DOCSLIB.ORG

Name Cat. No. Type Group Locality Fall Date Year Weight Units

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Name Cat. No. Type Group Locality Fall Date Year Weight Units Name Cat. No. Type Group Locality Fall Date Year Weight Units Aarhus 3986 OC H6 Denmark Fall October 2 1951 2.9 gms Abbott 4429 OC H6 New Mexico Find - 1951 5.3 gms Abbott 4748 OC H6 New Mexico Find - 1951 86.5 gms Abee 3907 EC EH4 Canada Fall June 10 1952 291.5 gms Abee 3987 EC EH4 Canada Fall June 10 1952 1010 gms Abernathy 3988 OC L6 Texas Find - 1941 2.2 gms Acapulco 4492 PA ACA Mexico Fall August 11 1976 10.3 gms Acfer 028 4806 OC H3 Algeria Find- 1989-90 16.6 gms Acfer 063 4759 SI MES Algeria Find - 1989-90 65.2 gms Acfer 082 4807 CC CV3 Algeria Find - 1989-90 10.2 gms Acfer 097 4808 CC CR2 Algeria Find - 1989-90 20.6 gms Acfer 139 4793 CC CR2 Algeria Find- 1989-90 8.8 gms Acfer 166 4809 OC H3-5 Algeria Find - 1989-90 21.5 gms Acfer 182 4810 CC CR CLANAlgeria Find - 1989-90 4.4 gms Acfer 202 4811 CC CO3 Algeria Find- 1989-90 1.4 gms Acfer 207 4828 CC CR CLANAlgeria Find - 1989-90 0.01 gms Acfer 214 4820 CC CR CLAN Algeria Find - 1991 9.8 gms Achilles 3837 OC H5 Kansas Find - 1924 138.7 gms Achiras 3933 OC L6 Argentina Fall - 1902 48.4 gms Acme 3990 OC H5 New Mexico Find - 1947 10.6 gms Acuna 4812 IR IVA Mexico Find - 1981 26.6 gms Adams County 3991 OC H5 Colorado Find - 1928 1 gms Adelaide 4718 CC CM2 Australia Find - 1972 0.78 gms Adelie Land 3992 OC L5 Antarctica Find - 1912 2.4 gms Adhi Kot 3993 EC EH4 Pakistan Fall May 1 1919 63.2 gms Admire 322 SI PAL Kansas Find - 1881 522.6 gms Admire 3754 SI PAL Kansas Find - 1881 5600 gms Admire 4176 SI PAL Kansas Find - 1881 223.7 gms Adrian 3994 OC H4 Texas Find - 1936 0.7 gms Adrian 4385 OC H4 Texas Find- 1936 129 gms Agen 394 OC H5 France Fall September 5 1814 77 gms Agoult 5176 AC EUC Morocco Find 2000 3.5 gms Aguada 3934 OC L6 Argentina Fall September 1930 74 gms Ahumada 323 SI PAL Mexico Find - 1909 2221.9 gms Ainsworth 35 IR IIB Nebraska Find - 1907 22 gms Ainsworth 67 IR IIB Nebraska Find - 1907 1054 gms Ainsworth 850 IR IIB Nebraska Find - 1907 2693.2 gms Ainsworth 853 IR IIB Nebraska Find - 1907 17.1 gms Aioun El Atrouss 4466 AC DIO Mauritania Fall April 17 1974 60.7 gms Akaba 3995 OC L6 Jordan Fall September 21 1949 0.6 gms Akron (1940) 3996 OC H6 Colorado Find - 1940 1.2 gms Akron (1961) 4160 OC L6 Colorado Find - 1961 42.6 gms Akwanga 3997 OC H Nigeria Fall July 2 1959 0.9 gms Akwanga 4829 OC H Nigeria Fall July 2 1959 5.4 gms Akwanga 4860 OC H Nigeria Fall July 2 1959 54 gms Al Rais 4168 CC CR2 Saudi Arabia Fall December 10 1957 1.85 gms Alais 395 CC CI1 France Fall March 15 1806 0.3 gms Alamogordo 3831 OC H5 New Mexico Find - 1938 365.4 gms Albin 4373 SI PAL Wyoming Find - 1915 1715 gms Albion 4894 IR IVA Washington Find - 1966 3953.9 gms Aldama 4707 IR IIIAB Mexico Find - 1985 156 gms Aldsworth 397 OC LL5 England Fall August 4 1835 0.5 gms Aleppo 398 OC L6 Syria Fall - 1873 126.8 gms Alessandria 2224 OC H5 Italy Fall February 2 1860 8.8 gms Alexander County 77 IR IA North Carolina Find - 1875 60.5 gms Alfianello 399 OC L6 Italy Fall February 16 1883 1363 gms Alfianello 638 OC L6 Italy Fall February 16 1883 5.6 gms Allan Hills 76009 4535 OC L6 Antarctica Find - 1976 910 gms Allegan 371 OC H5 Michigan Fall July 10 1899 95.4 gms Allende 4284 CC CV3 Mexico