John Rombi MAS Committee
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147 MISCELLANEOUS NOTES ASHBUKNHAM DEED No
Archaeologia Cantiana Vol. 63 1950 MISCELLANEOUS NOTES DISCOVERY Off MASONRY ON CASTLE HILL, FOLKESTONE CASTLE HILL, Folkestone, was excavated by Major-General A. H. L. F. Pitt-Rivers about 70 years ago and a report printed in Archceologia Vol. XLVII (1882). His conclusion from the " finds " was that the earthworks were Norman. He found no trace of masonry. In the summer of 1949 a fall of earth exposed a portion of walling about 10 feet long and 3 feet high in the southern face of the causeway across the inner ditch of the " camp." The masonry is of natural flints, chalk blocks, and blocks of iron- impregnated greensand set in coarse mortar. The wall appears to have been originally faced with roughly squared ironstone blocks. Near the base of the exposed wall was found a piece of Roman ridge-tile (imbrex), now in the custody of Folkestone Museum—the association of this may be purely accidental as it was a surface find. The exposed portion of wall showed no sign of Roman brick. It seems to have supported a causeway across the innermost trench round the hill-top. The causeway runs from W. to E. and the exposed wall is on its southern face. This causeway at present carries the main track eastwards from the crest of the hill (which is the centre of the " camp ") and is about the middle of the east-side of the central camp enclosure. The writer intended to carry out excavation during the summer of 1950 but circumstances prevented. The matter is worthy of further investigation. -
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. -
Glossary Glossary
Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts. -
Chester County Marriages Bride Index 1885-1930
Chester County Marriages Bride Index 1885-1930 Bride's Last Name Bride's First Name Bride's Middle Bride's Date of Birth Bride's Age Groom's First Groom's Last Date of Application Date of Marriage Place of Marriage License # Dabney Ruth 47 Arthur Garner October 16, 1929 West Chester 29675 Dabundo Louise 18 Saverio DiMaio December 10, 1925 West Chester 26115.5 Dadley Fannie K 23 Albert Smith April 12, 1916 Toughkenamon 19118 Dagastina LorenzaFebruary 6, 1889 Michele Mastragiolo March 16, 1908 Norristown 13663 Dagne Eva EJuly 8, 1874 Jesse Downs December 27, 1899 West Chester 7490 Dagostina Philomena 18 Nicholas Tuscano August 2, 1925 Phoenixville 25847 D'Agostino Angelina 28 Gabriele Natale April 19, 1915 Norristown 18401 Dague Anna LSeptember 23, 1884 James Porter December 18, 1907 Parkesburg 13097 Dague CoraNovember 10, 1874 Vernon Powell February 10, 1904 Lionville 10244 Dague Lillie AApril 27, 1873 Frederick Gottier April 7, 1902 West Chester 9034 Dague M KatieJanuary 1, 1872 Charles Gantt April 17, 1900 Downington 7673 Dague Mary J 29 Ralph Young March 5, 1921 Coatesville 22856 Dague Sara Ellen 36 Rees Helms October 4, 1922 Honey Brook 23933 Dague Sarah Emma1858 James Eppihimer January 14, 1886 West Chester 104 Dahl Olga G 23 Claude Prettyman January 24, 1925 West Chester 25559 Dahms Elsie Annie 26 Chester Kirkhoff October 31, 1929 Pottstown 29710 Dailey Agnes1859 John McCarthy January 13, 1886 West Chester 084 Dailey Anna 19 Rhinehart Merkt August 14, 1913 Downingtown 17216 Dailey Anna RApril 29, 1877 18 Thomas Argne January 4, 1896 -
Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
Planning a Mission to the Lunar South Pole
