Improving the efficiency of planning as a basis for management the investment activity of an industrial enterprise

The first and one of the most important functions of management is planning. At the same time, in the current market conditions, the time for the implementation of this stage is very limited. In many ways, this applies to the oil and gas industry all the same. Due to the reduction of the resource base of the industry, the share of super-profitable projects has decreased significantly. Extraction of hard-to-recover oil and gas reserves is associated with active investment activities and with the need to introduce expensive technologies and equipment. The most common type of investment project associated with the geological and technical activities is being considered in the present paper. In order to increase the economic efficiency of the geological and technical activities it is proposed to implement an automated model at the stage of planning. This model, on the basis of the generalized geological, technological, statistical, macroeconomic and economic indicators, allows to solve quickly the following problems: of more precise and prompt planning the expenses on carrying out geological and technical actions; of defining minimum admissible profitable level of an oil flow rate after carrying out geological and technical actions; of determining the most economically justified duration of the overhaul of the well; of organizing the projects of geological and technical measures according to their attractiveness. As a result of the implementation of the automated model, an efficiency matrix for a particular field was compiled that determines the impact of the necessary investments and planned flow rate on the economic indicators of the project. The use of this matrix made it possible to exclude several inefficient geological and technical measures from the plan. The method of ranking based on the calculation of the integrated efficiency coefficient has been developed. On its basis, the issue of making optimal management decisions taking into account the impact of risk assessment in the case of projects with the same economic efficiency is solved. © Belarusian National Technical University, 2019

Методический инструментарий оценки эффективности проектов капитального строительства нефтедобывающих предприятий

Due to the fact that most of the large oil fields in Russia, characterized by high production costs, are at the final stage of development; the issue of cost optimization has become increasingly important in recent years. The main cost items at oil and gas enterprises are design and construction (reconstruction) of oil field facilities. Analysis of currently used methods for ranking oil and gas projects has shown that all of them are inherently subjective, since they are based on expert opinion. The authors have developed a methodological tools for evaluating the effectiveness of capital construction projects of oil field facilities (for example, construction work on the site for inventory receiving bridges and lifting units), which allows  to eliminate the influence of expert opinion  as much as possible and, consequently,  significantly  improve  the quality and validity of management decisions. The choice of the optimal project is based on a two – level assessment (stage 1– technical assessment, stage 2 – economic assessment). At each stage, an integral indicator is determined by calculation based on the results of objective data analysis  and using the developed algorithms. Thus, it is possible to judge the effectiveness of any project without being based on a subjective approach in the assessment with the help of expert opinion.Ввиду того что большинство крупных нефтяных месторождений России, характеризующихся высокой себестоимостью добываемой продукции, находятся на заключительной стадии разработки, в последние годы вопрос оптимизации затрат приобретает все большее значение. Основные статьи затрат на предприятиях нефтегазового комплекса – проектирование и строительство (реконструкция) нефтепромысловых объектов. Анализ применяемых в настоящее время методов ранжирования нефтегазовых проектов показал, что все они по своей сути являются субъективными, так как основаны на экспертном мнении. Авторами разработан методический инструментарий оценки эффективности проектов капитального строительства нефтепромысловых объектов (на примере проведения строительных работ на площадке под инвентарные приемные мостки и подъемный агрегат), позволяющий максимально исключить влияние экспертного мнения и соответственно существенно повысить качество и обоснованность принимаемых управленческих решений. Выбор оптимального проекта осуществляется на основе двухуровневой оценки: технической (1-й этап) и экономической (2-й этап). При этом на каждом этапе расчетным путем по результатам анализа объективных данных и с помощью разработанных алгоритмов определяется интегральный показатель. Таким образом, можно судить об эффективности любого проекта, не основываясь на субъективном подходе в оценке с помощью экспертного мнения

