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Lunar Impact Crater Identification and Age Estimation with Chang’E
ARTICLE https://doi.org/10.1038/s41467-020-20215-y OPEN Lunar impact crater identification and age estimation with Chang’E data by deep and transfer learning ✉ Chen Yang 1,2 , Haishi Zhao 3, Lorenzo Bruzzone4, Jon Atli Benediktsson 5, Yanchun Liang3, Bin Liu 2, ✉ ✉ Xingguo Zeng 2, Renchu Guan 3 , Chunlai Li 2 & Ziyuan Ouyang1,2 1234567890():,; Impact craters, which can be considered the lunar equivalent of fossils, are the most dominant lunar surface features and record the history of the Solar System. We address the problem of automatic crater detection and age estimation. From initially small numbers of recognized craters and dated craters, i.e., 7895 and 1411, respectively, we progressively identify new craters and estimate their ages with Chang’E data and stratigraphic information by transfer learning using deep neural networks. This results in the identification of 109,956 new craters, which is more than a dozen times greater than the initial number of recognized craters. The formation systems of 18,996 newly detected craters larger than 8 km are esti- mated. Here, a new lunar crater database for the mid- and low-latitude regions of the Moon is derived and distributed to the planetary community together with the related data analysis. 1 College of Earth Sciences, Jilin University, 130061 Changchun, China. 2 Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, 100101 Beijing, China. 3 Key Laboratory of Symbol Computation and Knowledge Engineering of Ministry of Education, College of Computer Science and Technology, Jilin University, 130012 Changchun, China. 4 Department of Information Engineering and Computer ✉ Science, University of Trento, I-38122 Trento, Italy. -
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. -
Planetary Surfaces
Chapter 4 PLANETARY SURFACES 4.1 The Absence of Bedrock A striking and obvious observation is that at full Moon, the lunar surface is bright from limb to limb, with only limited darkening toward the edges. Since this effect is not consistent with the intensity of light reflected from a smooth sphere, pre-Apollo observers concluded that the upper surface was porous on a centimeter scale and had the properties of dust. The thickness of the dust layer was a critical question for landing on the surface. The general view was that a layer a few meters thick of rubble and dust from the meteorite bombardment covered the surface. Alternative views called for kilometer thicknesses of fine dust, filling the maria. The unmanned missions, notably Surveyor, resolved questions about the nature and bearing strength of the surface. However, a somewhat surprising feature of the lunar surface was the completeness of the mantle or blanket of debris. Bedrock exposures are extremely rare, the occurrence in the wall of Hadley Rille (Fig. 6.6) being the only one which was observed closely during the Apollo missions. Fragments of rock excavated during meteorite impact are, of course, common, and provided both samples and evidence of co,mpetent rock layers at shallow levels in the mare basins. Freshly exposed surface material (e.g., bright rays from craters such as Tycho) darken with time due mainly to the production of glass during micro- meteorite impacts. Since some magnetic anomalies correlate with unusually bright regions, the solar wind bombardment (which is strongly deflected by the magnetic anomalies) may also be responsible for darkening the surface [I]. -
Workshop on Lunar Volcanic Glasses: Scientific and Resource Potential
WORKSHOP ON LUNAR VOLCANIC GLASSES: SCIENTIFIC AND RESOURCE POTENTIAL t)--- LPI Technical Report Number 90~02 .. LUNAR AND PLANETARY INSTITUTE 3303 NASA ROAD 1 HOUSTON, TEXAS 77058-4399 WORKSHOP ON LUNAR VOLCANIC GLASSES: SCIENTIFIC AND RESOlTRCE POTENTIAL Edited by John W. Delano and Grant H. Heiken Held at Lunar and Planetary Institute Houston, Texas October 10 - 11, 1989 Sponsored by Lunar and Planetary Institute Lunar and Planetary Sample Team Lunar and Planetary Institute 3303 NASA Road 1 Houston, Texas 77058-4399 LPI Technical Report Number 90-02 Compiled in 1990 by the LUNAR AND PLANETARY INSTITUTE The Institute is operated by Universities Space Research Association under Contract NASW-4066 with the National Aeronautics and Space Administration. Material in this document may be copied without restraint for library, abstract service, educational, or personal research purposes; however, republication of any portion requires the written permission of the authors as well as appropriate acknowledgment of this publication. This report may be cited as: Delano J. W. and Heiken G. H., eds. (1990) Workshop on Lunar Volcanic Glasses: Scientific alld Resource Potelltial. LPI Tech. Rpt. 90-02. Lunar and Planetary Institute, Houston. 