19720020236.Pdf
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Handbook of Iron Meteorites, Volume 3
Sierra Blanca - Sierra Gorda 1119 ing that created an incipient recrystallization and a few COLLECTIONS other anomalous features in Sierra Blanca. Washington (17 .3 kg), Ferry Building, San Francisco (about 7 kg), Chicago (550 g), New York (315 g), Ann Arbor (165 g). The original mass evidently weighed at least Sierra Gorda, Antofagasta, Chile 26 kg. 22°54's, 69°21 'w Hexahedrite, H. Single crystal larger than 14 em. Decorated Neu DESCRIPTION mann bands. HV 205± 15. According to Roy S. Clarke (personal communication) Group IIA . 5.48% Ni, 0.5 3% Co, 0.23% P, 61 ppm Ga, 170 ppm Ge, the main mass now weighs 16.3 kg and measures 22 x 15 x 43 ppm Ir. 13 em. A large end piece of 7 kg and several slices have been removed, leaving a cut surface of 17 x 10 em. The mass has HISTORY a relatively smooth domed surface (22 x 15 em) overlying a A mass was found at the coordinates given above, on concave surface with irregular depressions, from a few em the railway between Calama and Antofagasta, close to to 8 em in length. There is a series of what appears to be Sierra Gorda, the location of a silver mine (E.P. Henderson chisel marks around the center of the domed surface over 1939; as quoted by Hey 1966: 448). Henderson (1941a) an area of 6 x 7 em. Other small areas on the edges of the gave slightly different coordinates and an analysis; but since specimen could also be the result of hammering; but the he assumed Sierra Gorda to be just another of the North damage is only superficial, and artificial reheating has not Chilean hexahedrites, no further description was given. -
No. 40. the System of Lunar Craters, Quadrant Ii Alice P
NO. 40. THE SYSTEM OF LUNAR CRATERS, QUADRANT II by D. W. G. ARTHUR, ALICE P. AGNIERAY, RUTH A. HORVATH ,tl l C.A. WOOD AND C. R. CHAPMAN \_9 (_ /_) March 14, 1964 ABSTRACT The designation, diameter, position, central-peak information, and state of completeness arc listed for each discernible crater in the second lunar quadrant with a diameter exceeding 3.5 km. The catalog contains more than 2,000 items and is illustrated by a map in 11 sections. his Communication is the second part of The However, since we also have suppressed many Greek System of Lunar Craters, which is a catalog in letters used by these authorities, there was need for four parts of all craters recognizable with reasonable some care in the incorporation of new letters to certainty on photographs and having diameters avoid confusion. Accordingly, the Greek letters greater than 3.5 kilometers. Thus it is a continua- added by us are always different from those that tion of Comm. LPL No. 30 of September 1963. The have been suppressed. Observers who wish may use format is the same except for some minor changes the omitted symbols of Blagg and Miiller without to improve clarity and legibility. The information in fear of ambiguity. the text of Comm. LPL No. 30 therefore applies to The photographic coverage of the second quad- this Communication also. rant is by no means uniform in quality, and certain Some of the minor changes mentioned above phases are not well represented. Thus for small cra- have been introduced because of the particular ters in certain longitudes there are no good determi- nature of the second lunar quadrant, most of which nations of the diameters, and our values are little is covered by the dark areas Mare Imbrium and better than rough estimates. -
Sulfide/Silicate Melt Partitioning During Enstatite Chondrite Melting
