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The symmetry analysis in Sulaiman Esa paintings through Islamic art concept

AIP conference Proceedings 2021年第1期2347卷

作者： W. M. Z. W. Soliana I. Marzuki S. Rushana G. N. Hafiza 1Fine Art Department Faculty of Art and Design Universiti Teknologi MARA Cawangan Kelantan Bukit Ilmu 18500 Machang Kelantan Malaysia 2Fakulti Reka Bentuk Inovatif dan Teknologi Universiti Sultan Zainal Abidin Kampus Gong Badak Terengganu Malaysia 3Textile Deparment Faculty of Art and Design Universiti Teknologi MARA Cawangan Kelantan Bukit Ilmu 18500 Machang Kelantan Malaysia

This study aims to identify the mathematical concept evident in the paintings entitled ‘Mahsuri ii’ (1983) by Sulaiman Esa through symmetry analysis. The objective of this study is to do research on the factors connecting art appreciation aspects by describing the concept of symmetry that exist trough the beauty of pattern design in paintings that exhibits Islamic art images. This study involves creative analysis through a qualitative approach with descriptive inter-disciplinary implementation. Symmetric feature research is performed to classify the pattern design of paintings through the process of symmetry involving repetition. The collection of written and visual data was performed by means of documentation, visual recording, and observation methods to obtain information on the subject, design and meaning of the artwork studied. The research uncovered that aesthetical beauty value in Islamic art images that is defined through mathematical expression became the underlying element in paintings design that applies symmetric pattern design concept. It is not an exaggeration to say that symmetry is the basic principle that has long been a hidden structure underpinning the best works of art ever produced in the history of Islamic art. Research has reported that painting can be seen not only from the art’s formalistic point of view, but also from the ethnomathematical angle, through the application of symmetrical features in the production of artworks. This study presents some of the ethnomathematical and Malay-Muslims discussions in its vast research. This is an implicit innovation element present in every thought of society. Efforts to enrich the scope of probable new possibilities in the field of painting are very meaningful and beneficial for today’s and future generations.

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Shale hydrocarbon analysis based on geochemical and seismic data in North West Java Basin

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AIP conference Proceedings 2018年第1期2023卷

作者： A. Ershad A. Haris A. Usman 1Reservoir Geophysics Graduate Program Department of Physics Faculty of Mathematics and Natural Sciences (FMIPA) Universitas Indonesia Jakarta 10430 Indonesia 2Geology and Geophysics Program Faculty of Mathematics and Natural Sciences (FMIPA) Universitas Indonesia Depok 16424 Indonesia 3New Energy and Green Technology Advisor II Pertamina Upstream Technology Center Jl. Medan Merdeka Timur Jakarta 10110 Indonesia

Nowadays, the energy source necessity such as oil and gas increasing simultaneously with industrial expansion and human beings needed. Unfortunately, the production of oil and gas reveal decrease. The world needs the alternative energy for fulfilment. The energy is called unconventional energy. That one of the unconventional energy is shale hydrocarbon. Unconventional means not conventional. In oil and gas exploration, is known-well that the production is come from reservoir, such as sandstone or limestone that is totally different with this energy. Shale is known in explorations stage as a source rock in petroleum system. Shale in this part become source rock and also reservoir. The objective of this study is to characterize source rock and reservoir, and to justify the shale prospect in this area. Based on the earlier research, Indonesia had big potency for developing it. With willingness of government to research about shale hydrocarbon to create a research it. North West Java Basin, based on earlier research, had shale gas potential in its formation, which is Talang Akar Formation. This research is to find more knowledge about how big of shale potential of Talang Akar Formation in Northwest Java Basin based on seismic data, log data and geochemical analysis. With the comprehensive method and data on this research is expected good result. That potency is estimated with good range reservoir, total organic carbon, and the geometry and shale gas zone formation. Generally, AE Field had good potency based on reservoir character, total organic content and also maturity. The result shows that reservoir prospect is located at southwest of the basin, with average of thickness is 60 meters and wide area ± 205.778.535 meters’ square.

