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In: Risk analysis: an international journal, Band 11, Heft 3, S. 409-417
ISSN: 1539-6924
ONGC's Hazira Gas‐Processing Complex (HGPC) consists of facilities for receiving natural gas along with associated condensate from an off‐shore field at a rate of 20 MMN M3 per day. After separating the condensate, which is processed in condensate fractionation units, the gas is processed through various steps to recover LPG and to reduce its dew point to less than 5°C in order to make it suitable for transportation over long distances. The acid gas recovered during the gas‐sweetening step is processed to obtain sulphur. The major products manufactured at HGPC therefore are lean sweet gas, LPG, NGL, and sulphur. The Oil and Natural Gas Commission awarded the assignment on Hazard Study and Risk Analysis of their Hazira Gas‐Processing Complex (HGPC) to the Council of Scientific and Industrial Research (CSIR) in association with the Netherlands Organisation for Applied Scientific Research (TNO). The scope of this assignment covered a number of closely related and fully defined activities normally encountered in this type of work. Identification of hazards through the most appropriate methods, assigning frequency of occurrence of major unwanted incidents, quantification and assessment of probable damage to plant equipment, environment, human and animal life due to an unexpected event, and evaluation of various methods for reducing risk, together constituted the methodology for this assignment. Detailed recommendations aimed at reducing risk and enhancing reliability of plant and machinery were made. This article gives an overview of the assignment.
Intro -- Tilte Page -- Copyright -- Contents -- Introduction -- Definition of an Environmental Audit -- Should an Environmental Audit be Conducted? -- Advantages/Disadvantages of an Environmental Audit -- Advantages -- Disadvantges -- History of Environmental Auditing -- Three Unique Features of this Book -- Why Does a Home Audit Make Sense? -- Business Office Audits -- What is not Included in this Book? -- Governmental Perspective -- Author's Perspective -- Industrial Perspective -- Is Environmental Compliance a priority? -- Chapter 1: Summary of Environmental Programs and Regulations -- 1.1 Major Environmental Programs -- 1.1.1 Solid and Hazardous Wastes -- 1.1.1.1 Solid wastes -- 1.1.1.2 Hazardous wastes -- 1.1.1.3 Universal wastes -- 1.1.1.4 Radioactive wastes -- 1.1.2 Water Resources -- 1.1.2.1 Vehicle washing -- 1.1.2.2 Floor drains -- 1.1.2.3 Septic tank/disposal system maintenance -- 1.1.2.4 Oil/water separator maintenance -- 1.1.2.5 General permit activities -- 1.1.3 Air Resources -- 1.1.3.1 Open burning -- 1.1.3.2 Waste-oil space heaters -- 1.1.3.3 Idling of heavy-duty, on-road vehicles -- 1.2 Medium (Less Publicized) Environmental Programs -- 1.2.1 Storm Water -- 1.2.1.1 Exempt activities from water resources permitting -- 1.2.2 Environmental Cleanups -- 1.2.3 Chemical/Petroleum Bulk Storage -- 1.2.3.1 Registration of tank and container facilities -- 1.2.3.2 Petroleum bulk storage (PBS) -- 1.2.3.3 Registration of PBS facilities -- 1.3 Minor (Least Publicized) Environmental Programs -- 1.3.1 Pesticides -- 1.3.1.1 Integrated pest management -- 1.3.2 Wetlands -- 1.3.2.1 Freshwater wetlands -- 1.3.2.2 Tidal wetlands -- 1.3.2.3 Federal- or state-protected wetlands -- 1.3.3 Stream Disturbance -- 1.3.4 Lands and Forests -- 1.3.4.1 Property boundaries -- 1.3.4.2 Protected plants -- 1.3.4.3 Stream crossings
In: Defence science journal: a journal devotet to science & technology in defence, Band 61, Heft 6, S. 554-559
ISSN: 0011-748X
In: Latin American perspectives: a journal on capitalism and socialism, Band 30, Heft 1, S. 543-548
ISSN: 0094-582X
In: HELIYON-D-24-36235
SSRN
In: HELIYON-D-24-31673
SSRN