61st Annual Meteoritical Society Meeting 5255.pdf SULFIDE/SILICATE MELT PARTITIONING DURING ENSTATITE CHONDRITE MELTING. C. Floss1, R. A. Fogel2, G. Crozaz1, M. Weisberg2, and M. Prinz2, 1McDonnell Center for the Space Sciences and Department of Earth and Planetary Sciences, Washington University, St. Louis MO 63130, USA ([email protected]), 2American Museum of Natural History, Department of Earth and Planetary Sciences, New York NY 10024, USA. Introduction: Aubrites are igneous rocks thought (present only in CaS-saturated charges) has a flat REE to have formed from an enstatite chondrite-like pattern with abundances of about 0.5 x CI. precursor [1]. Yet their origin remains poorly Discussion: Oldhamite/glass D values are close to understood, at least partly because of confusion over 1 for most REE, consistent with previous results the role played by sulfides, particularly oldhamite. [4,5,6], and significantly lower than those expected CaS in aubrites contains high rare earth element based on REE abundances in aubritic oldhamite. In (REE) abundances and exhibits a variety of patterns contrast, D values for FeS are surprisingly high (from [2] that reflect, to some extent, those seen in about 0.1 to 1), given the low REE abundances of oldhamite from enstatite chondrites [3]. However, natural troilite. FeS/silicate partition coefficients experimental work suggests that CaS/silicate melt reported by [5] are somewhat lower, but exhibit a REE partition coefficients are too low to account for similar pattern. Alkali loss from the charges, the high abundances observed [4,5] and do not explain resulting in Ca-enriched glass, might provide a partial the variable patterns. -
January 2019 Cardanus & Krafft
A PUBLICATION OF THE LUNAR SECTION OF THE A.L.P.O. EDITED BY: Wayne Bailey [email protected] 17 Autumn Lane, Sewell, NJ 08080 RECENT BACK ISSUES: http://moon.scopesandscapes.com/tlo_back.html FEATURE OF THE MONTH – JANUARY 2019 CARDANUS & KRAFFT Sketch and text by Robert H. Hays, Jr. - Worth, Illinois, USA September 24, 2018 04:40-05:04 UT, 15 cm refl, 170x, seeing 7/10, transparence 6/6. I drew these craters and vicinity on the night of Sept. 23/24, 2018. The moon was about 22 hours before full. This area is in far western Oceanus Procellarum, and was favorably placed for observation that night. Cardanus is the southern one of this pair and is of moderate depth. Krafft to the north is practically identical in size, and is perhaps slightly deeper. Neither crater has a central peak. Several small craters are near and within Krafft. The crater just outside the southeast rim of Krafft is Krafft E, and Krafft C is nearby within Krafft. The small pit to the west is Krafft K, and Krafft D is between Krafft and Cardanus. Krafft C, D and E are similar sized, but K is smaller than these. A triangular-shaped swelling protrudes from the north side of Krafft. The tiny pit, even smaller than Krafft K, east of Cardanus is Cardanus E. There is a dusky area along the southwest side of Cardanus. Two short dark strips in this area may be part of the broken ring Cardanus R as shown on the. Lunar Quadrant map. -
Special Catalogue Milestones of Lunar Mapping and Photography Four Centuries of Selenography on the Occasion of the 50Th Anniversary of Apollo 11 Moon Landing
Special Catalogue Milestones of Lunar Mapping and Photography Four Centuries of Selenography On the occasion of the 50th anniversary of Apollo 11 moon landing Please note: A specific item in this catalogue may be sold or is on hold if the provided link to our online inventory (by clicking on the blue-highlighted author name) doesn't work! Milestones of Science Books phone +49 (0) 177 – 2 41 0006 www.milestone-books.de [email protected] Member of ILAB and VDA Catalogue 07-2019 Copyright © 2019 Milestones of Science Books. All rights reserved Page 2 of 71 Authors in Chronological Order Author Year No. Author Year No. BIRT, William 1869 7 SCHEINER, Christoph 1614 72 PROCTOR, Richard 1873 66 WILKINS, John 1640 87 NASMYTH, James 1874 58, 59, 60, 61 SCHYRLEUS DE RHEITA, Anton 1645 77 NEISON, Edmund 1876 62, 63 HEVELIUS, Johannes 1647 29 LOHRMANN, Wilhelm 1878 42, 43, 44 RICCIOLI, Giambattista 1651 67 SCHMIDT, Johann 1878 75 GALILEI, Galileo 1653 22 WEINEK, Ladislaus 1885 84 KIRCHER, Athanasius 1660 31 PRINZ, Wilhelm 1894 65 CHERUBIN D'ORLEANS, Capuchin 1671 8 ELGER, Thomas Gwyn 1895 15 EIMMART, Georg Christoph 1696 14 FAUTH, Philipp 1895 17 KEILL, John 1718 30 KRIEGER, Johann 1898 33 BIANCHINI, Francesco 1728 6 LOEWY, Maurice 1899 39, 40 DOPPELMAYR, Johann Gabriel 1730 11 FRANZ, Julius Heinrich 1901 21 MAUPERTUIS, Pierre Louis 1741 50 PICKERING, William 1904 