74 pp. Papers in this report may be cited as: Author A. A. (1990) Title of paper. In Workshop Oil Lunar Volcanic Glasses: Scientific alld Resource Potelltial (J. W. Delano and G. H. Heiken, eds.), pp. xx-yy. LPI Tech. Rpt. 90-02. Lunar and Planetary Institute, Houston. This report is distributed by: ORDER DEPARTMENT Lunar and Planetary Institute 3303 NASA Road 1 Houston, TX 77058-4399 Mail order requestors will be ill voiced for the cost ofshippillg and halldling. -
A 1 Case-PR/ }*Rciofft.;Is Report
.A 1 case-PR/ }*rciofft.;is Report (a) This eruption site on Mauna Loa Volcano was the main source of the voluminous lavas that flowed two- thirds of the distance to the town of Hilo (20 km). In the interior of the lava fountains, the white-orange color indicates maximum temperatures of about 1120°C; deeper orange in both the fountains and flows reflects decreasing temperatures (<1100°C) at edges and the surface. (b) High winds swept the exposed ridges, and the filter cannister was changed in the shelter of a p^hoehoc (lava) ridge to protect the sample from gas contamination. (c) Because of the high temperatures and acid gases, special clothing and equipment was necessary to protect the eyes. nose, lungs, and skin. Safety features included military flight suits of nonflammable fabric, fuil-face respirators that are equipped with dual acidic gas filters (purple attachments), hard hats, heavy, thick-soled boots, and protective gloves. We used portable radios to keep in touch with the Hawaii Volcano Observatory, where the area's seismic activity was monitored continuously. (d) Spatter activity in the Pu'u O Vent during the January 1984 eruption of Kilauea Volcano. Magma visible in the circular conduit oscillated in a piston-like fashion; spatter was ejected to heights of 1 to 10 m. During this activity, we sampled gases continuously for 5 hours at the west edge. Cover photo: This aerial view of Kilauea Volcano was taken in April 1984 during overflights to collect gas samples from the plume. The bluish portion of the gas plume contained a far higher density of fine-grained scoria (ash). -
CALIFORNIA's NORTH COAST: a Literary Watershed: Charting the Publications of the Region's Small Presses and Regional Authors
CALIFORNIA'S NORTH COAST: A Literary Watershed: Charting the Publications of the Region's Small Presses and Regional Authors. A Geographically Arranged Bibliography focused on the Regional Small Presses and Local Authors of the North Coast of California. First Edition, 2010. John Sherlock Rare Books and Special Collections Librarian University of California, Davis. 1 Table of Contents I. NORTH COAST PRESSES. pp. 3 - 90 DEL NORTE COUNTY. CITIES: Crescent City. HUMBOLDT COUNTY. CITIES: Arcata, Bayside, Blue Lake, Carlotta, Cutten, Eureka, Fortuna, Garberville Hoopa, Hydesville, Korbel, McKinleyville, Miranda, Myers Flat., Orick, Petrolia, Redway, Trinidad, Whitethorn. TRINITY COUNTY CITIES: Junction City, Weaverville LAKE COUNTY CITIES: Clearlake, Clearlake Park, Cobb, Kelseyville, Lakeport, Lower Lake, Middleton, Upper Lake, Wilbur Springs MENDOCINO COUNTY CITIES: Albion, Boonville, Calpella, Caspar, Comptche, Covelo, Elk, Fort Bragg, Gualala, Little River, Mendocino, Navarro, Philo, Point Arena, Talmage, Ukiah, Westport, Willits SONOMA COUNTY. CITIES: Bodega Bay, Boyes Hot Springs, Cazadero, Cloverdale, Cotati, Forestville Geyserville, Glen Ellen, Graton, Guerneville, Healdsburg, Kenwood, Korbel, Monte Rio, Penngrove, Petaluma, Rohnert Part, Santa Rosa, Sebastopol, Sonoma Vineburg NAPA COUNTY CITIES: Angwin, Calistoga, Deer Park, Rutherford, St. Helena, Yountville MARIN COUNTY. CITIES: Belvedere, Bolinas, Corte Madera, Fairfax, Greenbrae, Inverness, Kentfield, Larkspur, Marin City, Mill Valley, Novato, Point Reyes, Point Reyes Station, Ross, San Anselmo, San Geronimo, San Quentin, San Rafael, Sausalito, Stinson Beach, Tiburon, Tomales, Woodacre II. NORTH COAST AUTHORS. pp. 91 - 120 -- Alphabetically Arranged 2 I. NORTH COAST PRESSES DEL NORTE COUNTY. CRESCENT CITY. ARTS-IN-CORRECTIONS PROGRAM (Crescent City). The Brief Pelican: Anthology of Prison Writing, 1993. 1992 Pelikanesis: Creative Writing Anthology, 1994. 1994 Virtual Pelican: anthology of writing by inmates from Pelican Bay State Prison. -