Fall February 8 1969 264.7 gms Allende 4285 CC CV3 Mexico Fall February 8 1969 301.7 gms Allende 4286 CC CV3 Mexico Fall February 8 1969 143 gms Allende 4287 CC CV3 Mexico Fall February 8 1969 238 gms Allende 4288 CC CV3 Mexico Fall February 8 1969 191.1 gms Allende 4289 CC CV3 Mexico Fall February 8 1969 102.8 gms Allende 4290 CC CV3 Mexico Fall February 8 1969 251.8 gms Allende 4291 CC CV3 Mexico Fall February 8 1969 448.3 gms Allende 4292 CC CV3 Mexico Fall February 8 1969 344.4 gms Allende 4293 CC CV3 Mexico Fall February 8 1969 102.9 gms Allende 4294 CC CV3 Mexico Fall February 8 1969 498 gms Allende 4295 CC CV3 Mexico Fall February 8 1969 477.9 gms Allende 4296 CC CV3 Mexico Fall February 8 1969 900.6 gms Allende 4297 CC CV3 Mexico Fall February 8 1969 141.3 gms Allende 4298 CC CV3 Mexico Fall February 8 1969 225.3 gms Allende 4299 CC CV3 Mexico Fall February 8 1969 174.4 gms Allende 4300 CC CV3 Mexico Fall February 8 1969 57.7 gms Allende 4301 CC CV3 Mexico Fall February 8 1969 230.6 gms Allende 4302 CC CV3 Mexico Fall February 8 1969 288.9 gms Allende 4303 CC CV3 Mexico Fall February 8 1969 360 gms Allende 4304 CC CV3 Mexico Fall February 8 1969 514.2 gms Allende 4305 CC CV3 Mexico Fall February 8 1969 161.8 gms Allende 4306 CC CV3 Mexico Fall February 8 1969 109.7 gms Allende 4307 CC CV3 Mexico Fall February 8 1969 114.6 gms Allende 4308 CC CV3 Mexico Fall February 8 1969 161.8 gms Allende 4309 CC CV3 Mexico Fall February 8 1969 77.1 gms Allende 4310 CC CV3 Mexico Fall February 8 1969 94.5 gms Allende 4311 CC CV3 Mexico Fall February 8 1969 66.4 gms Allende 4312 CC CV3 Mexico Fall February 8 1969 660.5 gms Allende 4313 CC CV3 Mexico Fall February 8 1969 356 gms Allende 4314 CC CV3 Mexico Fall February 8 1969 91.5 gms Allende 4315 CC CV3 Mexico Fall February 8 1969 143.8 gms Allende 4316 CC CV3 Mexico Fall February 8 1969 49.8 gms Allende 4317 CC CV3 Mexico Fall February 8 1969 69.2 gms Allende 4318 CC CV3 Mexico Fall February 8 1969 96 gms Allende 4319 CC CV3 Mexico Fall February 8 1969 586 gms Allende 4320 CC CV3 Mexico Fall February 8 1969 646 gms Allende 4321 CC CV3 Mexico Fall February 8 1969 367.7 gms Allende 4322 CC CV3 Mexico Fall February 8 1969 546.1 gms Allende 4323 CC CV3 Mexico Fall February 8 1969 412.4 gms Allende 4324 CC CV3 Mexico Fall February 8 1969 112.4 gms Allende 4327 CC CV3 Mexico Fall February 8 1969 733.5 gms Allende 4328 CC CV3 Mexico Fall February 8 1969 1101.6 gms Allende 4329 CC CV3 Mexico Fall February 8 1969 559.8 gms Allende 4330 CC CV3 Mexico Fall February 8 1969 461.4 gms Allende 4331 CC CV3 Mexico Fall February 8 1969 763 gms Allende 4332 CC CV3 Mexico Fall February 8 1969 772.5 gms Allende 4333 CC CV3 Mexico Fall February 8 1969 4057 gms Allende 4880 CC CV3 Mexico Fall February 8 1969 55.8 gms Allende 4884 CC CV3 Mexico Fall February 8 1969 1741.3 gms Allende 4946 CC CV3 Mexico Fall February 8 1969 5.2 gms Allende 4947 CC CV3 Mexico Fall February 8 1969 35.6 gms Allende 4948 CC CV3 Mexico Fall February 8 1969 1413.5 gms Allende 5046 CC CV3 Mexico Fall February 8 1969 72.9 gms Allende 5047 CC CV3 Mexico Fall February 8 1969 81.5 gms Allende 5048 CC CV3 Mexico Fall February 8 1969 406.6 gms Allende 5049 CC CV3 Mexico Fall February 8 1969 83.8 gms Allende 5050 CC CV3 Mexico Fall February 8 1969 140.2 gms Allende 5051 CC CV3 Mexico Fall February 8 1969 40.9 gms Allende 