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Appendix I Lunar and Martian Nomenclature
APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei -
Nature of Bright C-Complex Asteroids
Publ. Astron. Soc. Japan (2014) 00(0), 1–20 1 doi: 10.1093/pasj/xxx000 Nature of bright C-complex asteroids Sunao HASEGAWA,1,* Toshihiro KASUGA,2 Fumihiko USUI,3 and Daisuke KURODA4 1Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara 252-5210, Japan 2Public Relations Center, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka-shi, Tokyo 181-8588, Japan 3Center for Planetary Science, Graduate School of Science, Kobe University, 7-1-48, Minatojima-minamimachi, Chuo-Ku, Kobe 650-0047, Japan 4Okayama Astronomical Observatory, Graduate School of Science, Kyoto University, 3037-5 Honjo, Kamogata-cho, Asakuchi, Okayama 719-0232, Japan ∗E-mail: [email protected] Received ; Accepted Abstract Most C-complex asteroids have albedo values less than 0.1, but there are some high-albedo (bright) C-complex asteroids with albedo values exceeding 0.1. To reveal the nature and origin of bright C-complex asteroids, we conducted spectroscopic observations of the asteroids in visible and near-infrared wavelength regions. As a result, the bright B-, C-, and Ch-type (Bus) asteroids, which are subclasses of the Bus C-complex, are classified as DeMeo C-type aster- oids with concave curvature, B-, Xn-, and K-type asteroids. Analogue meteorites and material (CV/CK chondrites, enstatite chondrites/achondrites, and salts) associated with these spec- tral types of asteroids are thought to be composed of minerals and material exposed to high temperatures. A comparison of the results obtained in this study with the SDSS photometric data suggests that salts may have occurred in the parent bodies of 24 Themis and 10 Hygiea, as well as 2 Pallas. -
The 2019 Eruption Dynamics and Morphology at Ebeko Volcano Monitored by Unoccupied Aircraft Systems (UAS) and Field Stations
remote sensing Article The 2019 Eruption Dynamics and Morphology at Ebeko Volcano Monitored by Unoccupied Aircraft Systems (UAS) and Field Stations Thomas R. Walter 1,* , Alexander Belousov 2, Marina Belousova 2, Tatiana Kotenko 2 and Andreas Auer 3 1 Department of Geophysics, GFZ Potsdam, Telegrafenberg, 14473 Potsdam, Germany 2 Institute of Volcanology and Seismology, FED RAS, 683006 Petropavlovsk, Russia; [email protected] (A.B.); [email protected] (M.B.); [email protected] (T.K.) 3 Department of Geoscience, Shimane University, Matsue 690-8504, Japan; [email protected] * Correspondence: [email protected] Received: 20 May 2020; Accepted: 16 June 2020; Published: 18 June 2020 Abstract: Vulcanian explosions are hazardous and are often spontaneous and direct observations are therefore challenging. Ebeko is an active volcano on Paramushir Island, northern Kuril Islands, showing characteristic Vulcanian-type activity. In 2019, we started a comprehensive survey using a combination of field station records and repeated unoccupied aircraft system (UAS) surveys to describe the geomorphological features of the edifice and its evolution during ongoing activity. Seismic data revealed the activity of the volcano and were complemented by monitoring cameras, showing a mean explosion interval of 34 min. Digital terrain data generated from UAS quadcopter photographs allowed for the identification of the dimensions of the craters, a structural architecture and the tephra deposition at cm-scale resolution. The UAS was equipped with a thermal camera, which in combination with the terrain data, allowed it to identify fumaroles, volcano-tectonic structures and vents and generate a catalog of 282 thermal spots. The data provide details on a nested crater complex, aligned NNE-SSW, erupting on the northern rim of the former North Crater. -
Planetary Defense Final Report I