Another Shipment of Six Short-Period Giant Planets from TESS

We present the discovery and characterization of six short-period, transiting giant planets from NASA's Transiting Exoplanet Survey Satellite (TESS) -- TOI-1811 (TIC 376524552), TOI-2025 (TIC 394050135), TOI-2145 (TIC 88992642), TOI-2152 (TIC 395393265), TOI-2154 (TIC 428787891), & TOI-2497 (TIC 97568467). All six planets orbit bright host stars (8.9 <G< 11.8, 7.7 <K< 10.1). Using a combination of time-series photometric and spectroscopic follow-up observations from the TESS Follow-up Observing Program (TFOP) Working Group, we have determined that the planets are Jovian-sized (R$_{P}$ = 1.00-1.45 R$_{J}$), have masses ranging from 0.92 to 5.35 M$_{J}$, and orbit F, G, and K stars (4753 $<$ T$_{eff}$ $<$ 7360 K). We detect a significant orbital eccentricity for the three longest-period systems in our sample: TOI-2025 b (P = 8.872 days, $e$ = $0.220\pm0.053$), TOI-2145 b (P = 10.261 days, $e$ = $0.182^{+0.039}_{-0.049}$), and TOI-2497 b (P = 10.656 days, $e$ = $0.196^{+0.059}_{-0.053}$). TOI-2145 b and TOI-2497 b both orbit subgiant host stars (3.8 $<$ $\log$ g $<$4.0), but these planets show no sign of inflation despite very high levels of irradiation. The lack of inflation may be explained by the high mass of the planets; $5.35^{+0.32}_{-0.35}$ M$_{\rm J}$ (TOI-2145 b) and $5.21\pm0.52$ M$_{\rm J}$ (TOI-2497 b). These six new discoveries contribute to the larger community effort to use {\it TESS} to create a magnitude-complete, self-consistent sample of giant planets with well-determined parameters for future detailed studies.Comment: 20 Pages, 6 Figures, 8 Tables, Accepted by MNRA

A Possible Alignment between the Orbits of Planetary Systems and their Visual Binary Companions

Astronomers do not have a complete picture of the effects of wide-binary companions (semimajor axes greater than 100 au) on the formation and evolution of exoplanets. We investigate these effects using new data from Gaia Early Data Release 3 and the Transiting Exoplanet Survey Satellite mission to characterize wide-binary systems with transiting exoplanets. We identify a sample of 67 systems of transiting exoplanet candidates (with well-determined, edge-on orbital inclinations) that reside in wide visual binary systems. We derive limits on orbital parameters for the wide-binary systems and measure the minimum difference in orbital inclination between the binary and planet orbits. We determine that there is statistically significant difference in the inclination distribution of wide-binary systems with transiting planets compared to a control sample, with the probability that the two distributions are the same being 0.0037. This implies that there is an overabundance of planets in binary systems whose orbits are aligned with those of the binary. The overabundance of aligned systems appears to primarily have semimajor axes less than 700 au. We investigate some effects that could cause the alignment and conclude that a torque caused by a misaligned binary companion on the protoplanetary disk is the most promising explanation. © 2022. The Author(s). Published by the American Astronomical Society.AB022006; ANR-15-IDEX-01; 80NSSC19K1727; National Science Foundation, NSF; National Aeronautics and Space Administration, NASA: 18-2XRP18_2-0136; New York Community Trust, NYCT; Australian Research Council, ARC; National Research Foundation, NRF; Japan Society for the Promotion of Science, KAKEN: 15H02063, 18H05442, 20K14521, 22000005, JP17H04574, JP18H05439, JP20J21872, JP20K14518, JP21K13955; Ministry of Education, Culture, Sports, Science and Technology, MEXT; Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung, SNF; Fonds De La Recherche Scientifique - FNRS, FNRS: FRFC 2.5.594.09; Ministry of Science, ICT and Future Planning, MSIP; Nagoya University, NU: 10147207, 10147214; Université de Liège, ULg; Universidad Católica de la Santísima Concepción, UCSC: DI-FIAI 03/2021; National Astronomical Observatory of Japan, NAOJ; Precursory Research for Embryonic Science and Technology, PRESTO: JPMJPR1775; Instituto de Astrofísica de Andalucía, IAA: SEV-2017-0709This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA’s Science Mission directorate.K.K.M. acknowledges support from the New York Community Trust's Fund for Astrophysical Research.The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant FRFC 2.5.594.09.F. TRAPPIST-North is a project funded by the University of Liège (Belgium), in collaboration with Cadi Ayyad University of Marrakech (Morocco).This work is partly supported by JSPS KAKENHI grant No. JP20K14518, and by Astrobiology Center SATELLITE Research project AB022006.This work is partly supported by JSPS KAKENHI grant No. JP21K13955.This work is partly supported by JSPS KAKENHI grant No. 20K14521.This paper is based on observations made with the MuSCAT3 instrument, developed by the Astrobiology Center and under financial supports by JSPS KAKENHI (JP18H05439) and JST PRESTO (JPMJPR1775), at Faulkes Telescope North on Maui, HI, operated by the Las Cumbres Observatory.The IRSF project is a collaboration between Nagoya University and the South African Astronomical Observatory (SAAO) supported by the Grants-in-Aid for Scientific Research on Priority Areas (A) (grant Nos. 10147207 and 10147214) and Optical & Near-Infrared Astronomy Inter-University Cooperation Program, from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan and the National Research Foundation (NRF) of South Africa.C.R.-L. acknowledges financial support from the State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709).M.T. is supported by MEXT/JSPS KAKENHI grant Nos. 18H05442, 15H02063, and 22000005.This work is partly supported by JSPS KAKENHI grant No. JP18H05439, and JST PRESTO grant No. JPMJPR1775, and a University Research Support Grant from the National Astronomical Observatory of Japan (NAOJ).P.J.A. acknowledges support from grant AYA2016-79425-C3-3-P of the Spanish Ministry of Economy and Competitiveness (MINECO) and the Centre of Excellence “Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709)