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Coalbed Gas and Shale Gas Resource Prospect of Heyang-Hancheng Area

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IOP conference Series: Earth and Environmental Science 2019年第2期300卷

作者： Min Liang Hui Liang Jinhui Yuan Yuhai Fan Geological Exploration Institute of Aerial Photogrammetry and Remote Sensing Bureau Xi'an 710054 China China Jikan Research Institute of Engineering Investigations and Design co. Ltd. Xi'an 710043 China

As an important coal production area, Heyang-Hancheng has already reached coalbed gas exploration stage. However past study had been focused on coal resources survey; systematic oil gas resources assessment had never been conducted. Based on sediment environment research, this paper using field coal survey data combined with source rock organic geochemistry analysis, argillaceous shale and coalbed aero field absorption and resolve tests, isothermy absorption tests, coalbed gas well logging and gas well logging methods etc. to assess the coalbed gas and shale gas exploration prospects. Resource rock of this area is widely distributed and rich in organic matters, has plenty of type ii kerogen, and its organic maturity reaches post mature dry gas stage; thus, has sound hydrocarbon production potential. Both coalbed gas well-logging and isothermy absorption indicated gas content has reached resource evaluation criteria; both shale gas in-situ desorption and gas well-logging show existence of gas, and the natural gas is mainly methane (CH4) with heavy hydrocarbon ***. Locates at the intersection of Hancheng and Chenghe Mining Area in Weibei Coalfield in Hancheng City and Heyang County, the study area has a width of 20.14km from east to west, length of 22.58km from north to south, with an irregular shape and has a total area of 300km2. The area, rich in coal resources, is an important coal resource producing area with widely distributed coal-bearing construction and good continuity. The loess covers a large part of area, and the bedrock is intermittently exposed along the valley. The structural position is in the turning position of the anti-'S' type head in the Weibei coalfield, which is not conform to the monoclinic structure of the NW or NNW, and the dip angle of the stratum is 3°~7°. The faults are all normal faults, with strike of NE or NEE, usually less than 10 km, the section dips NW, and the fault scale is generally tens of meters to more than 1

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山东招远大尹格庄金矿深部三维可视化建模与定位预测

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矿山工程 2020年第2期8卷 151-164页

作者：李洪奎毛先成汤磊石冰陈国栋张玉波梁太涛韩学林山东省地质科学研究院山东济南自然资源部金矿成矿地质过程与资源利用重点实验室山东济南中南大学地球科学与信息物理学院湖南长沙招金矿业股份有限公司山东招远

山东招远大尹格庄金矿床位于华北板块之胶北隆起区内的招远–平度断裂带(简称招平断裂)中。招平断裂带是沿玲珑花岗岩体和前寒武纪结晶基底岩系的侵入接触带而发展、承生、并经多期构造叠加的一条北东向断裂,既属控矿构造,又是导矿和容... 详细信息

山东招远大尹格庄金矿床位于华北板块之胶北隆起区内的招远–平度断裂带(简称招平断裂)中。招平断裂带是沿玲珑花岗岩体和前寒武纪结晶基底岩系的侵入接触带而发展、承生、并经多期构造叠加的一条北东向断裂,既属控矿构造,又是导矿和容矿构造,大尹格庄金矿床主要产于招平断裂下盘的碎裂状玲珑花岗岩中,在其上盘的基底岩系中亦有分布,为一典型的破碎带蚀变岩型金矿床。本文以大尹格庄金矿田为研究对象,引入三维地质建模(3DGM)及三维可视化技术,研究探索隐伏矿体预测的三维化、定量化及可视化技术,重点突破了复杂地质体三维形态分析、控矿地质因素场模拟、成矿信息三维定量提取等关键技术,初步形成了隐伏矿体三维可视化预测的方法。依据勘探工程数据、矿体圈定规范和成矿地质规律并结合已知的地震、重力、大地电磁等方法获得的各类数据作为研究深部地质构造的基本资料,对深部成矿构造进行了三维重构,对大尹格庄金矿深部进行了矿化空间分析和三维成矿信息提取,开展了三维定量成矿预测,在此基础上建立了三维定量成矿预测模型。在大尹格庄金矿田共圈定了I、ii和Ⅲ号三个可视化立体找矿靶区,为今后深部工作优选区位提供了方向。