GRAIL Twins Toast New Year from Lunar Orbit
Jet JANUARY Propulsion 2012 Laboratory VOLUME 42 NUMBER 1 GRAIL twins toast new year from Three-month ‘formation flying’ mission will By Mark Whalen lunar orbit study the moon from crust to core Above: The GRAIL team celebrates with cake and apple cider. Right: Celebrating said. “So it does take a lot of planning, a lot of test- the other spacecraft will accelerate towards that moun- GRAIL-A’s Jan. 1 lunar orbit insertion are, from left, Maria Zuber, GRAIL principal ing and then a lot of small maneuvers in order to get tain to measure it. The change in the distance between investigator, Massachusetts Institute of Technology; Charles Elachi, JPL director; ready to set up to get into this big maneuver when we the two is noted, from which gravity can be inferred. Jim Green, NASA director of planetary science. go into orbit around the moon.” One of the things that make GRAIL unique, Hoffman JPL’s Gravity Recovery and Interior Laboratory (GRAIL) A series of engine burns is planned to circularize said, is that it’s the first formation flying of two spacecraft mission celebrated the new year with successful main the twins’ orbit, reducing their orbital period to a little around any body other than Earth. “That’s one of the engine burns to place its twin spacecraft in a perfectly more than two hours before beginning the mission’s biggest challenges we have, and it’s what makes this an synchronized orbit around the moon. 82-day science phase. “If these all go as planned, we exciting mission,” he said. -
New Lunar Impact Melt Flows As Revealed by Mini-Rf on Lro
43rd Lunar and Planetary Science Conference (2012) 2388.pdf NEW LUNAR IMPACT MELT FLOWS AS REVEALED BY MINI-RF ON LRO. C. D. Neish1, N. Glines2, L. M. Carter3, V. J. Bray4, B. R. Hawke5, D. B. J. Bussey1, and the Mini-RF Science Team, 1The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, 20723 ([email protected]), 2Mount Holyoke College, South Hadley, MA, 01075, 3NASA Goddard Spaceflight Center, Greenbelt, MD, 20770, 4The University of Ari- zona, Tucson, AZ, 85721, 5The University of Hawai’i at Manoa, Honolulu, HI, 96822. Introduction: Flow-like deposits of impact melt fying impact melts. After a candidate melt is identified, are commonly observed on the Moon, typically around data from the LRO Camera (LROC) was used to iden- young fresh craters. These flows are thought to be mix- tify additional features associated with impact melt tures of clasts and melted material that are emplaced deposits, such as cooling cracks in ponds and tension during the late stages of impact crater formation [1]. cracks in veneers, confirming these features as impact Lunar impact melts have been primarily studied at op- melts. tical wavelengths, but complementary information can be obtained by observing impact melts at radar wave- lengths. Radar data is sensitive to surface and sub- surface roughness, and thus can highlight these rough surface features, even when they not easily seen in optical data due to burial or imperfect lighting condi- tions (Fig. 1). Impact melts have been identified in radar data on the lunar near side [2], but they have yet to be studied in depth on the lunar far side, given the lack of global radar data prior to the launch of NASA’s Mini-RF instrument on the Lunar Reconnaissance Or- biter (LRO) in 2009. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
DESCHUTES NATIONAL FOREST CAMPGROUND STATUS (July 16, 2020)
DESCHUTES NATIONAL FOREST CAMPGROUND STATUS (July 16, 2020) If you have questions, please contact the appropriate Bend-Ft. Rock Ranger District: 541-383-5300 Ranger District (M-F, 8 a.m. to 4:30 p.m.) Sisters Ranger District: 541-549-7700 Crescent Ranger District: 541-433-3200 Open Opening TBD IMPORTANT PLEASE NOTE THE FOLLOWING INFORMATION FOR THIS YEAR! Most campgrounds moved to 100% reservations to decrease contact between hosts and visitors. People are encouraged to make reservations ahead of time. Reservations can be made at Recreation.gov. Sites are available with a two-day booking window, excepts sites in the Newberry National Volcanic Monument that have a three-day booking window. The booking window is how far in advance you can book the site. Any sites not reserved will be "first-come, first-serve;" however, if you are using a “first-come, first-serve” site you will have to leave the site by the date of an incoming reservation shown on the placard. BEND-FT ROCK RANGER DISTRICT Campgrounds Site Status Water Campfires ONLY Campfires Allowed in Established NEVER allowed Campfire Rings Big Cove Boat-In Campground Open No No campfires Chief Paulina Horse Camp Open Yes Cinder Hill Campground Open Yes Crane Prairie Campground Open (Partial) Yes Yes Cultus Lake Campground Open Yes Yes Devils Lake Campground Open No Campfires East Lake Campground Open Yes Elk Lake Campground Open Yes Yes Gull Point Campground Open Yes Yes Lava Lake Campground Open Yes Yes Little Cove Boat-in Campground Open No No campfires Little Cultus Campground Open -