5052 CC CV3 Mexico Fall February 8 1969 78.5 gms Allende 5053 CC CV3 Mexico Fall February 8 1969 179.2 gms Allende 5054 CC CV3 Mexico Fall February 8 1969 141.5 gms Allende 5055 CC CV3 Mexico Fall February 8 1969 6.7 gms Allende 5056 CC CV3 Mexico Fall February 8 1969 129.7 gms Allende 5057 CC CV3 Mexico Fall February 8 1969 73.4 gms Allende 5058 CC CV3 Mexico Fall February 8 1969 216 gms Allende 5059 CC CV3 Mexico Fall February 8 1969 86.7 gms Allende 5060 CC CV3 Mexico Fall February 8 1969 15.5 gms Allende 5061 CC CV3 Mexico Fall February 8 1969 57.3 gms Allende 5062 CC CV3 Mexico Fall February 8 1969 6.2 gms Allende 5063 CC CV3 Mexico Fall February 8 1969 154.5 gms Allende 5064 CC CV3 Mexico Fall February 8 1969 6460 gms Allende 5085 CC CV3 Mexico Fall February 8 1969 703 gms Allende 5144 CC CV3 Mexico Fall February 8 1969 149 gms Allende 5145 CC CV3 Mexico Fall February 8 1969 38 gms Allende 5146 CC CV3 Mexico Fall February 8 1969 18 gms Allende 5147 CC CV3 Mexico Fall February 8 1969 17.6 gms Allende (Presolar Diamonds) 4975 CC CV3 Mexico Fall February 8 1969 0.9 mgs Allende (Std) 3529 CC CV3 Mexico Fall February 8 1969 6.1 gms Alvord 4588 IR IVA Iowa Find June 15 1976 77.6 gms Ambapur Nagla 401 OC H5 India Fall May 27 1895 82.6 gms Amherst 4593 OC L6 Nebraska Find- 1947 40.9 gms Andover 3998 OC L6 Maine Fall August 5 1898 0.8 gms Andura 3999 OC H6 India Fall August 9 1939 1 gms Angelica 3913 IR IIIA Wisconsin Find - 1916 110.3 gms Angers 402 OC L6 France Fall June 3 1822 1 gms Angers 1049 OC L6 France Fall June 3 1822 18.7 gms Angra Dos Reis 4494 AC ANG Brazil Fall January 1869 0.1 gms Angra Dos Reis 4628 AC ANG Brazil Fall January 1869 0.08 gms Angra Dos Reis 4790 AC ANG Brazil Fall January 1869 3.9 gms Anoka 4161 IR IIIC Minnesota Find - 1961 39.4 gms Apoala 129 IR IIIB Mexico Find - 1889 79 gms Appley Bridge 3922 OC LL6 England Fall October 13 1914 214.9 gms Apt 403 OC L6 France Fall October 8 1803 1.3 gms Arapahoe 4271 OC L5 Colorado Find- 1940 52.2 gms Arcadia 3939 OC LL6 Nebraska Find- 1937 63.4 gms Archie 4000 OC H6 Missouri Fall August 10 1932 46 gms Arispe 236 IR IC-AN Mexico Find - 1896 6104.8 gms Arlington 61 IR IIE Minnesota Find - 1894 991.7 gms Armel 4334 OC L5 Colorado Find- 1967 63.2 gms Armel 4461 OC L5 Colorado Find- 1967 61.5 gms Arriba 3820 OC L5 Colorado Find- 1936 169.9 gms Artracoona 4001 OC L6 Australia Find - 1914 5.7 gms Asco 606 OC L France FallNovember 1805 1.9 gms Ashmore 4371 OC H5 Texas Find- 1969 100.3 gms Assam 599 OC L5 India Find - 1846 1.3 gms Assisi 405 OC H5 Italy Fall May 24 1886 4.4 gms Atemajac 4002 OC L6 Mexico Fall February 26 1896 0.5 gms Atlanta 3923 EC EL6 Louisiana Find - 1938 141.8 gms Atwood 4248 OC L6 Colorado Find- 1963 49.2 gms Augusta County 122 IR IIIA Virginia Find - 1859 1143.7 gms Augustinovka 193 IR IIIB Ukraine Find - 1890 252.5 gms Augustinovka 2537 IR IIIB Ukraine Find - 1890 51 gms Aumale 407 OC L6 Algeria Fall August 25 1865 60 gms Aumieres 652 OC L6 France Fall June 3 1842 45.2 gms Aurora 4003 OC H4 New Mexico Find - 1938 2.3 gms
Load more

Recommended publications
  • 19660017397.Pdf