关键词：深部成矿三维建模可视化定位预测构造重建金矿床招远大尹格庄

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Entering 'A NEW REALM' of KIBO Payload Operations - Continuous efforts for microgravity experiment environment and lessons learned from real time experiment operations in KIBO -

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Journal of Physics: conference Series 2011年第1期327卷

作者： K Sakagami M Goto S Matsumoto H Ohkuma Utilization Engineering Department Japan Manned Space Systems Corporation 2-1-1 Sengen Tsukuba-shi Ibaraki Japan To whom any correspondence should be addressed Japanese Experiment Module (JEM) Mission Operations and Integration Center Japan Aerospace Exploration Agency 2-1-1 Sengen Tsukuba-shi Ibaraki Japan Institute of Space and Astronautical Science Japan Aerospace Exploration Agency 2-1-1 Sengen Tsukuba-shi Ibaraki Japan Space Station Engineering Department Advanced Engineering Services Co. Ltd. 2-1-1 Sengen Tsukuba-shi Ibaraki Japan

On January 22nd, 2011(JST), KOUNOTORI2 (H-ii Transfer Vehicle: HTV2) was successfully launched from Tanegashima Space Center toward the International Space Station (ISS) and two new JAXA payload racks, Kobairo rack and MSPR (Multi-purpose Small Payload Rack) were transferred to ISS/KIBO (Japanese Experiment Module: JEM). In addition to Saibo rack and Ryutai rack which are already in operation in KIBO, in total 4 Japanese experiment payload racks start operations in KIBO. Then KIBO payload operations embark on a new realm, full utilization phase. While the number and variety of microgravity experiments become increasing, simultaneous operation constraints should be considered to achieve multitask payload operations in ISS/KIBO and ever more complicated cooperative operations between crewmember and flight control team/science team are required. Especially for g-jitter improvement in ISS/KIBO, we have greatly advanced cooperative operations with crewmember in the recent increment based on the microgravity data analysis results. In this paper, newly operating Japanese experiment payloads characteristics and some methods to improve g-jitter environment are introduced from the front line of KIBO payload operations.

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The all-particle cosmic ray energy spectrum measured with HAWC 37

The all-particle cosmic ray energy spectrum measured with HA...

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37th International Cosmic Ray conference, ICRC 2021