64 WOLFF, Christian von 1747 88 FAUTH, Philipp 1907 18 CLAIRAUT, Alexis-Claude 1765 9 GOODACRE, Walter 1910 23 MAYER, Johann Tobias 1770 51 KRIEGER, Johann 1912 34 SAVOY, Gaspare 1770 71 LE MORVAN, Charles 1914 37 EULER, Leonhard 1772 16 WEGENER, Alfred 1921 83 MAYER, Johann Tobias 1775 52 GOODACRE, Walter 1931 24 SCHRÖTER, Johann Hieronymus 1791 76 FAUTH, Philipp 1932 19 GRUITHUISEN, Franz von Paula 1825 25 WILKINS, Hugh Percy 1937 86 LOHRMANN, Wilhelm Gotthelf 1824 41 USSR ACADEMY 1959 1 BEER, Wilhelm 1834 4 ARTHUR, David 1960 3 BEER, Wilhelm 1837 5 HACKMAN, Robert 1960 27 MÄDLER, Johann Heinrich 1837 49 KUIPER Gerard P. -
Feature of the Month - August 2006
RECENT BACK ISSUES: http://www.zone-vx.com/tlo_back.html A PUBLICATION OF THE LUNAR SECTION OF THE A.L.P.O. EDITED BY: William M. Dembowski, F.R.A.S. - [email protected] Elton Moonshine Observatory - http://www.zone-vx.com 219 Old Bedford Pike (Elton) - Windber, PA 15963 FEATURE OF THE MONTH - AUGUST 2006 RHEITA E Sketch and text by Robert H. Hays, Jr. - Worth, Illinois, USA March 5, 200 - 01:15 to 01:45 UT 15cm Newtonian - 170x - Seeing 7-8/10 I sketched this crater and vicinity on the evening of March 4, 2006 after observing two occultations. This feature is located amid a jumble of craters south of Mare Fecunditatis. This is an elongated crater that appears to be the result of at least three impacts. The north and south lobes are about the same size, but the southern lobe is definitely deeper. The central portion is about the size of the north and south lobes combined. There are some bits of shadow on the floor, but I saw no obvious hills or craters there. I have drawn the shadowing within and around Rheita E as I saw it. There is an obvious ridge extending westward from the south lobe. The crater Rheita F is adjacent to the south lobe of Rheita E, and has a strip of shadow parallel to the ridge from Rheita E. Rheita M is the large, shallow crater east of Rheita E's south end, and Rheita N is the small, shallow pit between them. Stevinus D is the slightly smaller, but deeper crater north of Rheita M. -
Handbook of Iron Meteorites, Volume 2 (Canyon Diablo, Part 2)
Canyon Diablo 395 The primary structure is as before. However, the kamacite has been briefly reheated above 600° C and has recrystallized throughout the sample. The new grains are unequilibrated, serrated and have hardnesses of 145-210. The previous Neumann bands are still plainly visible , and so are the old subboundaries because the original precipitates delineate their locations. The schreibersite and cohenite crystals are still monocrystalline, and there are no reaction rims around them. The troilite is micromelted , usually to a somewhat larger extent than is present in I-III. Severe shear zones, 100-200 J1 wide , cross the entire specimens. They are wavy, fan out, coalesce again , and may displace taenite, plessite and minerals several millimeters. The present exterior surfaces of the slugs and wedge-shaped masses have no doubt been produced in a similar fashion by shear-rupture and have later become corroded. Figure 469. Canyon Diablo (Copenhagen no. 18463). Shock The taenite rims and lamellae are dirty-brownish, with annealed stage VI . Typical matte structure, with some co henite crystals to the right. Etched. Scale bar 2 mm. low hardnesses, 160-200, due to annealing. In crossed Nicols the taenite displays an unusual sheen from many small crystals, each 5-10 J1 across. This kind of material is believed to represent shock annealed fragments of the impacting main body. Since the fragments have not had a very long flight through the atmosphere, well developed fusion crusts and heat-affected rim zones are not expected to be present. The energy responsible for bulk reheating of the small masses to about 600° C is believed to have come from the conversion of kinetic to heat energy during the impact and fragmentation. -
Mobility Statistics and Automated Hazard Mapping for Debris Flows and Rock Avalanches