Lunar Reconnaissance Orbiter: (Diviner) Audience Planning a Mission to Grades 9-10 the Lunar South Pole Time Recommended 1-2 hours AAAS STANDARDS Learning Objectives: • 12A/H1: Exhibit traits such as curiosity, honesty, open- • Learn about recent discoveries in lunar science. ness, and skepticism when making investigations, and value those traits in others. • Deduce information from various sources of scientific data. • 12E/H4: Insist that the key assumptions and reasoning in • Use critical thinking to compare and evaluate different datasets. any argument—whether one’s own or that of others—be • Participate in team-based decision-making. made explicit; analyze the arguments for flawed assump- • Use logical arguments and supporting information to justify decisions. tions, flawed reasoning, or both; and be critical of the claims if any flaws in the argument are found. • 4A/H3: Increasingly sophisticated technology is used Preparation: to learn about the universe. Visual, radio, and X-ray See teacher procedure for any details. telescopes collect information from across the entire spectrum of electromagnetic waves; computers handle Background Information: data and complicated computations to interpret them; space probes send back data and materials from The Moon’s surface thermal environment is among the most extreme of any remote parts of the solar system; and accelerators give planetary body in the solar system. With no atmosphere to store heat or filter subatomic particles energies that simulate conditions in the Sun’s radiation, midday temperatures on the Moon’s surface can reach the stars and in the early history of the universe before 127°C (hotter than boiling water) whereas at night they can fall as low as stars formed. -
Analysis of Polarimetric Mini-SAR and Mini-RF Datasets for Surface Characterization and Crater Delineation on Moon †
Proceeding Paper Analysis of Polarimetric Mini-SAR and Mini-RF Datasets for Surface Characterization and Crater Delineation on Moon † Himanshu Kumari and Ashutosh Bhardwaj * Photogrammetry and Remote Sensing Department, Indian Institute of Remote Sensing, Dehradun 248001, India; [email protected] * Correspondence: [email protected]; Tel.: +91-9410319433 † Presented at the 3rd International Electronic Conference on Atmospheric Sciences, 16–30 November 2020; Available online: https://ecas2020.sciforum.net/. Abstract: The hybrid polarimetric architecture of Mini-SAR and Mini-RF onboard Indian Chan- drayaan-1 and LRO missions were the first to acquire shadowed polar images of the Lunar surface. This study aimed to characterize the surface properties of Lunar polar and non-polar regions con- taining Haworth, Nobile, Gioja, an unnamed crater, Arago, and Moltke craters and delineate the crater boundaries using a newly emerged approach. The Terrain Mapping Camera (TMC) data of Chandrayaan-1 was found useful for the detection and extraction of precise boundaries of the cra- ters using the ArcGIS Crater tool. The Stokes child parameters estimated from radar backscatter like the degree of polarization (m), the relative phase (δ), Poincare ellipticity (χ) along with the Circular Polarization Ratio (CPR), and decomposition techniques, were used to study the surface attributes of craters. The Eigenvectors and Eigenvalues used to measure entropy and mean alpha showed distinct types of scattering, thus its comparison with m-δ, m-χ gave a profound conclusion to the lunar surface. The dominance of surface scattering confirmed the roughness of rugged material. The results showed the CPR associated with the presence of water ice as well as a dihedral reflection inside the polar craters. -
The Problem of the Brisbane Tuff
50 VoL. XLV., No. 11. The Problem of the Brisbane Tuff. By PROFESSOR H. C. RICHARDS, D. Sc., and W. H. BRYAN, D. Sc. (Department of Geology, University of Queensland). PLATES IV.