作者： Morales-Soto, J.A. Arteaga-Velázquez, J.C. Abeysekara, A.U. Albert, A. Alfaro, R. Alvarez, C. Álvarez, J.D. Angeles Camacho, J.R. Arteaga-Velázquez, J.C. Arunbabu, K.P. Avila Rojas, D. Ayala Solares, H.A. Babu, R. Baghmanyan, V. Barber, A.S. Becerra Gonzalez, J. Belmont-Moreno, E. BenZvi, S.Y. Berley, D. Brisbois, C. Caballero-Mora, K.S. Capistrán, T. Carramiñana, A. Casanova, S. Chaparro-Amaro, O. Cotti, U. Cotzomi, J. Coutiño de León, S. De la Fuente, E. de León, C. Diaz-Cruz, L. Diaz Hernandez, R. Díaz-Vélez, J.C. Dingus, B.L. Durocher, M. DuVernois, M.A. Ellsworth, R.W. Engel, K. Espinoza, C. Fan, K.L. Fang, K. Fernández Alonso, M. Fick, B. Fleischhack, H. Flores, J.L. Fraija, N.I. Garcia, D. García-González, J.A. García-Luna, J.L. García-Torales, G. Garfias, F. Giacinti, G. Goksu, H. González, M.M. Goodman, J.A. Harding, J.P. Hernandez, S. Herzog, I. Hinton, J. Hona, B. Huang, D. Hueyotl-Zahuantitla, F. Hui, C.M. Humensky, B. Hüntemeyer, P. Iriarte, A. Jardin-Blicq, A. Jhee, H. Joshi, V. Kieda, D. Kunde, G.J. Kunwar, S. Lara, A. Lee, J. Lee, W.H. Lennarz, D. León Vargas, H. Linnemann, J. Longinotti, A.L. López-Coto, R. Luis-Raya, G. Lundeen, J. Malone, K. Marandon, V. Martinez, O. Martinez-Castellanos, I. Martínez-Huerta, H. Martínez-Castro, J. Matthews, J.A.J. McEnery, J. Miranda-Romagnoli, P. Morales-Soto, J.A. Moreno, E. Mostafá, M. Nayerhoda, A. Nellen, L. Newbold, M. Nisa, M.U. Noriega-Papaqui, R. Olivera-Nieto, L. Omodei, N. Peisker, A. Pérez Araujo, Y. Pérez-Pérez, E.G. Rho, C.D. Rivière, C. Rosa-Gonzalez, D. Ruiz-Velasco, E. Ryan, J. Salazar, H. Salesa Greus, F. Sandoval, A. Schneider, M. Schoorlemmer, H. Serna-Franco, J. Sinnis, G. Smith, A.J. Springer, R.W. Surajbali, P. Taboada, I. Tanner, M. Tollefson, K. Torres, I. Torres-Escobedo, R. Turner, R. Ureña-Mena, F. Villaseñor, L. Wang, X. Watson, I.J. Weisgarber, T. Werner, F. Willox, E. Wood, J. Yodh, G.B. Zepeda, A. Zhou, H. Instituto de Física y Matemáticas Universidad Michoacana de San Nicolás de Hidalgo Morelia Mexico Centro de Investigación en Computación Instituto Politécnico Nacional Ciudad de México Mexico Physics Department Centro de Investigación y de Estudios Avanzados del IPN Ciudad de México Mexico Erlangen Centre for Astroparticle Physics Friedrich Alexander UniversitÃ¤t BY Erlangen Germany Facultad de Ciencias Físico Matemáticas Benemérita Universidad Autónoma de Puebla Puebla Mexico School of Physics Center for Relativistic Astrophysics Georgia Institute of Technology AtlantaGA United States NASA Goddard Space Flight Center GreenbeltMD United States Instituto de Astronomía Universidad Nacional Autónoma de México Ciudad de México Mexico Instituto de Ciencias Nucleares Universidad Nacional Autónoma de México Ciudad de México Mexico Instituto de Física Universidad Nacional Autónoma de México Ciudad de México Mexico Institute of Nuclear Physics Polish Academy of Sciences Krakow Poland Instituto de Geofísica Universidad Nacional Autónoma de México Ciudad de México Mexico Instituto Nacional de Astrofísica Óptica y Electrónica Tonantzintla Puebla Mexico INFN Padova Padova Italy Tecnologico de Monterrey Escuela de Ingeniería y Ciencias Ave. Eugenio Garza Sada 2501 N.L. Monterrey64849 Mexico Physics Division Los Alamos National Laboratory Los AlamosNM United States Max-Planck Institute for Nuclear Physics Heidelberg Germany NASA Marshall Space Flight Center Astrophysics Office HuntsvilleAL United States Department of Physics and Astronomy Michigan State University East LansingMI United States Department of Physics Michigan Technological University HoughtonMI United States Space Science Center University of New Hampshire DurhamNH United States Department of Physics Pennsylvania State University University ParkPA United States Department of Physics and Astronomy University of Rochester RochesterNY United States Tsung-Dao Lee Institute School of Phys