    .. & METEORITIC RUTILE Peter R. Buseck Departments of Geology and Chemistry Arizona State University Tempe, Arizona Klaus Keil Space Sciences Division National Aeronautics and Space Administration Ames Research Center Mof fett Field, California r ABSTRACT Rutile has not been widely recognized as a meteoritic constituent. show, Recent microscopic and electron microprobe studies however, that Ti02 . is a reasonably widespread phase, albeit in minor amounts. X-ray diffraction studies confirm the Ti02 to be rutile. It was observed in the following meteorites - Allegan, Bondoc, Estherville, Farmington, and Vaca Muerta, The rutile is associated primarily with ilmenite and chromite, in some cases as exsolution lamellae. Accepted for publication by American Mineralogist . Rutile, as a meteoritic phase, is not widely known. In their sunanary . of meteorite mineralogy neither Mason (1962) nor Ramdohr (1963) report rutile as a mineral occurring in meteorites, although Ramdohr did describe a similar phase from the Faxmington meteorite in his list of "unidentified minerals," He suggested (correctly) that his "mineral D" dght be rutile. He also ob- served it in several mesosiderites. The mineral was recently mentioned to occur in Vaca Huerta (Fleischer, et al., 1965) and in Odessa (El Goresy, 1965). We have found rutile in the meteorites Allegan, Bondoc, Estherville, Farming- ton, and Vaca Muerta; although nowhere an abundant phase, it appears to be rather widespread. Of the several meteorites in which it was observed, rutile is the most abundant in the Farmington L-group chondrite. There it occurs in fine lamellae in ilmenite. The ilmenite is only sparsely distributed within the . meteorite although wherever it does occur it is in moderately large clusters - up to 0.5 mn in diameter - and it then is usually associated with chromite as well as rutile (Buseck, et al., 1965), Optically, the rutile has a faintly bluish tinge when viewed in reflected, plane-polarized light with immersion objectives.
    [Show full text]
  • Meteorite in Den Polargebiefen
    Literatur: chemische Untersuchungen in den Alpen. Zb1. 1) Gor h a m , E.: The salt content of some Ice­ Aerosolforsch. 10, 1962, 97-105. samples from Nordaustlandet, Svalbord, :r. of 6) Tarn a n n , G.: Die Bildung des Gletscher­ Glaciology, 3, 1957, 181-186. korns, Naturwiss. 17, 1929, 851-854. 2) Gor h a m , E.: Soluble salts in a temperate 7) Renaud, A.: A contribution to the study of glacier Tellus, 10, 1958, 496-497. the glacter-graln. J. of Glaciology, 1, 1949, 3) Renaud, A.: Nouvelle contribution ä l' Hude 328-324. du grain de glacier. IUGG-Konferenzbericht, 8) R e v eIl e, R. und S u e s S, H.: Carbon dio­ Brüssel 1951, 206-211. xide exehange between atmosphere and ocean 4) Junge, C. E.: Sulfur in the atmosphere. :r of and the question of anincrease of atmospheric Geophys. Res .. 65, 1960, 227-237. CO. during the past decades Tellus, 9, 1957, 5) G e 0 r g 11, H. W. und Web er, E.: Luft- 18-27. Meteorite in den Polargebiefen Von Werner Sandner, Grafing-Bahnhof '}) Gegenüber den Vertretern aller anderen tische Gebiet zu zählen sind und wieviele naturwissenschaftlichen Disziplinen ist der Fundorte bereits südlich desselben liegen. Astronom insofern benachteiligt, als er die Was die benutzten literarischen Unterlagen Objekte seines Forschens nicht im Labora­ betrifft, so reicht der Katalog von Leonard torium einer Untersuchung unterwerfen, bis zum Jahre 1955, während das Werk von nicht mit ihnen "experimentieren" kann. Er Krinow alle Fälle und Funde bis 1956 ent­ ist vielmehr auf die Kunde angewiesen, die hält.