Team Project - Planetary Defense Final Report i Team Project - Planetary Defense Final Report ii Team Project - Planetary Defense Cover designed by: Tihomir Dimitrov Images courtesy of: Earth Image - NASA US Geological Survey Detection Image - ESA's Optical Ground Station Laser Tags ISS Deflection Image - IEEE Space Based Lasers Collaboration Image - United Nations General Assembly Building Outreach Image - Dreamstime teacher with students in classroom Evacuation Image - Libyan City of Syrte destroyed in 2011 Shield Image - Silver metal shield PNG image The cover page was designed to include a visual representation of the roadmap for a robust Planetary Defense Program that includes five elements: detection, deflection, global collaboration, outreach, and evacuation. The shield represents the idea of defending our planet, giving confidence to the general public that the Planetary Defense elements are reliable. The orbit represents the comet threat and how it is handled by the shield, which represents the READI Project. The curved lines used in the background give a sense of flow representing the continuation and further development for Planetary Defense programs after this team project, as we would like for everyone to be involved and take action in this noble task of protecting Earth. The 2015 Space Studies Program of the International Space University was hosted by the Ohio University, Athens, Ohio, USA. While all care has been taken in the preparation of this report, ISU does not take any responsibility for the accuracy of its content. -
Margaritifer Sinus, MC-19
315°E 320°E 325°E 330°E 335°E 340°E 345°E 350°E 355°E 360°E Hydraotes 0° Iamuna Colles 0° . Chaos HYDRAOTES CHAOS Dia-Cau Vallis vi Ra . Camiling Aromatum Chaos Rypin . Uzer Chimbote Mega MERIDIANI PLANUM . IANI MER Opportunity + . v Wicklow Landing Site .Victoria Windfall . Zulanka . Endeavour .Pebas . Tuskegee . Iazu Pinglo . XANTHE Oglala . Miyamoto Bopolu .Ada . Bamba .Locana CHAOS . Bahn . Zarand . .Spry Manti . Tarata Balboa . ARABIA Huancayo . Vaals AUREUM . Groves . Conches _ Sitka . Berseba . Kaid . Chinju Lachute .Manah Rakke CHAOS Airy-0 . Stobs . Byske . -5° . Butte Airy . -5° Kong . Andapa Azusa Timbuktu . Quorn TERRA . Creel . Wink . Innsbruck TERRA A .Kholm M . Daet S A . Ganges .Sfax .Paks H Batoka Chasma C . Rincon I Glide R P AURORAE CHAOS A Arsinoes Chaos C I S R M R N E A E I R F R G A R I T I -10° ColumbiaValles A -10° M Pyrrhae Chaos C H A O S . S Ubud E L L Tigre A Daga V Vallis Valles . MARGARITIFER Eos Mensa EOS CHASMA Beer -15° Morava Valles -15° . Alnif L o i r e Osuga Valles Eos TERRA Chaos Luba Valles Jones . Noord . Cardona Vinogradov Lorica . -20° Polotsk -20° . Kimry Sigli . Lebu S . Kansk . Shambe . Longa . Gagra a Gringauz ma Arda Valles Glazov ra Paraná Valles L a . V Peta d Nitro . a . o Aspen Grójec n . l Guir l e . Campos Roddy s Dollfus V . Loto Erythraeum . a .Echt Golden - Himera Valles . Galu l . Manzi Chaos l Circle . e . Kirsanov . Bentong s .Bend Yegros . Chapais . Singa Honda . -
NATIONAL AERONAUTICS and SPACE ADMINISTRATION M19-Rz" WASHINGTON, D
NASA TECHNICAL MEMORANDUM NASA TM-75035 THE LUNAR NOMENCLATURE: THE REVERSE SIDE OF THE MOON (1961-1973) (NASA-TM-75035) THE LUNAR NOMENCLATURE: N78-11960 THE REVERSE SIDE OF TEE MOON (1961-1973) (National Aeronautics and Space Administration) 111 p HC AO,6/MF A01 Unclas CSCL 03B G3/91 49797 K. Shingareva, G. Burba Translation of "Lunnaya Nomenklatura; Obratnaya storona luny 1961-1973", Academy of Sciences USSR, Institute of Space Research, Moscow, "Nauka" Press, 1977, pp. 1-56 NATIONAL AERONAUTICS AND SPACE ADMINISTRATION M19-rz" WASHINGTON, D. C. 20546 AUGUST 1977 A % STANDARD TITLE PAGE -A R.,ott No0... r 2. Government Accession No. 31 Recipient's Caafog No. NASA TIM-75O35 4.