Thanks to recent technological development, a new generation of cosmic ray experiments have been developed with more sensitivity to study these particles in the primary energy interval from 10 TeV to 1 PeV, such as HAWC. Due to its design and high altitude, the HAWC gamma-ray and cosmic ray observatory can provide a bridge between the data from direct and indirect cosmic ray detectors. In 2017 the HAWC collaboration published its first result on the total energy spectrum of cosmic rays, which covers the range from 10 to 500 TeV. This work updates the previous result by extending the energy interval of the measured all-particle cosmic-ray energy spectrum up to 1 PeV. The energy spectrum was obtained from the analysis of two years of HAWC’s data using an unfolding method. We employed the QGSJET-ii-04 model for the energy calibration and the spectrum reconstruction. The results confirm the presence of a knee like feature at tens of TeV, as previously reported by the HAWC collaboration in 2017. © Copyright owned by the author(s).

关键词： Cosmic rays

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The Real-Time analysis Platform of KM3NeT and its first results 38

The Real-Time Analysis Platform of KM3NeT and its first resu...

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38th International Cosmic Ray conference, ICRC 2023

作者： Celli, S. Dornic, D. Filippini, F. Giorgio, E. Le Guirriec, E. Lamoureux, M. Mastrodicasa, M. Palacios Gonzalez, J. Le Stum, S. Vannoye, G. Veutro, A. Zegarelli, A. Aiello, S. Albert, A. Alves Garre, S. Aly, Z. Ambrosone, A. Ameli, F. Andre, M. Androutsou, E. Anguita, M. Aphecetche, L. Ardid, M. Ardid, S. Atmani, H. Aublin, J. Bailly-Salins, L. Bardačová, Z. Baret, B. Bariego-Quintana, A. Basegmez du Pree, S. Becherini, Y. Bendahman, M. Benfenati, F. Benhassi, M. Benoit, D.M. Berbee, E. Bertin, V. Biagi, S. Boettcher, M. Bonanno, D. Boumaaza, J. Bouta, M. Bouwhuis, M. Bozza, C. Bozza, R.M. Brânzaş, H. Bretaudeau, F. Bruijn, R. Brunner, J. Bruno, R. Buis, E. Buompane, R. Busto, J. Caiffi, B. Calvo, D. Campion, S. Capone, A. Carenini, F. Carretero, V. Cartraud, T. Castaldi, P. Cecchini, V. Celli, S. Cerisy, L. Chabab, M. Chadolias, M. Chen, A. Cherubini, S. Chiarusi, T. Circella, M. Cocimano, R. Coelho, J.A.B. Coleiro, A. Coniglione, R. Coyle, P. Creusot, A. Cruz, A. Cuttone, G. Dallier, R. Darras, Y. De Benedittis, A. De Martino, B. Decoene, V. Del Burgo, R. Di Cerbo, U.M. Di Mauro, L.S. Di Palma, I. Díaz, A.F. Diaz, C. Diego-Tortosa, D. Distefano, C. Domi, A. Donzaud, C. Dörr, M. Drakopoulou, E. Drouhin, D. Dvornický, R. Eberl, T. Eckerová, E. Eddymaoui, A. van Eeden, T. Eff, M. van Eijk, D. El Bojaddaini, I. El Hedri, S. Enzenhöfer, A. Ferrara, G. Filipović, M.D. Franciotti, D. Fusco, L.A. Gabriel, J. Gagliardini, S. Gal, T. García Méndez, J. Garcia Soto, A. Gatius Oliver, C. Geißelbrecht, N. Ghaddari, H. Gialanella, L. Gibson, B.K. Goos, I. Goupilliere, D. Gozzini, S.R. Gracia, R. Graf, K. Guidi, C. Guillon, B. Gutiérrez, M. van Haren, H. Heijboer, A. Hekalo, A. Hennig, L. Hernández-Rey, J.J. Huang, F. Idrissi Ibnsalih, W. Illuminati, G. James, C.W. de Jong, M. de Jong, P. Jung, B.J. Kalaczyński, P. Kalekin, O. Katz, U.F. Khan Chowdhury, N.R. Khatun, A. Kistauri, G. Kopper, C. Kouchner, A. Kulikovskiy, V. Sapienza Università di Roma Piazzale Aldo Moro 5 Rome00185 Italy