-VI. ( Accepted for publication by the Roya� Society of Qiu!ensland, 30th November, 1933). · 1. INTRODUCTION. The following paper recor�s an attempt to discover the ongm, and explain the mode of formation of the rock now known as the Brisbane Tuff. While the authors long ago realised that this rock possessed a number of unusual features, their doubts as to its true nature were revived and strengthened when a section showing well developed columnar structure was exposed in the municipal quarry at Windsor some three miles north of the centre of the city of Brisbane. A more detailed examination disclosed other anomalous features, but a search of the literature showed that the characters displayed by the Brisbane Tuff, although rare, were not unique but could be closely paralleled in the "Great Hot Sand Flow" of Alaska and in the "Ignimbrites " of New Zealand, while they also resembled in certain respects the " Nitees ardentes" of Mt. Pelee. In the pages which follow only those features that have a direct bearing on the origin and nature of the Eris bane Tuff will be con sidered. For a more general account the reader is referred. to the paper by Mrs. C. Briggs (1928) published in these proceedings. 2. EARLIER VIEWS AS TO ORIGIN AND MODE OF FORMATION. The rock which is now knpwn as the Eris bane Tuff was first described by Leichhardt (1855) who examined the rock on his visit to Brisbane in 1844. -
Proceedings Geological Society of London
Downloaded from http://jgslegacy.lyellcollection.org/ at University of California-San Diego on February 18, 2016 PROCEEDINGS OF THE GEOLOGICAL SOCIETY OF LONDON. SESSION 1884-851 November 5, 1884. Prof. T. G. Bo~sEY, D.Sc., LL.D., F.R.S., President, in the Chair. William Lower Carter, Esq., B.A., Emmanuel College, Cambridge, was elected a Fellow of the Society. The SECRETARYaunouneed.bhat a water-colour picture of the Hot Springs of Gardiner's River, Yellowstone Park, Wyoming Territory, U.S.A., which was painted on the spot by Thomas Moran, Esq., had been presented to the Society by the artist and A. G. Re"::~aw, Esq., F.G.S. The List of Donations to the Library was read. The following communications were read :-- 1. "On a new Deposit of Pliocene Age at St. Erth, 15 miles east of the Land's End, Cornwall." By S. V. Wood, Esq., F.G.S. 2. "The Cretaceous Beds at Black Ven, near Lyme Regis, with some supplementary remarks on the Blackdown Beds." By the Rev. W. Downes, B.A., F.G.S. 3. "On some Recent Discoveries in the Submerged Forest of Torbay." By D. Pidgeon, Esq., F.G.S. The following specimens were exhibited :- Specimens exhibited by Searles V. Wood, Esq., the Rev. W. Downes, B.A., and D. Pidgeon, Esq., in illustration of their papers. a Downloaded from http://jgslegacy.lyellcollection.org/ at University of California-San Diego on February 18, 2016 PROCEEDINGS OF THE GEOLOGICAL SOCIETY. A worked Flint from the Gravel-beds (? Pleistocene) in the Valley of the Tomb of the Kings, near Luxor (Thebes), Egypt, ex- hibited by John E. -
Preliminary Science Report
7. Photographic Summary of Apollo 77 Mission James H. Sasser The geographical exploration of new frontiers mil Estar polyester base. Ektachrome EF S016S has usually occurred many years before scien- color film on a 2.5-mil Estar polyester base was tists visited and studied the areas in detail. For exposed on the lunar surface. Thc higher speed example, the existence of Antarctica as a conti- of this color film was expected to be more suit- nent was known from the time Charles Wilkes able for lunar surface photography because of explored 1500 miles of the coastline in 1840. tl~elow light levels anticipated and confirmed However, extensive Antarctic exploration did to exist on the lunar surface. Other color 70-mm not begin until the 20th century with the voy- exposures of the Earth and Moon were taken ages of Scott, Amundsen, Shackleton, and Byrd. on Ektachrome MS S036S color reversal film It was not until the International Geophysical on a 2.5-mil Estar polyester base. Year (July 1957 to December 1958) that scien- The 16-mm film taken during lunar module tists from 12 countries began conducting an (LM) descent provided the first accurate knowl- ambitious Antarctic research program. In this edge of the exact landing point on the lunar respect, the first manned lunar exploration was surface. The 70-mm photographs taken on the unique. The scientific experiments were care- lunar surface provided panoramic views of the fully planned, and the astronauts were trained surface near the landed LM and allowed de- as surrogates for scientists representing many tailed topographic mapping of the lunar surface disciplines. -