-"irl. and Subtitie 5. Repo;t Dote THE LUNAR NOMENCLATURE: THE REVERSE SIDE OF THE August 1977 MOON (1961-1973) 6. Performing Organization Code 7. Author(s) 8. Performing Organizotion Report No. K,.Shingareva, G'. .Burba o 10. Coit Un t No. 9. Perlform:ng Organization Nome and Address ]I. Contract or Grant .SCITRAN NASw-92791 No. Box 5456 13. T yp of Report end Period Coered Santa Barbara, CA 93108 Translation 12. Sponsoring Agiicy Noms ond Address' Natidnal Aeronautics and Space Administration 34. Sponsoring Agency Code Washington,'.D.C. 20546 15. Supplamortary No9 Translation of "Lunnaya Nomenklatura; Obratnaya storona luny 1961-1973"; Academy of Sciences USSR, Institute of Space Research, Moscow, "Nauka" Press, 1977, pp. Pp- 1-56 16. Abstroct The history of naming the details' of the relief on.the near and reverse sides 6f . the moon .ip examined. The book contains lists "of the naes of crater of the reverse side of the moon in Russian and the Latin .spellings: 17, Key Words (Selected by Author(s)) 18. -
Articles Dans Des Revues À Comité De Lecture
Articles dans des revues à comité de lecture 2012 [ACL005] Barstow Joanna K., Tsang C. C. C., Wilson C. F., Irwin P. G. J., Taylor F. W., McGouldrick Kevin, Drossart [ACL001] Abramowski A., Acero F., Aharonian F., Pierre, Piccioni G., Tellmann Silvia. Models of the global cloud Akhperjanian A. G., Anton G., Balzer A., Barnacka A., Barres de structure on Venus derived from Venus Express observations. Almeida U., Becherini Y., Becker J., Behera B., Benbow W., Icarus, 2012, vol. 217, pp. 542-560. Bernlöhr K., Bochow A., Boisson C., Bolmont J., Bordas P., Bouteilier T., Brucker J., Brun F., Brun P., Bulik T., Büsching I., [ACL006] Barucci Antonella, Belskaya Irina, Fornasier Sonia, Carrigan S., Casanova S., Cerruti M., Chadwick P. M., Fulchignoni Marcello, Clark B. E., Coradini A., Capaccioni F., Charbonnier A., Chaves R. C. G., Cheesebrough A., Chounet Dotto E., Birlan Mirel, Leyrat C., Sierks H., Thomas N., Vincent L.-M., Clapson A. C., Coignet G., Cologna G., Colom Pierre, J. B. Overview of Lutetia's surface composition. Planetary and Conrad J., Coudreau N., Dalton M., Daniel M.K., Davids I. D., Space Science, 2012, vol. 66, pp. 23-30. Degrange B., Deil C., Dickinson H. J., Djannati-Ataï A., Domainko W., Drury L. O.'C., Dubois F., Dubus G., Dutson K., [ACL007] Barucci Antonella, Merlin Frédéric, Perna Davide, Dyks J., Dyrda M., Edwards P., Egberts K., Eger P., Espigat P., Alvarez-Candal A., Müller T., Mommert M., Kiss C., Fornasier Fallon L., Farnier C., Fegan S., Feinstein F., Fernandes M. V., Sonia, Santos-Sanz Pablo, Dotto E. The extra red plutino (55638) Fiasson A., Fontaine G., Förster A., Füßling M., Gallant Y. -
Future of Venus Research and Exploration
Space Sci Rev (2018) 214:89 https://doi.org/10.1007/s11214-018-0528-z Future of Venus Research and Exploration Lori S. Glaze1 · Colin F. Wilson2 · Liudmila V. Zasova3 · Masato Nakamura4 · Sanjay Limaye5 Received: 5 September 2017 / Accepted: 10 July 2018 / Published online: 23 July 2018 © The Author(s) 2018 Abstract Despite the tremendous progress that has been made since the publication of the Venus II book in 1997, many fundamental questions remain concerning Venus’ history, evo- lution and current geologic and atmospheric processes. The international science community has taken several approaches to prioritizing these questions, either through formal processes like the Planetary Decadal Survey in the United States and the Cosmic Vision in Europe, or informally through science definition teams utilized by Japan, Russia, and India. These questions are left to future investigators to address through a broad range of research ap- proaches that include Earth-based observations, laboratory and modeling studies that are based on existing data, and new space flight missions. Many of the highest priority ques- tions for Venus