Another shipment of six short-period giant planets from TESS

We present the discovery and characterization of six short-period, transiting giant planets from NASA’s Transiting Exoplanet Survey Satellite (TESS) – TOI-1811 (TIC 376524552), TOI-2025 (TIC 394050135), TOI-2145 (TIC 88992642), TOI-2152 (TIC 395393265), TOI-2154 (TIC 428787891), and TOI-2497 (TIC 97568467). All six planets orbit bright host stars (8.9 &lt;G &lt; 11.8, 7.7 &lt;K &lt; 10.1). Using a combination of time-series photometric and spectroscopic follow-up observations from the TESS Follow-up Observing Program Working Group, we have determined that the planets are Jovian-sized (RP = 0.99–1.45 RJ), have masses ranging from 0.92 to 5.26 MJ, and orbit F, G, and K stars (4766 ≤ Teff ≤ 7360 K). We detect a significant orbital eccentricity for the three longest-period systems in our sample: TOI-2025 b (P = 8.872 d, 0.394+0.035-0.038), TOI-2145 b (P = 10.261 d, e = 0.208+0.034-0.047), and TOI-2497 b (P = 10.656 d, e = 0.195+0.043-0.040). TOI-2145 b and TOI-2497 b both orbit subgiant host stars (3.8 &lt; log g &lt;4.0), but these planets show no sign of inflation despite very high levels of irradiation. The lack of inflation may be explained by the high mass of the planets; 5.26+0.38-0.37 MJ (TOI-2145 b) and 4.82 ± 0.41 MJ (TOI-2497 b). These six new discoveries contribute to the larger community effort to use TESS to create a magnitude-complete, self-consistent sample of giant planets with well-determined parameters for future detailed studies. © 2023 The Author(s).80NSSC20K0250; LE140100050; FEUZ-2020-0038, PGC2018-098153-B-C31; National Science Foundation, NSF: 1516242, 1608203, 2007811, AST-1751874, AST-1907790; David and Lucile Packard Foundation, DLPF; National Aeronautics and Space Administration, NASA: GN-2018B-LP-101, NNX13AM97A, XRP 80NSSC22K0233; W. M. Keck Foundation, WMKF; New York Community Trust, NYCT; Research Corporation for Science Advancement, RCSA; Pennsylvania Space Grant Consortium, PSGC; Ames Research Center, ARC; George Mason University, GMU; University of North Carolina, UNC; Massachusetts Institute of Technology, MIT; University of Pennsylvania; Ohio State University, OSU; California Institute of Technology, CIT; University of Florida, UF; Michigan State University, MSU; University of North Carolina at Chapel Hill, UNC-CH; Pennsylvania State University, PSU; University of Montana, UM; University of Texas at Austin, UT; Smithsonian Astrophysical Observatory, SAO; Horizon 2020 Framework Programme, H2020: 1952545, 724427; Mt. Cuba Astronomical Foundation; Accelerated Bridge Construction University Transportation Center, ABC-UTC; National Centres of Competence in Research SwissMAP; Diabetes Patient Advocacy Coalition, DPAC; European Research Council, ERC; European Space Agency, ESA; Australian Research Council, ARC: DP180100972, DP210103119, DP220100365, FL220100117, LE160100001; Deutsche Forschungsgemeinschaft, DFG: HA 3279/12-1, SPP1992; Japan Society for the Promotion of Science, KAKEN: JP18H05439; University of New South Wales, UNSW; University of Southern Queensland, USQ; Fondo Nacional de Desarrollo Científico y Tecnológico, FONDECYT: 11200751, 1210718, 14ENI2-26865, IC120009; Core Research for Evolutional Science and Technology, CREST: JPMJCR1761; Ministry of Education and Science of the Russian Federation, Minobrnauka: 075-15-2020-780, N13.1902.21.0039; Ministério da Ciência, Tecnologia e Inovação, MCTI; University of Toronto, U of T; Université de Genève, UNIGE; Ministry of Economy; Nanjing University, NJU; Instituto de Astrofísica de Canarias, IAC; NCCR Catalysis, NCCRThe authors thank the CHIRON team members, including Todd Henry, Leonardo Paredes, Hodari James, Azmain Nisak, Rodrigo Hinojosa, Roberto Aviles, Wei-Chun Jao, and CTIO staffs, for their work in acquiring RVs with CHIRON at CTIO. This research has made use of SAO/NASA’s Astrophysics Data System Bibliographic Services. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work makes use of observations from the LCO network. Based in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia e Inovações (MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU).Funding for the TESS mission is provided by NASA’s Science Mission directorate. The authors acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the NASA Exoplanet Archive and the Exoplanet Follow-up Observation Program website, which are operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). This paper includes observations obtained under Gemini program GN-2018B-LP-101. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This publication makes use of The Data and Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planets data visualisation, exchange and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the Swiss expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch .LC, KS, EA, JR, JER, JAR, PW, and EZ are grateful for support from NSF grants AST-1751874 and AST-1907790, along with a Cottrell Fellowship from the Research Corporation. CZ is supported by a Dunlap Fellowship at the Dunlap Institute for Astronomy & Astrophysics, funded through an endowment established by the Dunlap family and the University of Toronto. T.H. acknowledges support from the European Research Council under the Horizon 2020 Framework Program via the ERC Advanced Grant Origins 83 24 28. JVS acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project Four Aces; grant agreement No. 724427). PR acknowledges support from NSF grant No. 1952545. RB and AJ acknowledges support from FONDECYT Projects 11200751 and 1210718 and from the CORFO project N◦14ENI2-26865. AJ, RB and MH acknowledge support from project IC120009 ‘Millennium Institute of Astrophysics (MAS)’ of the Millenium Science Initiative, Chilean Ministry of Economy. The Pennsylvania State University Eberly College of Science. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. KKM gratefully acknowledges support from the New York Community Trust’s Fund for Astrophysical Research. LG and AG are supported by NASA Massachusetts Space Grant Fellowships. EWG, ME, and PC acknowledge support by Deutsche Forschungsgemeinschaft (DFG) grant HA 3279/12-1 within the DFG Schwerpunkt SPP1992, Exploring the Diversity of Extrasolar Planets. BSG was partially supported by the Thomas Jefferson Chair for Space Exploration at the Ohio State University. CD acknowledges support from the Hellman Fellows Fund and NASA XRP via grant 80NSSC20K0250. BSS, MVG, and AAB acknowledge the support of Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780 (N13.1902.21.0039). BA is supported by Australian Research Council Discovery Grant DP180100972. TRB acknowledges support from the Australian Research Council (DP210103119). TRB acknowledges support from the Australian Research Council (DP210103119 and FL220100117). The authors thank the CHIRON team members, including Todd Henry, Leonardo Paredes, Hodari James, Azmain Nisak, Rodrigo Hinojosa, Roberto Aviles, Wei-Chun Jao, and CTIO staffs, for their work in acquiring RVs with CHIRON at CTIO. This research has made use of SAO/NASA’s Astrophysics Data System Bibliographic Services. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work makes use of observations from the LCO network. Based in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia e Inovações (MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). Funding for the TESS mission is provided by NASA’s Science Mission directorate. The authors acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the NASA Exoplanet Archive and the Exoplanet Follow-up Observation Program website, which are operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). This paper includes observations obtained under Gemini program GN-2018B-LP-101. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This publication makes use of The Data and Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planets data visualisation, exchange and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the Swiss expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch. MINERVA-Australis is supported by Australian Research Council LIEF Grant LE160100001 (Discovery Grant DP180100972 and DP220100365) Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. The authors respectfully acknowledge the traditional custodians of all lands throughout Australia and recognize their continued cultural and spiritual connection to the land, waterways, cosmos, and community. The authors pay our deepest respects to all Elders, ancestors and descendants of the Giabal, Jarowair, and Kambuwal nations, upon whose lands the MINERVA-Australis facility at Mt Kent is situated. MINERVA-North is a collaboration among the Harvard-Smithsonian Center for Astrophysics, The Pennsylvania State University, the University of Montana, the University of Southern Queensland, University of Pennsylvania, and George Mason University. It is made possible by generous contributions from its collaborating institutions and Mt. Cuba Astronomical