In this Letter we report on the first inverse kinematics measurement of key resonances in the 22Ne(p, γ )23Na reaction which forms part of the NeNa cycle, and is relevant for 23Na synthesis in asymptotic giant branch (AGB) stars. An anti-correlation in O and Na abundances is seen across all well-studied globular clusters (GC), however, reaction-rate uncertainties limit the precision as to which stellar evolution models can reproduce the observed isotopic abundance patterns. Given the importance of GC observations in testing stellar evolution models and their dependence on NeNa reaction rates, it is critical that the nuclear physics uncertainties on the origin of 23Na be addressed. We present results of direct strengths measurements of four key resonances in 22Ne(p, γ )23Na at Ec.m. = 149 keV, 181 keV, 248 keV and 458 keV. The strength of the important Ec.m. = 458 keV reference resonance has been determined independently of other resonance strengths for the first time with an associated strength of ωγ = 0.439(22) eV and with higher precision than previously reported. Our result deviates from the two most recently published results obtained from normal kinematics measurements performed by the LENA and LUNA collaborations but is in agreement with earlier measurements. The impact of our rate on the Na-pocket formation in AGB stars and its relation to the O-Na anti-correlation was assessed via network calculations. Further, the effect on isotopic abundances in CO and ONe novae ejecta with respect to pre-solar grains was investigated ; The authors thank the ISAC operations and technical staff at TRIUMF. TRIUMF's core operations are supported via a contribution from the federal government through the National Research Council Canada, and the Government of British Columbia provides building capital funds. DRAGON is supported by funds from the National Sciences and Engineering Research Council of Canada SAPPJ-2019-00039. The authors acknowledge support from the "ChETEC" COST Action (CA16117), supported by COST 116 (European Cooperation in Science and Technology). MW, AML, JR were supported by the UK Science and Technology Facilities Council (STFC) ST/P003885/1. UB acknowledges support from the European Research Council ERC-2015-STG Nr. 677497. J. José acknowledges support from the Spanish MINECO grant AYA2017-86274-P, the EU FEDER funds and the AGAUR/Generalitat de Catalunya grant SGR-661/2017. Authors from the Colorado School of Mines acknowledge funding via the U.S. Department of Energy grant DE-FG02-93ER40789. ; Peer reviewed
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[Background]: Globular clusters are known to exhibit anomalous abundance trends such as the sodium-oxygen anticorrelation. This trend is thought to arise via pollution of the cluster interstellar medium from a previous generation of stars. Intermediate-mass asymptotic giant branch stars undergoing hot bottom burning (HBB) are a prime candidate for producing sodium-rich oxygen-poor material, and then expelling this material via strong stellar winds. The amount of 23Na produced in this environment has been shown to be sensitive to uncertainties in the 22Ne(p,γ)23Na reaction rate. The 22Ne(p,γ)23Na reaction is also activated in classical nova nucleosynthesis, strongly influencing predicted isotopic abundance ratios in the Na-Al region. Therefore, improved nuclear physics uncertainties for this reaction rate are of critical importance for the identification and classification of pre-solar grains produced by classical novae. ; [Purpose]: At temperatures relevant for both HBB in AGB stars and classical nova nucleosynthesis, the 22Ne(p,γ)23Na reaction rate is dominated by narrow resonances, with additional contribution from direct capture. This study presents new strength values for seven resonances, as well as a study of direct capture. ; [Method]: The experiment was performed in inverse kinematics by impinging an intense isotopically pure beam of 22Ne onto a windowless H2 gas target. The 23Na recoils and prompt γ rays were detected in coincidence using a recoil mass separator coupled to a 4π bismuth-germanate scintillator array surrounding the target. ; [Results]: For the low-energy resonances, located at center of mass energies of 149, 181, and 248 keV, we recover stength values of ωγ149=0.17+0.05−0.04, ωγ181=2.2±0.4, and ωγ248=8.2±0.7 μeV, respectively. These results are in broad agreement with recent studies performed by the LUNA and TUNL groups. However, for the important reference resonance at 458 keV we obtain a strength value of ωγ458=0.44±0.02 eV, which is significantly lower than recently reported values. This is the first time that this resonance has been studied completely independently from other resonance strengths. For the 632-keV resonance we recover a strength value of ωγ632=0.48±0.02 eV, which is an order of magnitude higher than a recent study. For reference resonances at 610- and 1222-keV, our strength