Coulomb Force C 16. Babcock model Q. 3. Continuous Spectrum K 10. Large-impact hypothesis I 17.
Astronomy 1 S 16 Exam 1 Name Identify terms Label each term with the appropriate letter of a definition listed 1. Spectral line R 8. Albedo H 15. helioseismology E 2. Terrestrial Planet G 9. Coulomb Force
More informationAstronomy 103: First Exam
Name: Astronomy 103: First Exam Stephen Lepp October 27, 2010 Each question is worth 2 points. Write your name on this exam and on the scantron. 1 Short Answer A. What is the largest of the terrestrial
More information