    [Show full text]
  • The M~Neralogical Composition and Structure of the Assisi Meteorite
    595 The m~neralogical composition and structure of the Assisi meteorite By G. R. LEvI-DoNATI (Doctor in Natural Sciences) Istituto di Mineralogia, Facolth di Scienze, Universit~ di Perugia, Italy [Taken as read 2 November 1966] Summary. The principal data about the fall and the distribution of the fragments of the Assisi (Perugia, Italy) meteorite are collected. A fragment of the stone, weighing 146.5 g, preserved in the British Museum (Natural History) (B.M. 63621), is described in some detail. Crust morphology, mineralogical composition, and structure are studied. Optical data are established by microscopical analysis of five thin sections and two polished surfaces. Compared with electron-probe analysis, they are found in good agreement. Assisi is an olivine-bronzite chondrite, H group, with characteristic features of metamorphism. N 24 May 1886, at 7 a.m., the sky being clear, a single stone weigh- O ing 1795 g fell in a cornfield in Tordandrea, 7"5 Km south-west of Assisi (Perugia, Italy). Three peasants were present and immediately unearthed the small meteorite. It was at a depth of about 60 cm, in an apparently vertical hole about 25 cm in diameter. The stone was 13.8 cm long, 12.8 cm wide. The fall was first described by Bellucci (1887), who submitted the individual specimen to a macroscopic examination. In the same year the complete meteorite was sent by Be]lucci to Vienna, where Eger made a cast of the stone and sawed the meteorite in several pieces. 1 Museums and collections later purchased the fragments, which (1967) are now widely distributed (B.
    [Show full text]
  • Laboratory Spectroscopy of Meteorite Samples at UV-Vis-NIR Wavelengths: Analysis and Discrimination by Principal Components Analysis
    Laboratory spectroscopy of meteorite samples at UV-Vis-NIR wavelengths: Analysis and discrimination by principal components analysis Antti Penttil¨aa,∗, Julia Martikainena, Maria Gritsevicha, Karri Muinonena,b aDepartment of Physics, P.O. Box 64, FI-00014 University of Helsinki, Finland bFinnish Geospatial Research Institute FGI, National Land Survey of Finland, Geodeetinrinne 2, FI-02430 Masala, Finland Abstract Meteorite samples are measured with the University of Helsinki integrating-sphere UV-Vis- NIR spectrometer. The resulting spectra of 30 meteorites are compared with selected spectra from the NASA Planetary Data System meteorite spectra database. The spectral measure- ments are transformed with the principal component analysis, and it is shown that different meteorite types can be distinguished from the transformed data. The motivation is to im- prove the link between asteroid spectral observations and meteorite spectral measurements. Keywords: Meteorites, spectroscopy, principal component analysis 1. Introduction While a planet orbits the Sun, it is subject to impacts by objects ranging from tiny dust particles to much larger asteroids and comet nuclei. Such collisions of small Solar System bodies with planets have taken place frequently over geological time and played an 5 important role in the evolution of planets and development of life on the Earth. Every day approximately 30{180 tons of interplanetary material enter the Earth's atmosphere [1, 2]. This material is mostly represented by smaller meteoroids that undergo rapid ablation in the atmosphere. Under favorable initial conditions part of a meteoroid may survive the atmospheric entry and reach the ground [3]. The fragments recovered on the ground are 10 called meteorites, our valuable samples of the Solar System.
    [Show full text]
  • Appendix A: Scientific Notation
    Appendix A: Scientific Notation Since in astronomy we often have to deal with large numbers, writing a lot of zeros is not only cumbersome, but also inefficient and difficult to count. Scientists use the system of scientific notation, where the number of zeros is short handed to a superscript. For example, 10 has one zero and is written as 101 in scientific notation. Similarly, 100 is 102, 100 is 103. So we have: 103 equals a thousand, 106 equals a million, 109 is called a billion (U.S. usage), and 1012 a trillion. Now the U.S. federal government budget is in the trillions of dollars, ordinary people really cannot grasp the magnitude of the number. In the metric system, the prefix kilo- stands for 1,000, e.g., a kilogram. For a million, the prefix mega- is used, e.g. megaton (1,000,000 or 106 ton). A billion hertz (a unit of frequency) is gigahertz, although I have not heard of the use of a giga-meter. More rarely still is the use of tera (1012). For small numbers, the practice is similar. 0.1 is 10À1, 0.01 is 10À2, and 0.001 is 10À3. The prefix of milli- refers to 10À3, e.g. as in millimeter, whereas a micro- second is 10À6 ¼ 0.000001 s. It is now trendy to talk about nano-technology, which refers to solid-state device with sizes on the scale of 10À9 m, or about 10 times the size of an atom. With this kind of shorthand convenience, one can really go overboard.