Foundation, The David & Lucile Packard Foundation, National Aeronautics and Space Administration (EPSCOR grant NNX13AM97A, XRP 80NSSC22K0233), the Australian Research Council (LIEF grant LE140100050), and the National Science Foundation (grants 1516242, 1608203, and 2007811). This article is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sánchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. This work is partly financed by the Spanish Ministry of Economics and Competitiveness through grants PGC2018-098153-B-C31.The work of VK was supported by the Ministry of science and higher education of the Russian Federation, topic FEUZ-2020-0038. This work is partly supported by JSPS KAKENHI Grant Number JP18H05439, JST CREST Grant Number JPMJCR1761. This article is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sánchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide.Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.This article is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sánchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. This work is partly financed by the Spanish Ministry of Economics and Competitiveness through grants PGC2018-098153-B-C31.The work of VK was supported by the Ministry of science and higher education of the Russian Federation, topic FEUZ-2020-0038.LC, KS, EA, JR, JER, JAR, PW, and EZ are grateful for support from NSF grants AST-1751874 and AST-1907790, along with a Cottrell Fellowship from the Research Corporation. CZ is supported by a Dunlap Fellowship at the Dunlap Institute for Astronomy & Astrophysics, funded through an endowment established by the Dunlap family and the University of Toronto. T.H. acknowledges support from the European Research Council under the Horizon 2020 Framework Program via the ERC Advanced Grant Origins 83 24 28. JVS acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project Four Aces; grant agreement No. 724427). PR acknowledges support from NSF grant No. 1952545. RB and AJ acknowledges support from FONDECYT Projects 11200751 and 1210718 and from the CORFO project N°14ENI2-26865. AJ, RB and MH acknowledge support from project IC120009 ‘Millennium Institute of Astrophysics (MAS)’ of the Millenium Science Initiative, Chilean Ministry of Economy. The Pennsylvania State University Eberly College of Science. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. KKM gratefully acknowledges support from the New York Community Trust’s Fund for Astrophysical Research. LG and AG are supported by NASA Massachusetts Space Grant Fellowships. EWG, ME, and PC acknowledge support by Deutsche Forschungsgemeinschaft (DFG) grant HA 3279/12-1 within the DFG Schwerpunkt SPP1992, Exploring the Diversity of Extrasolar Planets. BSG was partially supported by the Thomas Jefferson Chair for Space Exploration at the Ohio State University. CD acknowledges support from the Hellman Fellows Fund and NASA XRP via grant 80NSSC20K0250. BSS, MVG, and AAB acknowledge the support of Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780 (N13.1902.21.0039). BA is supported by Australian Research Council Discovery Grant DP180100972. TRB acknowledges support from the Australian Research Council (DP210103119). TRB acknowledges support from the Australian Research Council (DP210103119 and FL220100117).Minerva -Australis is supported by Australian Research Council LIEF Grant LE160100001 (Discovery Grant DP180100972 and DP220100365) Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. The authors respectfully acknowledge the traditional custodians of all lands throughout Australia and recognize their continued cultural and spiritual connection to the land, waterways, cosmos, and community. The authors pay our deepest respects to all Elders, ancestors and descendants of the Giabal, Jarowair, and Kambuwal nations, upon whose lands the Minerva -Australis facility at Mt Kent is situated.MINERVA-North is a collaboration among the Harvard-Smithsonian Center for Astrophysics, The Pennsylvania State University, the University of Montana, the University of Southern Queensland, University of Pennsylvania, and George Mason University. It is made possible by generous contributions from its collaborating institutions and Mt. Cuba Astronomical Foundation, The David & Lucile Packard Foundation, National Aeronautics and Space Administration (EPSCOR grant NNX13AM97A, XRP 80NSSC22K0233), the Australian Research Council (LIEF grant LE140100050), and the National Science Foundation (grants 1516242, 1608203, and 2007811)