values are in agreement with the literature. In the case of direct capture, we recover an S factor of 60 keV b, consistent with prior forward kinematics experiments. ; [Conclusions]: In summary, we have performed the first direct measurement of 22Ne(p,γ)23Na in inverse kinematics. Our results are in broad agreement with the literature, with the notable exception of the 458-keV resonance, for which we obtain a lower strength value. We assessed the impact of the present reaction rate in reference to a variety of astrophysical environments, including AGB stars and classical novae. Production of 23Na in AGB stars is minimally influenced by the factor of 4 increase in the present rate compared to the STARLIB-2013 compilation. The present rate does however impact upon the production of nuclei in the Ne-Al region for classical novae, with dramatically improved uncertainties in the predicted isotopic abundances present in the novae ejecta. ; The authors thank the ISAC operations and technical staff at TRIUMF. TRIUMFs core operations are supported via a contribution from the federal government through the National Research Council Canada, and the Government of British Columbia provides building capital funds. DRAGON is supported by funds from the National Sciences and Engineering Research Council of Canada. UK authors gratefully acknowledge support from the Science and Technology Facilities Council (STFC). J.J. acknowledges support from the Spanish MINECO Grant No. AYA2017-86274-P, the EU FEDER funds and the AGAUR/ Generalitat de Catalunya Grant No. SGR-661/2017. Authors from the Colorado School of Mines acknowledge funding via U.S. Department of Energy Grant No. DE-FG02-93ER40789. U.B. acknowledges support from the European Research Council (Grant No. ERC-2015-STG Nr. 677497). This article also benefited from discussions within the ChETEC COST Action (Grant No. CA16117). ; Peer reviewed
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We report the results of a search for the B -> Y(4260)K, Y(4260) -> J/psi pi(+)pi thorn p-decays. This study is based on a data sample corresponding to an integrated luminosity of 711 fb(-1), collected at the Upsilon(4S) resonance with the Belle detector at the KEKB asymmetric-energy e(+)e(-) collider. We investigate the J/psi pi(+)pi(-) thorn p-invariant mass distribution in the range 4.0 to 4.6 GeV/c(2) using both B+ -> J/psi pi(+)pi K--(+) and B-0 -> J/psi pi(+)pi K--(S)0 decays. We find excesses of events above the background levels, with significances of 2.1 and 0.9 standard deviations for charged and neutral B -> Y(4260)K decays, respectively, taking into account the systematic uncertainties. These correspond to upper limits on the product of branching fractions, B(B+ -> Y(4260)K+) x B(Y(4260) -> J/psi pi(+)pi(-)) Y(4260)K-0) x B(Y(4260) -> J/psi pi(+)pi(-)) < 1.7 x 10(-5) at the 90% confidence level. ; Public domain authored by a U.S. government employee
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BMWFW (Austria) ; FWF (Austria) ; FNRS (Belgium) ; FWO (Belgium) ; Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) ; Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) ; Fundação de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ) ; Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP) ; MES (Bulgaria) ; CERN (China) ; CAS (China) ; MoST (China) ; NSFC (China) ; COLCIENCIAS (Colombia) ; MSES (Croatia) ; CSF (Croatia) ; RPF (Cyprus) ; SENESCYT (Ecuador) ; MoER (Estonia) ; ERC IUT (Estonia) ; ERDF (Estonia) ; Academy of Finland (Finland) ; MEC (Finland) ; HIP (Finland) ; CEA (France) ; CNRS/IN2P3 (France) ; BMBF (Germany) ; DFG (Germany) ; HGF (Germany) ; GSRT (Greece) ; OTKA (Hungary) ; NIH (Hungary) ; DAE (India) ; DST (India) ; IPM (Iran) ; SFI (Ireland) ; INFN (Italy) ; MSIP (Republic of Korea) ; NRF (Republic of Korea) ; LAS (Lithuania) ; MOE (Malaysia) ; UM (Malaysia) ; BUAP (Mexico) ; CINVESTAV (Mexico) ; CONACYT (Mexico) ; LNS (Mexico) ; SEP (Mexico) ; UASLP-FAI (Mexico) ; MBIE (New Zealand) ; PAEC (Pakistan) ; MSHE (Poland) ; NSC (Poland) ; FCT (Portugal) ; JINR (Dubna) ; MON (Russia) ; RosAtom (Russia) ; RAS (Russia) ; RFBR (Russia) ; MESTD (Serbia) ; SEIDI (Spain) ; CPAN (Spain) ; Swiss Funding Agencies (Switzerland) ; MST (Taipei) ; ThEPCenter (Thailand) ; IPST (Thailand) ; STAR (Thailand) ; NSTDA (Thailand) ; TUBITAK (Turkey) ; TAEK (Turkey) ; NASU (Ukraine) ; SFFR (Ukraine) ; STFC (United Kingdom) ; DOE (USA) ; NSF (USA) ; Marie-Curie programme (European Union) ; European Research Council (European Union) ; EPLANET (European Union) ; Leventis Foundation ; A.P. Sloan Foundation ; Alexander von Humboldt Foundation ; Belgian Federal Science Policy Office ; Fonds pour la Formation a la Recherche dans l'Industrie et dans l'Agriculture (FRIA-Belgium) ; Agentschap voor Innovatie door Wetenschap en Technologie (IWT-Belgium) ; Ministry of Education, Youth and Sports (MEYS) of the Czech Republic ; Council of Science and Industrial Research, India ; HOMING PLUS programme of the Foundation for Polish Science ; Regional Development Fund ; National Science Center (Poland) ; Thalis programme - EU-ESF ; National Priorities Research Program by Qatar National Research Fund ; Programa Clarin-COFUND del Principado de Asturias ; Rachadapisek Sompot Fund for Postdoctoral Fellowship, Chulalongkorn University ; Chulalongkorn Academic into Its 2nd Century Project Advancement Project (Thailand) ; Welch Foundation ; European Union ; Mobility Plus programme of the Ministry of Science and Higher Education ; Thalis programme - Greek NSRF ; Aristeia programme - EU-ESF ; Aristeia programme - Greek NSRF ; Science and Technology Facilities Council ; National Science Center (Poland): Harmonia 2014/14/M/ST2/00428 ; National Science Center (Poland): Opus 2013/11/B/ST2/04202 ; National Science Center (Poland): 2014/13/B/ST2/02543 ; National Science Center (Poland): 2014/15/B/ST2/03998 ; National Science Center (Poland): Sonata-bis 2012/07/E/ST2/01406 ; Welch Foundation: C-1845 ; Science and Technology Facilities Council: ST/K001256/1 ; Science and Technology Facilities Council: ST/N000250/1 ; Science and Technology Facilities Council: CMS ; Science and Technology Facilities Council: GRIDPP ; The WZ production cross section in proton-proton collisions at root s = 13 Tev is measured with the CMS experiment at the LHC using a data sample corresponding to an integrated luminosity of 2.3 fb(-1). The measurement is performed in the leptonic decay modes WZ -> lVl'l', where l,l'=e,mu. The measured cross section for the range 60 WZ) = 39.9 +/- 3.2(stat)(2.9)(-3.1)(syst)+/- 0.4(theo)+/- 1.3(lumi)pb, consistent with the standard model prediction.
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Austrian Federal Ministry of Education, Science and Research ; Austrian Science Fund ; Belgian Fonds de la Recherche Scientifique ; Fonds voor Wetenschappelijk Onderzoek ; Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) ; Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) ; Fundação de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ) ; FAPERGS ; Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP) ; Bulgarian Ministry of Education and Science ; CERN ; Chinese Academy of Sciences ; Ministry of Science and Technology ; National Natural Science Foundation of China ; Colombian Funding Agency (COLCIENCIAS) ; Croatian Ministry of Science, Education and Sport ; Croatian Science Foundation ; Research Promotion Foundation, Cyprus ; Secretariat for Higher Education, Science, Technology and Innovation, Ecuador ; Ministry of Education and Research, Estonia ; Estonian Research Council, Estonia ; European Regional Development Fund, Estonia ; Academy of Finland ; Finnish Ministry of Education and Culture ; Helsinki Institute of Physics ; Institut National de Physique Nucleaire et de Physique des Particules / CNRS, France ; Commissariat a l'Energie Atomique et aux Energies Alternatives / CEA, France ; Bundesministerium fur Bildung und Forschung, Germany ; Deutsche Forschungsgemeinschaft, Germany ; Helmholtz-Gemeinschaft Deutscher Forschungszentren, Germany ; General Secretariat for Research and Technology, Greece ; National Research, Development and Innovation Fund, Hungary ; Department of Atomic Energy, India ; Department of Science and Technology, India ; Institute for Studies in Theoretical Physics and Mathematics, Iran ; Science Foundation, Ireland ; Istituto Nazionale di Fisica Nucleare, Italy ; Ministry of Science, ICT and Future Planning, Republic of Korea ; National Research Foundation (NRF), Republic of Korea ; Ministry of Education and Science of the Republic of Latvia ; Lithuanian Academy of Sciences ; Ministry of Education ; University of Malaya (Malaysia) ; Ministry of Science of Montenegro ; BUAP ; CINVESTAV ; CONACYT ; LNS ; SEP ; UASLP-FAI ; Ministry of Business, Innovation and Employment, New Zealand ; Pakistan Atomic Energy Commission ; Ministry of Science and Higher Education, Poland ; National Science Center, Poland ; Fundacao para a Ciencia e a Tecnologia, Portugal ; JINR, Dubna ; Ministry of Education and Science of the Russian Federation ; Federal Agency of Atomic Energy of the Russian Federation ; Russian Academy of Sciences ; Russian Foundation for Basic Research ; National Research Center Kurchatov Institute ; Ministry of Education, Science and Technological Development of Serbia ; Secretaria de Estado de Investigacion, Desarrollo e Innovacion, Programa Consolider-Ingenio 2010, Plan Estatal de Investigacion Cientifica y Tecnica y de Innovacion 2013-2016, Plan de Ciencia, Tecnologia e Innovacion 2013-2017 del Principado de Asturias, S ; Fondo Europeo de Desarrollo Regional, Spain ; Ministry of Science, Technology and Research, Sri Lanka ; ETH Board ; PSI ; SNF ; UniZH ; Canton Zurich ; SER ; Ministry of Science and Technology, Taipei ; Thailand Center of Excellence in Physics ; Institute for the Promotion of Teaching Science and Technology of Thailand ; Special Task Force for Activating Research ; National Science and Technology Development Agency of Thailand ; Scientific and Technical Research Council of Turkey ; Turkish Atomic Energy Authority ; National Academy of Sciences of Ukraine, Ukraine ; State Fund for Fundamental Researches, Ukraine ; Science and Technology Facilities Council, U.K. ; US Department of Energy ; US National Science Foundation ; Marie-Curie program (European Union) ; European Research Council (European Union) ; Horizon 2020 (European Union) ; Leventis Foundation ; A. P. Sloan Foundation ; Alexander von Humboldt Foundation ; Belgian Federal Science Policy Office ; Fonds pour la Formation a la Recherche dans l'Industrie et dans l'Agriculture (FRIA-Belgium) ; Agentschap voor Innovatie door Wetenschap en Technologie (IWT-Belgium) ; F.R.S.-FNRS (Belgium) ; FWO (Belgium) ; Ministry of Education, Youth and Sports (MEYS) of the Czech Republic ; Hungarian Academy of Sciences (Hungary) ; New National Excellence Program UNKP (Hungary) ; NKFIA (Hungary) ; Council of Scientific and Industrial Research, India ; HOMING PLUS program of the Foundation for Polish Science ; European Union, Regional Development Fund ; Mobility Plus program of the Ministry of Science and Higher Education ; National Science Center (Poland) ; National Priorities Research Program by Qatar National Research Fund ; Programa de Excelencia Maria de Maeztu ; Programa Severo Ochoa del Principado de Asturias ; Thalis program ; Aristeia program ; EU-ESF ; Greek NSRF ; Rachadapisek Sompot Fund for Postdoctoral Fellowship, Chulalongkorn University (Thailand) ; Chulalongkorn Academic into Its 2nd Century Project Advancement Project (Thailand) ; Welch Foundation ; Weston Havens Foundation (U.S.A.) ; Estonian Research Council, Estonia: IUT23-4 ; Estonian Research Council, Estonia: IUT23-6 ; Horizon 2020 (European Union): 675440 ; FWO (Belgium): 30820817 ; NKFIA (Hungary): 123842 ; NKFIA (Hungary): 123959 ; NKFIA (Hungary): 124845 ; NKFIA (Hungary): 124850 ; NKFIA (Hungary): 125105 ; National Science Center (Poland): Harmonia 2014/14/M/ST2/00428 ; National Science Center (Poland): Opus 2014/13/B/ST2/02543 ; National Science Center (Poland): 2014/15/B/ST2/03998 ; National Science Center (Poland): 2015/19/B/ST2/02861 ; National Science Center (Poland): Sonata-bis 2012/07/E/ST2/01406 ; Welch Foundation: C-1845 ; An embedding technique is presented to estimate standard model tau tau backgrounds from data with minimal simulation input. In the data, the muons are removed from reconstructed mu mu events and replaced with simulated tau leptons with the same kinematic properties. In this way, a set of hybrid events is obtained that does not rely on simulation except for the decay of the tau leptons. The challenges in describing the underlying event or the production of associated jets in the simulation are avoided. The technique described in this paper was developed for CMS. Its validation and the inherent uncertainties are also discussed. The demonstration of the performance of the technique is based on a sample of proton-proton collisions collected by CMS in 2017 at root s = 13 TeV corresponding to an integrated luminosity of 41.5 fb(-1).
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