TRANSFLO Express Scan Station Locations 4/12/2021 9:00:10 AM
TRANSFLO Express Scan Station Locations 4/12/2021 9:00:10 AM Store Company Name Address City State Interstate Number FJ792 Flying J 1260 Cassils Road East Brooks AB 1260 Cassils Road FJ793 Flying J 4216 72 AVENUE SE Calgary AB 72 Ave SE FJ848 Flying J 4949 Barlow Trail SE Calgary AB Barlow Trail FJ785 Flying J 11511 - 40 St. S.E Calgary AB 11511 40th Street SE FJ850 Flying J 16806 118 Ave Edmonton AB 118 Ave FJ846 Flying J Hwy 9 & Hwy 36 South Hanna AB Hwy 9 & Hwy 36 South FJ868 Flying J 2194 Saamis Drive Medicine Hat AB PK868 Pilot Travel Center Kiosk 2194 Saamis Drive Medicine Hat AB FJ869 Flying J 2810 21st Avenue, TOL 1R0 Nanton AB HWY-2 N. FJ795 Flying J 302 20 AVENUE Nisku AB 302 20th Ave FJ796 Flying J 6607 67th Street Red Deer AB 67th Ave. & 67 St PK786 Pilot Travel Center Kiosk 50 Pembina Rd. Sherwood Park AB Hwy 16 PK824 Pilot Travel Center Kiosk 5329 Govenlock Mountain Whitecourt AB Hwy 43 Road FJ824 Flying J 5329 Govenlock Mountain Whitecourt AB hWY 43 Road PT1030 Pilot Travelcenters 12680 South Kedzie ave Alsip AL I-57,Exit 353 PK602 Pilot Travel Center Kiosk 224 Daniel Payne Drive Birmingham AL I-65 & SR 94, Exit 2 PT369 Pilot Travelcenters 901 Bankhead Highway West Birmingham AL I-20/59/65 AL78 X123 FJ602 Flying J 224 Daniel Payne Drive Birmingham AL I-65&SR 94, Exit 264 PK369 Pilot Travel Center Kiosk 901 Bankhead Highway West Birmingham AL I-20/59/65 AL78 X123 LV368 Love's Travel Stops & Country Stores I-65, Exit 208 Clanton AL I-65, Exit 208 PK4555 Pilot Travel Center Kiosk 3201 Buttermilk Rd Cottondale AL I-59 & I-20 Exit 77 TA016 Travel Centers of America 3501 Buttermilk Road Cottondale AL I-20, Exit 77 AB104 Ambest, Inc. -
Secondary Craters on Europa and Implications for Cratered Surfaces
Vol 437|20 October 2005|doi:10.1038/nature04069 LETTERS Secondary craters on Europa and implications for cratered surfaces Edward B. Bierhaus1, Clark R. Chapman2 & William J. Merline2 For several decades, most planetary researchers have regarded the craters were typically not spatially random, but instead appeared in impact crater populations on solid-surfaced planets and smaller clumps and clusters16 even at distances far (several hundred kilo- bodies as predominantly reflecting the direct (‘primary’) impacts metres) from the nearest large primary crater. This clustered spatial of asteroids and comets1. Estimates of the relative and absolute distribution contrasts with primary impacts, which are spatially ages of geological units on these objects have been based on this random. The low spatial density and unusual non-random spatial assumption2. Here we present an analysis of the comparatively distribution of Europa’s small craters enabled us to achieve what has sparse crater population on Jupiter’s icy moon Europa and suggest been previously difficult, namely unambiguous identification and that this assumption is incorrect for small craters. We find that quantification of the contribution of distant secondary craters to the ‘secondaries’ (craters formed by material ejected from large total crater SFD. This, in turn, allows us to re-examine the overall primary impact craters) comprise about 95 per cent of the small crater age-dating methodology. We discuss the specifics of the craters (diameters less than 1 km) on Europa. We therefore con- Europa data first. clude that large primary impacts into a solid surface (for example, We measured more than 17,000 craters in 87 low-compression, ice or rock) produce far more secondaries than previously low-sun, high-resolution Europa images (scales ,60 m pixel21), believed, implying that the small crater populations on the which cover nine regions totalling 0.2% of Europa’s surface (a much Moon, Mars and other large bodies must be dominated by larger percentage of Europa has been imaged at lower resolutions), secondaries.