Ore Bin / Oregon Geology Magazine / Journal
Vol . 36, No . 2 February 1974 STATE OF OREGON DEPARTMENT OF GEOlOGY AND MINERAL INDUSTRIES The Ore Bin Published Monthly By STATE OF OREGON DEPARTMENT OF GEOlOGY AND MINERAL INDUSTRIES Head Office: 1069 State Office Bldg., Portland, Oregon - 97201 Telephone: 229 - 5580 FIELD OFFICES 2033 First Street 521 N . E. "E" Street Baker 97814 Grants Pass 97526 xxxxxxxxxxxxxxxxxxxx Subscription rate - $2.00 per calencbr year Available bock issues $.25 each Second class postage paid at Portland, Oregon GOVERNING SOARD R. W. deWeese, Portland, Chairman Willic:m E. Miller, Bend H. lyle Von Gordon, Grants Pass STATE GEOlOGIST R. E. Corcoran GEOLOGISTS IN CHARGE OF FIELD OFFICES Howard C. Brooks, Boker len Romp, Grants Pass Permission i. granted to reprint information contaiMd herein . Credit given the State of Oregon Oepcrtment af Geology and Min_allndustries fO( compiling this information will be appreciated. State of Oregon The ORE BIN Departmentof Geology Volume 36,No.2 and Mineral Industries 1069 State Office Bldg. February 1974 Portland Oregon 97201 ECONOMICS OF GEOTHERMAL DEVELOPMENT The following article by Dr. RobertW. Rex is the text of his remarks to the Sub-Committee on Energy, Committee on Science and Astronautics, U. S. House of Representatives, on September 18, 1973. This text was previously published in Geothermal Energy, vol. 1, no. 4, December 1973. We are reprinting it in this issue of The ORE BIN because we believe the thoughts expressed are pertinent to Oregon at this time and should have as wide dissemination as possible. Dr. Rex is the President of Republic Geothermal, Inc., Playa del Rey, California. -
GRAIL Reveals Secrets of the Lunar Interior
GRAIL Reveals Secrets of the Lunar Interior — Dr. Patrick J. McGovern, Lunar and Planetary Institute A mini-flotilla of spacecraft sent to the Moon in the past few years by several nations has revealed much about the characteristics of the lunar surface via techniques such as imaging, spectroscopy, and laser ranging. While the achievements of these missions have been impressive, only GRAIL has seen deeply enough to reveal inner secrets that the Moon holds. LRecent Lunar Missions Country Name Launch Date Status ESA Small Missions for Advanced September 27, 2003 Ended with lunar surface impact on Research in Technology-1 (SMART-1) September 3, 2006 USA Acceleration, Reconnection, February 27, 2007 Extension of the THEMIS mission; ended Turbulence and Electrodynamics of in 2012 the Moon’s Interaction with the Sun (ARTEMIS) Japan SELENE (Kaguya) September 14, 2007 Ended with lunar surface impact on June 10, 2009 PChina Chang’e-1 October 24, 2007 Taken out of orbit on March 1, 2009 India Chandrayaan-1 October 22, 2008 Two-year mission; ended after 315 days due to malfunction and loss of contact USA Lunar Reconnaissance Orbiter (LRO) June 18, 2009 Completed one-year primary mission; now in five-year extended mission USA Lunar Crater Observation and June 18, 2009 Ended with lunar surface impact on Sensing Satellite (LCROSS) October 9, 2009 China Chang’e-2 October 1, 2010 Primary mission lasted for six months; extended mission completed flyby of asteroid 4179 Toutatis in December 2012 USA Gravity Recovery and Interior September 10, 2011 Ended with lunar surface impact on I Laboratory (GRAIL) December 17, 2012 To probe deeper, NASA launched the Gravity Recovery and Interior Laboratory (GRAIL) mission: twin spacecraft (named “Ebb” and “Flow” by elementary school students from Montana) flying in formation over the lunar surface, tracking each other to within a sensitivity of 50 nanometers per second, or one- twenty-thousandth of the velocity that a snail moves [1], according to GRAIL Principal Investigator Maria Zuber of the Massachusetts Institute of Technology.