can be answered with new measurements acquired by orbiting or in situ missions that use current technologies, and several plausible implementation concepts have Venus III Edited by Bruno Bézard, Christopher T. Russell, Takehiko Satoh, Suzanne E. Smrekar and Colin F. Wilson B L.S. Glaze [email protected] C.F. Wilson [email protected] L.V. Zasova [email protected] M. Nakamura [email protected] S. Limaye [email protected] 1 NASA Goddard Space Flight Center, Greenbelt, MD, USA 2 Oxford University, Oxford, UK 3 Space Research Institute, IKI RAS, Moscow, Russia 4 Institute of Space and Astronautical Science, JAXA, Sagamihara, Japan 5 University of Wisconsin, Madison, Madison, USA 89 Page 2 of 37 L.S. -
The New Martian Nomenclature of the International Astronomical Union IG
ICARUS 26,85-98 (1975) The New Martian Nomenclature of the International Astronomical Union IG. de VAUCOULEURS, 2J. BLUNCK, 3M. DAVIES, 4A. DOLLFUS, 51. K. KOVAL, 6G. P. KUIPERt, 7H. MASURSKY, 8S. l\HYAMOTO, 9V. I. MOROZ, IOCARL SAGAN, AND IIBRADFORD SMITH 1 Department of Ast·ronomy, University of Texas, Austin, Texas 78712; 2Hamburg, Federal Republic of Germany; 3 RAN D Corporation, Santa Monica, California 90-106 ; 40bservatoire de Par is , 1\1[ eudon, France; 5M ain Astronomical Observatory, [J krainian Academy of Sciences, Kiev, U.S.S.R.; 6 University of Arizona, Tucson, A'rizona 8.ji21; 'U.S. Geological Survey, Flagstaff, Arizona 86001; 8J{tcasan Observatory, Cniversity of Kyoto, Yamashina, Kyoto, Japan; "Lnstitute jor Cosmic Research, Moscow, V.S.S.R.; lOCornell University, Ithaca, New York 14853; 11 University of Arizona, Tucson, Arizona 85721 Received December 30, 1974 A new nomenclature for Martian regions and topographic features uncovered by Mariner 9, as officially adopted by the International Astronomical Union, is described. About 180 craters, generally of diameters >100km, have been named, as well as 13 classes of topographic features designated catena, chasma, dorsum, fossa, labyrinthus, mensa, mons, patera, planit.ia, planum, tholus, vallis, and vastit.as. In addition seven craters and the Kepler Dorsum are named on Phobos, and two craters on Deirnos , Coordinates and maps of each named feature are displayed. In August 1970, a Working Group on some prominent Martian topographic fea- Martian Nomenclature was appointed by tures (with reference to the lists of names J. S. Hall, then President of Commission 16 already submitted by Commission 16 (Physics of the Planets) ofthe International members). -
Upper Limits on the Amplitude of Ultra-High-Frequency Gravitational Waves from Graviton to Photon Conversion
Eur. Phys. J. C manuscript No. (will be inserted by the editor) Upper limits on the amplitude of ultra-high-frequency gravitational waves from graviton to photon conversion A. Ejllia,1, D. Ejlli3, A. M. Cruise2, G. Pisano1, H. Grote1 1Cardiff University, School of Physics and Astronomy, The Parade, Cardiff, CF24 3AA, UK 2Birmingham University, School of Physics and Astronomy, Edgbaston Park Rd, Birmingham B15 2TT, UK 3Department of Physics, Novosibirsk State University, 2 Pirogova Street, Novosibirsk, 630090, Russia the date of receipt and acceptance should be inserted later Abstract In this work, we present the first experimental up- and the abundance of sources facilitated the first detections. per limits on the presence of stochastic gravitational waves Coalescences of compact objects such as black holes and in a frequency band with frequencies above 1 THz. We ex- neutron stars have been detected, and spinning neutron stars, clude gravitational waves in the frequency bands from (2:7 − 14)supernovae× and stochastic signals are likely future sources. 1014 Hz and (5 − 12)×1018 Hz down to a characteristic am- Since in principle, GWs can be emitted at any frequency, min −26 min −28 plitude of hc ≈ 6 × 10 and hc ≈ 5 × 10 at 95% they are expected over many decades of frequency below confidence level, respectively. To obtain these results, we the audio band, but also above it. At lower frequencies, the used data from existing facilities that have been constructed space-based laser interferometer LISA is firmly planned to and operated with the aim of detecting WISPs (weakly in- cover the 0:1 − 10 mHz band [7,8], targeting, for example, teracting slim particles), pointing out that these facilities are black hole and white dwarf binaries. -