    [Show full text]
  • Deep Carbon Science
    From Crust to Core Carbon plays a fundamental role on Earth. It forms the chemical backbone for all essential organic molecules produced by living organ- isms. Carbon-based fuels supply most of society’s energy, and atmos- pheric carbon dioxide has a huge impact on Earth’s climate. This book provides a complete history of the emergence and development of the new interdisciplinary field of deep carbon science. It traces four cen- turies of history during which the inner workings of the dynamic Earth were discovered, and it documents the extraordinary scientific revolutions that changed our understanding of carbon on Earth for- ever: carbon’s origin in exploding stars; the discovery of the internal heat source driving the Earth’s carbon cycle; and the tectonic revolu- tion. Written with an engaging narrative style and covering the scien- tific endeavors of about 150 pioneers of deep geoscience, this is a fascinating book for students and researchers working in Earth system science and deep carbon research. is a life fellow at St. Edmund’s College, University of Cambridge. For more than 50 years he has passionately engaged in bringing discoveries in astronomy and cosmology to the general public. He is a fellow of the Royal Historical Society, a former vice- president of the Royal Astronomical Society and a fellow of the Geological Society. The International Astronomical Union designated asteroid 4027 as Minor Planet Mitton in recognition of his extensive outreach activity and that of Dr. Jacqueline Mitton. From Crust to Core A Chronicle of Deep Carbon Science University of Cambridge University Printing House, Cambridge CB2 8BS, United Kingdom One Liberty Plaza, 20th Floor, New York, NY 10006, USA 477 Williamstown Road, Port Melbourne, VIC 3207, Australia 314–321, 3rd Floor, Plot 3, Splendor Forum, Jasola District Centre, New Delhi – 110025, India 79 Anson Road, #06–04/06, Singapore 079906 Cambridge University Press is part of the University of Cambridge.
    [Show full text]
  • Putative Microbial Mediation in NASA Lunar Sample Set: Microtextural Features at High Magnification
    EPSC Abstracts Vol. 13, EPSC-DPS2019-1-1, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Putative microbial mediation in NASA lunar sample set: microtextural features at high magnification Szaniszló Bérczi (1), Márta Polgári (2,3), Ildikó Gyollai (2), Arnold Gucsik A.(3) (1) Eötvös University, Institute of Physics, Dept. Materials Physics, Cosmic Materials Space Res. Group, H-1117 Bu-dapest, Pázmány Péter sétány 1/a. Hungary, ([email protected]), (2) Institute for Geological and Geochemical Research, RCAES, Biogeochemical Working Group, HAS, H-1112 Budapest, Budaörsi u. 45, Hungary, ([email protected]), ([email protected]), (3) Eszterházy Károly University, Department of Natural Geography and Geoinformatics, 3300 Eger, Leányka str. 6, Hungary ([email protected]). Abstract 60025 lunar sample is a coarse grained brecciated (cata- The NASA Lunar Educational Set is since 25 year in clastic) anorthosite, in which rarely pyroxene is spotted. In Hungary, curating by B. Sz. at Eötvös University. As non- the vicinity of the pyroxenes the texture was interwoven by destructive method, only high resolution optical mi-crobial-like filamentous biosignatures (Fig. 3). microscopy is allowed by NASA. This method is good for microtextural studies of processes, where we found 2. Results and Discussion putative microbial features. To determination of microbial Optical microscopy is the allowed study form for the signatures Raman and FTIR spectroscopy would be NASA educational samples. We used it in extremely large requires to identify fine-grained biominerals and organic magnifica-tion capacity in order to see the texture in fine material, as the authors did by other meteorite and details [3, 4, 5, 6, 7].