Mobility Statistics and Automated Hazard Mapping for Debris Flows and Rock Avalanches Scientific Investigations Report 2007–5276 Version 1.1 U.S. Department of the Interior U.S. Geological Survey Mobility Statistics and Automated Hazard Mapping for Debris Flows and Rock Avalanches By Julia P. Griswold and Richard M. Iverson Scientific Investigations Report 2007–5276 Version 1.1 U.S. Department of the Interior U.S. Geological Survey U.S. Department of the Interior DIRK KEMPTHORNE, Secretary U.S. Geological Survey Mark D. Myers, Director U.S. Geological Survey, Reston, Virginia: 2008 Revised 2014 This report and any updates to it are available at: http://pubs.usgs.gov/sir/2007/5276/ For product and ordering information: World Wide Web: http://www.usgs.gov/pubprod Telephone: 1-888-ASK-USGS For more information on the USGS--the Federal source for science about the Earth, its natural and living resources, natural hazards, and the environment: World Wide Web: http://www.usgs.gov Telephone: 1-888-ASK-USGS Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. Government. Although this report is in the public domain, permission must be secured from the individual copyright owners to reproduce any copyrighted materials contained within this report. Suggested citation: Griswold, J.P., and Iverson, R.M., 2008, Mobility statistics and automated hazard mapping for debris flows and rock avalanches (ver. 1.1, April 2014): U.S. Geological Survey Scientific Investigations Report 2007-5276, 59 p. Manuscript approved for publication, December 12, 2007 Text edited by Tracey L. -
By DWG Arthur, Alice P. Agnieray, Ruth H. Pellicori, CA Wood, and T
No. 50 THE SYSTEM OF LUNAR CRATERS, QUADRANT III by D. W. G. Arthur, Alice P. Agnieray, Ruth H. Pellicori, C. A. Wood, and T. Weller February 25, 1965 ABSTRACT The designation, diameter, position, central peak information, and state of completeness are listed for each discernible crater with a diameter exceeding 3.5 km in the third lunar quadrant. The catalog contains about 5200 items and is illustrated by a map in 11 sections. on the averted lunar hemisphere, and therefore, these Thistem Communication of Lunar Craters, is the which third is part a catalog of The in Sys four are not listed in the catalog. parts of all craters recognizable with reasonable The approximate positions and diameters for certainty on photographs and having a diameter these craters are: greater than 3.5 km. It is thus a continuation of the work in Comm. LPL Nos. 30 and 40, and the same Long. Lat. Diam, (.00Ir) Hausen -91?5 - 6 5 ? 6 9 9 . 5 conventions and format are used. Boltzmann -96?0 - 7 5 ? 5 3 9 . 1 As in the earlier parts, it was found necessary S t e f a n - 9 4 ? 0 - 7 2 ? 0 7 8 . 0 to add names for large craters in the extreme limb regions. The new crater names for Quadrant III are: The above are mere additions to the Blagg and Miiller scheme. A more notable innovation, which Baade German-American astronomer has already been authorized by the International Boltzmann Austrian physicist Astronomical Union at its 1964 general meeting at Drygalski German geographer Hamburg, is the addition of the name Mare Cogni- Hartwig German selenodetist tum (the known sea) for the dark area between Krasnov Russian selenodetic observer Riphaeus and the crater Guerike. -
Planetary Science : a Lunar Perspective
APPENDICES APPENDIX I Reference Abbreviations AJS: American Journal of Science Ancient Sun: The Ancient Sun: Fossil Record in the Earth, Moon and Meteorites (Eds. R. 0.Pepin, et al.), Pergamon Press (1980) Geochim. Cosmochim. Acta Suppl. 13 Ap. J.: Astrophysical Journal Apollo 15: The Apollo 1.5 Lunar Samples, Lunar Science Insti- tute, Houston, Texas (1972) Apollo 16 Workshop: Workshop on Apollo 16, LPI Technical Report 81- 01, Lunar and Planetary Institute, Houston (1981) Basaltic Volcanism: Basaltic Volcanism on the Terrestrial Planets, Per- gamon Press (1981) Bull. GSA: Bulletin of the Geological Society of America EOS: EOS, Transactions of the American Geophysical Union EPSL: Earth and Planetary Science Letters GCA: Geochimica et Cosmochimica Acta GRL: Geophysical Research Letters Impact Cratering: Impact and Explosion Cratering (Eds. D. J. Roddy, et al.), 1301 pp., Pergamon Press (1977) JGR: Journal of Geophysical Research LS 111: Lunar Science III (Lunar Science Institute) see extended abstract of Lunar Science Conferences Appendix I1 LS IV: Lunar Science IV (Lunar Science Institute) LS V: Lunar Science V (Lunar Science Institute) LS VI: Lunar Science VI (Lunar Science Institute) LS VII: Lunar Science VII (Lunar Science Institute) LS VIII: Lunar Science VIII (Lunar Science Institute LPS IX: Lunar and Planetary Science IX (Lunar and Plane- tary Institute LPS X: Lunar and Planetary Science X (Lunar and Plane- tary Institute) LPS XI: Lunar and Planetary Science XI (Lunar and Plane- tary Institute) LPS XII: Lunar and Planetary Science XII (Lunar and Planetary Institute) 444 Appendix I Lunar Highlands Crust: Proceedings of the Conference in the Lunar High- lands Crust, 505 pp., Pergamon Press (1980) Geo- chim. -
The Moon After Apollo
ICARUS 25, 495-537 (1975) The Moon after Apollo PAROUK EL-BAZ National Air and Space Museum, Smithsonian Institution, Washington, D.G- 20560 Received September 17, 1974 The Apollo missions have gradually increased our knowledge of the Moon's chemistry, age, and mode of formation of its surface features and materials. Apollo 11 and 12 landings proved that mare materials are volcanic rocks that were derived from deep-seated basaltic melts about 3.7 and 3.2 billion years ago, respec- tively. Later missions provided additional information on lunar mare basalts as well as the older, anorthositic, highland rocks. Data on the chemical make-up of returned samples were extended to larger areas of the Moon by orbiting geo- chemical experiments. These have also mapped inhomogeneities in lunar surface chemistry, including radioactive anomalies on both the near and far sides. Lunar samples and photographs indicate that the moon is a well-preserved museum of ancient impact scars. The crust of the Moon, which was formed about 4.6 billion years ago, was subjected to intensive metamorphism by large impacts. Although bombardment continues to the present day, the rate and size of impact- ing bodies were much greater in the first 0.7 billion years of the Moon's history. The last of the large, circular, multiringed basins occurred about 3.9 billion years ago. These basins, many of which show positive gravity anomalies (mascons), were flooded by volcanic basalts during a period of at least 600 million years. In addition to filling the circular basins, more so on the near side than on the far side, the basalts also covered lowlands and circum-basin troughs. -
Family Group Sheets Surname Index
PASSAIC COUNTY HISTORICAL SOCIETY FAMILY GROUP SHEETS SURNAME INDEX This collection of 660 folders contains over 50,000 family group sheets of families that resided in Passaic and Bergen Counties. These sheets were prepared by volunteers using the Societies various collections of church, ceme tery and bible records as well as city directo ries, county history books, newspaper abstracts and the Mattie Bowman manuscript collection. Example of a typical Family Group Sheet from the collection. PASSAIC COUNTY HISTORICAL SOCIETY FAMILY GROUP SHEETS — SURNAME INDEX A Aldous Anderson Arndt Aartse Aldrich Anderton Arnot Abbott Alenson Andolina Aronsohn Abeel Alesbrook Andreasen Arquhart Abel Alesso Andrews Arrayo Aber Alexander Andriesse (see Anderson) Arrowsmith Abers Alexandra Andruss Arthur Abildgaard Alfano Angell Arthurs Abraham Alje (see Alyea) Anger Aruesman Abrams Aljea (see Alyea) Angland Asbell Abrash Alji (see Alyea) Angle Ash Ack Allabough Anglehart Ashbee Acker Allee Anglin Ashbey Ackerman Allen Angotti Ashe Ackerson Allenan Angus Ashfield Ackert Aller Annan Ashley Acton Allerman Anners Ashman Adair Allibone Anness Ashton Adams Alliegro Annin Ashworth Adamson Allington Anson Asper Adcroft Alliot Anthony Aspinwall Addy Allison Anton Astin Adelman Allman Antoniou Astley Adolf Allmen Apel Astwood Adrian Allyton Appel Atchison Aesben Almgren Apple Ateroft Agar Almond Applebee Atha Ager Alois Applegate Atherly Agnew Alpart Appleton Atherson Ahnert Alper Apsley Atherton Aiken Alsheimer Arbuthnot Atkins Aikman Alterman Archbold Atkinson Aimone