Nazionale di Fisica Nucleare Sezione di Roma Piazzale Aldo Moro 5 Rome00185 Italy INFN Sezione di Catania Via Santa Sofia 64 Catania95123 Italy Université de Strasbourg CNRS IPHC UMR 7178 StrasbourgF-67000 France IFIC - Instituto de Física Corpuscular CSIC Universitat de València c/Catedrático José Beltrán 2 Paterna Valencia46980 Spain Aix Marseille Univ CNRS IN2P3 CPPM Marseille France INFN Sezione di Napoli Complesso Universitario di Monte S. Angelo Via Cintia ed. G Napoli80126 Italy Università di Napoli "Federico II" Dip. Scienze Fisiche "E. Pancini" Complesso Universitario di Monte S. Angelo Via Cintia ed. G Napoli80126 Italy INFN Sezione di Roma Piazzale Aldo Moro 2 Roma00185 Italy Universitat Politècnica de Catalunya Laboratori d’Aplicacions Bioacústiques Centre Tecnològic de Vilanova i la Geltrú Avda. Rambla Exposició s/n Vilanova i la Geltrú08800 Spain NCSR Demokritos Institute of Nuclear and Particle Physics Ag. Paraskevi Attikis Athens15310 Greece University of Granada Dept. of Computer Architecture and Technology/CITIC Granada18071 Spain Subatech IMT Atlantique IN2P3-CNRS Université de Nantes 4 rue Alfred Kastler - La Chantrerie BP Nantes20722 44307 France Universitat Politècnica de València Instituto de Investigación para la Gestión Integrada de las Zonas Costeras C/ Paranimf 1 Gandia46730 Spain University Mohammed V in Rabat Faculty of Sciences 4 av. Ibn Battouta B.P. 1014 RabatR.P. 10000 Morocco Université Paris Cité CNRS Astroparticule et Cosmologie ParisF-75013 France LPC CAEN Normandie Univ ENSICAEN UNICAEN CNRS IN2P3 6 boulevard Maréchal Juin Caen14050 France Czech Technical University in Prague Institute of Experimental and Applied Physics Husova 240/5 Prague110 00 Czech Republic Comenius University in Bratislava Department of Nuclear Physics and Biophysics Mlynska dolina F1 Bratislava842 48 Slovakia Nikhef National Instit

KM3NeT is a multi-site neutrino telescope under construction in the depth of the Mediterranean Sea, consisting of two Cherenkov telescopes, ARCA and ORCA, both of which are currently in data-taking. Among the primary scientific goals of KM3NeT are the observation of cosmic neutrinos and the investigation of their sources. ARCA and ORCA are optimized in complementary energy ranges, allowing for the exploration of neutrino astronomy from MeV to tens of PeV. The combination of an extended field of view and a high duty cycle of Cherenkov-based neutrino detectors is crucial for detecting and informing other telescopes about interesting neutrino candidates in a very short time. As emission from these sources can rapidly fade, the alerts need to be shared with low latency, in order to allow for a prompt follow-up in the multi-messenger and multi-wavelength domains, particularly for the detection of transient and variable sources. In the case of poorly localized triggers, such as gravitational waves, KM3NeT can provide refined pointing directions, representing a further advantage. This contribution reports on the status of the software architecture implemented in KM3NeT for a fast reconstruction and classification of events occurring in the detectors. Additionally, the results of the online processing of KM3NeT data in coincidence with GRB221009A will be presented. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Cosmology

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