    [Show full text]
  • 18Th EANA Conference European Astrobiology Network Association
    18th EANA Conference European Astrobiology Network Association Abstract book 24-28 September 2018 Freie Universität Berlin, Germany Sponsors: Detectability of biosignatures in martian sedimentary systems A. H. Stevens1, A. McDonald2, and C. S. Cockell1 (1) UK Centre for Astrobiology, University of Edinburgh, UK ([email protected]) (2) Bioimaging Facility, School of Engineering, University of Edinburgh, UK Presentation: Tuesday 12:45-13:00 Session: Traces of life, biosignatures, life detection Abstract: Some of the most promising potential sampling sites for astrobiology are the numerous sedimentary areas on Mars such as those explored by MSL. As sedimentary systems have a high relative likelihood to have been habitable in the past and are known on Earth to preserve biosignatures well, the remains of martian sedimentary systems are an attractive target for exploration, for example by sample return caching rovers [1]. To learn how best to look for evidence of life in these environments, we must carefully understand their context. While recent measurements have raised the upper limit for organic carbon measured in martian sediments [2], our exploration to date shows no evidence for a terrestrial-like biosphere on Mars. We used an analogue of a martian mudstone (Y-Mars[3]) to investigate how best to look for biosignatures in martian sedimentary environments. The mudstone was inoculated with a relevant microbial community and cultured over several months under martian conditions to select for the most Mars-relevant microbes. We sequenced the microbial community over a number of transfers to try and understand what types microbes might be expected to exist in these environments and assess whether they might leave behind any specific biosignatures.
    [Show full text]
  • The Mineralogical Magazine Journal
    THE MINERALOGICAL MAGAZINE AND JOURNAL OF THE MINERALOGICAL SOCIETY. 1~o. 40. OCTOBER 1889. Vol. VIII. On the Meteorites which have been found iu the Desert of Atacama and its neighbourhood. By L. FLETCHER, M.A., F.R.S., Keeper of Minerals in the British Museum. (With a Map of the District, Plate X.) [Read March 12th and May 7th, ]889.J 1. THE immediate object of the present paper is to place on record J- the history and characters of several Atacama meteorites of which no description has yet been published; but incidentally it is con- venient at the same time to consider the relationship of these masses to others from the same region, which either have been already described, or at least are stated to be preserved in one or more of the known Meteo. rite-Collections. 2. The term " Desert of Atacama " is generally applied to that part of western South America which lies between the towns of Copiapo and Cobija, about 330 miles distant from each other, and which extends island as far as the Indian hamlet of Antofagasta, about 180 miles from 224 L. FLETCHER ON THE METEORITES OF ATACAMA. the coast. The Atacama meteorites preserved in the Collections have been found at several places widely separated throughout the Desert. 3. A critical examination of the descriptive literature, and a compari- son of the manuscript and printed meteorite-lists, which have been placed at my service, lead to the conclusion that all the meteoritic frag- ments from Atacama now preserved in the known Collections belong to one or other of at most thirteen meteorites, which, for reasons given below, are referred to in this paper under the following names :-- 1.
    [Show full text]
  • Organic Matter in Meteorites Department of Inorganic Chemistry, University of Barcelona, Spain
    REVIEW ARTICLE INTERNATIONAL MICROBIOLOGY (2004) 7:239-248 www.im.microbios.org Jordi Llorca Organic matter in meteorites Department of Inorganic Chemistry, University of Barcelona, Spain Summary. Some primitive meteorites are carbon-rich objects containing a vari- ety of organic molecules that constitute a valuable record of organic chemical evo- lution in the universe prior to the appearance of microorganisms. Families of com- pounds include hydrocarbons, alcohols, aldehydes, ketones, carboxylic acids, amino acids, amines, amides, heterocycles, phosphonic acids, sulfonic acids, sugar-relat- ed compounds and poorly defined high-molecular weight macromolecules. A vari- ety of environments are required in order to explain this organic inventory, includ- ing interstellar processes, gas-grain reactions operating in the solar nebula, and hydrothermal alteration of parent bodies. Most likely, substantial amounts of such Received 15 September 2004 organic materials were delivered to the Earth via a late accretion, thereby provid- Accepted 15 October 2004 ing organic compounds important for the emergence of life itself, or that served as a feedstock for further chemical evolution. This review discusses the organic con- Address for correspondence: Departament de Química Inorgànica tent of primitive meteorites and their relevance to the build up of biomolecules. Universitat de Barcelona [Int Microbiol 2004; 7(4):239-248] Martí i Franquès, 1-11 08028 Barcelona, Spain Tel. +34-934021235. Fax +34-934907725 Key words: primitive meteorites · prebiotic chemistry · chemical evolution · E-mail: [email protected] origin of life providing new opportunities for scientific advancement. One Introduction of the most important findings regarding such bodies is that comets and certain types of meteorites contain organic mole- Like a carpentry shop littered with wood shavings after the cules formed in space that may have had a relevant role in the work is done, debris left over from the formation of the Sun origin of the first microorganisms on Earth.