Geomorphology
EGU General Assembly 2011 EGU General Assembly 2011 Programme Group Programme GM – Geomorphology Monday, 04 April ........................................................................................................................................................................ 2 GM3.1 ....................................................................................................................................................................................... 2 NH10.4/BG2.18/GM4.4/SSS1.12 .................................................................................................................................................. 3 GM5.1/TS4.9 .............................................................................................................................................................................. 4 NH3.2/GM6.3 ............................................................................................................................................................................ 10 GM8.2 ..................................................................................................................................................................................... 11 GM8.3 ..................................................................................................................................................................................... 12 GM10.1 ................................................................................................................................................................................... -
JUSTIN FILIBERTO PHONE: +1 (281) 486-2118 Lunar and Planetary Institute, USRA EMAIL: [email protected] 3600 Bay Area Blvd
Dr. JUSTIN FILIBERTO PHONE: +1 (281) 486-2118 Lunar and Planetary Institute, USRA EMAIL: [email protected] 3600 Bay Area Blvd. www.JustinFiliberto.com Houston, TX 77058 SUMMARY: • Co-I on a 2020 NASA Discovery Mission currently in Phase-A: DAVINCI+ to Venus • Two current NASA ROSES grants with continuous funding since 2009 • Lead editor of Volatiles in the Martian Crust book (published in 2019) • 61 peer-reviewed publications and 4 book chapters • NASA Planetary Science Advisory Committee (Deputy Chair 2020 – present) 2017 – present • Mars Exploration Analysis Group (MEPAG) Steering Committee 2018 – present • Co-Chair Mars Subcommittee Extraterrestrial Materials Analysis Group (ExMAG; formally CAPTEM) Steering Committee 2019 – present • Associate Editor – American Mineralogist (for the special issue dedicated to Jim Webster) EDUCATION: Ph.D. Geology, 2006, Stony Brook University. Dissertation: Constraints on the Chemistry of Martian Magmas. B.S. Geological Sciences and Marine Science, 2001, University of Miami. Thesis: Volatiles in basaltic glasses from a subglacial volcano in northern British Columbia (Canada): implications for ice sheet thickness and mantle volatiles. PROFESSIONAL EXPERIENCE: Manager for Geology and Petrology, Lunar and Planetary Institute, USRA. 2019 – present Senior Staff Scientist, Lunar and Planetary Institute, USRA. 2018 – present Associate Professor, Southern Illinois University (SIU). 2016 – 2018 Visiting Fellow, The Open University, United Kingdom. 2015 – 2017 Assistant Professor, Southern Illinois University.