    [Show full text]
  • A Magnetic Susceptibility Database for Stony Meteorites
    Direttore Enzo Boschi Comitato di Redazione Cesidio Bianchi Tecnologia Geofisica Rodolfo Console Sismologia Giorgiana De Franceschi Relazioni Sole-Terra Leonardo Sagnotti Geomagnetismo Giancarlo Scalera Geodinamica Ufficio Editoriale Francesca Di Stefano Istituto Nazionale di Geofisica e Vulcanologia Via di Vigna Murata, 605 00143 Roma Tel. (06) 51860468 Telefax: (06) 51860507 e-mail: [email protected] A MAGNETIC SUSCEPTIBILITY DATABASE FOR STONY METEORITES Pierre Rochette1, Leonardo Sagnotti1, Guy Consolmagno2, Luigi Folco3, Adriana Maras4, Flora Panzarino4, Lauri Pesonen5, Romano Serra6 and Mauri Terho5 1Istituto Nazionale di Geofisica e Vulcanologia, Roma, Italy [[email protected]] 2Specola Vaticana, Castel Gandolfo, Italy 3Antarctic [PNRA] Museum of Siena, Siena, Italy 4Università La Sapienza, Roma, Italy 5University of Helsinki, Finland 6“Giorgio Abetti” Museum of San Giovanni in Persiceto, Italy Pierre Rochette et alii: A Magnetic Susceptibility Database for Stony Meteorites 1. Introduction the Museo Nationale dell’Antartide in Siena [Folco and Rastelli, 2000], the University of More than 22,000 different meteorites Roma “la Sapienza” [Cavaretta Maras, 1975], have been catalogued in collections around the the “Giorgio Abetti” Museum in San Giovanni world (as of 1999) of which 95% are stony types Persiceto [Levi-Donati, 1996] and the private [Grady, 2000]. About a thousand new meteorites collection of Matteo Chinelatto. In particular, are added every year, primarily from Antarctic the Antarctic Museum in Siena is the curatorial and hot-desert areas. Thus there is a need for centre for the Antarctic meteorite collection rapid systematic and non-destructive means to (mostly from Frontier Mountain) recovered by characterise this unique sampling of the solar the Italian Programma Nazionale di Ricerche in system materials.
    [Show full text]
  • Curt Teich Postcard Archives Towns and Cities
    Curt Teich Postcard Archives Towns and Cities Alaska Aialik Bay Alaska Highway Alcan Highway Anchorage Arctic Auk Lake Cape Prince of Wales Castle Rock Chilkoot Pass Columbia Glacier Cook Inlet Copper River Cordova Curry Dawson Denali Denali National Park Eagle Fairbanks Five Finger Rapids Gastineau Channel Glacier Bay Glenn Highway Haines Harding Gateway Homer Hoonah Hurricane Gulch Inland Passage Inside Passage Isabel Pass Juneau Katmai National Monument Kenai Kenai Lake Kenai Peninsula Kenai River Kechikan Ketchikan Creek Kodiak Kodiak Island Kotzebue Lake Atlin Lake Bennett Latouche Lynn Canal Matanuska Valley McKinley Park Mendenhall Glacier Miles Canyon Montgomery Mount Blackburn Mount Dewey Mount McKinley Mount McKinley Park Mount O’Neal Mount Sanford Muir Glacier Nome North Slope Noyes Island Nushagak Opelika Palmer Petersburg Pribilof Island Resurrection Bay Richardson Highway Rocy Point St. Michael Sawtooth Mountain Sentinal Island Seward Sitka Sitka National Park Skagway Southeastern Alaska Stikine Rier Sulzer Summit Swift Current Taku Glacier Taku Inlet Taku Lodge Tanana Tanana River Tok Tunnel Mountain Valdez White Pass Whitehorse Wrangell Wrangell Narrow Yukon Yukon River General Views—no specific location Alabama Albany Albertville Alexander City Andalusia Anniston Ashford Athens Attalla Auburn Batesville Bessemer Birmingham Blue Lake Blue Springs Boaz Bobler’s Creek Boyles Brewton Bridgeport Camden Camp Hill Camp Rucker Carbon Hill Castleberry Centerville Centre Chapman Chattahoochee Valley Cheaha State Park Choctaw County
    [Show full text]