Ранние оптические наблюдения семи гамма-всплесков в сравнении с их гамма-рентгеновскими характеристиками на глобальной сети телескопов-роботов МГУ МАСТЕР

Seven gamma-ray bursts – GRB 130907A, GRB 140311B, GRB 140129B, GRB 160227A, GRB 120404A, GRB 110801A, and GRB 120811C were observed by the MSU MASTER (Mobile Astronomical System of TElescope Robots) Global Network. Full automation of the observations provided for obtaining unique data on the properties of early optical radiation accompanying gamma-ray bursts. The data are compared in the optical (MASTER), X-ray (SWIFT X-ray Telescope, XRT) and gamma (SWIFT Burst Alert Telescope, BAT) ranges. Based on the data obtained, two groups are identified, and their radiation mechanisms are revealed. The effect of gamma-ray bursts on the biosphere of the Earth is determined, and the estimates and the scale of such an effect are considered.В статье представлены результаты наблюдений семи гамма-всплесков – GRB 130907A, GRB 140311B, GRB 140129B, GRB 160227A, GRB 120404A, GRB 110801A, GRB 120811C, полученные на телескопах-роботах глобальной сети МГУ «МАСТЕР». Полная автоматизация наблюдений позволила получить уникальные данные о свойствах раннего оптического излучения, сопровождавшего гамма-всплески. Выполнено сравнение данных в оптическом (МАСТЕР), рентгеновском (SWIFTX-rayTelescope (XRT)) и гамма (SWIFTBurstAlertTelescope (BAT)) диапазонах. На основании полученных данных выделены две группы, для которых определен механизм излучения. Также определено воздействие гамма-всплесков на биосферу Земли и рассмотрены оценки и масштаб такого влияния

A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions

Astronomers do not have a complete picture of the effects of wide-binary companions (semimajor axes greater than 100 au) on the formation and evolution of exoplanets. We investigate these effects using new data from Gaia Early Data Release 3 and the Transiting Exoplanet Survey Satellite mission to characterize wide-binary systems with transiting exoplanets. We identify a sample of 67 systems of transiting exoplanet candidates (with well-determined, edge-on orbital inclinations) that reside in wide visual binary systems. We derive limits on orbital parameters for the wide-binary systems and measure the minimum difference in orbital inclination between the binary and planet orbits. We determine that there is statistically significant difference in the inclination distribution of wide-binary systems with transiting planets compared to a control sample, with the probability that the two distributions are the same being 0.0037. This implies that there is an overabundance of planets in binary systems whose orbits are aligned with those of the binary. The overabundance of aligned systems appears to primarily have semimajor axes less than 700 au. We investigate some effects that could cause the alignment and conclude that a torque caused by a misaligned binary companion on the protoplanetary disk is the most promising explanation

Information Modeling as a Foundation for Revealing the Production Potential of an Oil Production Company

All major oil fields in the Urals and the Volga Region, Russia, are in the final stage of exploration, when oil production is becoming too costly. In the light of the novel coronavirus pandemic that has led to a reduction in oil demand, in turn resulting in limited production, optimizing the oil production costs is even more critical. This paper dwells upon developing methodological toolkit for information modeling to help identify the production potential associated with optimizing the operating costs of an oil production company; the case study uses the costs of well maintenance and repair. This methodology features little to no use of expert opinions to make the best and most sound managerial decisions. By finding the correlating indicators of oil fields in the Urals and the Volga Region, the authors apply Microsoft Excel Solver, a simplex-based linear programming solver, to comprehensively identify how the frequency and the average duration of repairs could be reduced. The authors propose organizational measures, adopting which will help optimize the well repair cycle

Improving the Efficiency of Planning

The first and one of the most important functions of management is planning. At the same time, in the current market conditions, the time for the implementation of this stage is very limited. In many ways, this applies to the oil and gas industry all the same. Due to the reduction of the resource base of the industry, the share of super-profitable projects has decreased significantly. Extraction of hard-to-recover oil and gas reserves is associated with active investment activities and with the need to introduce expensive technologies and equipment. The most common type of investment project associated with the geological and technical activities is being considered in the present paper. In order to increase the economic efficiency of the geological and technical activities it is proposed to implement an automated model at the stage of planning. This model, on the basis of the generalized geological, technological, statistical, macroeconomic and economic indicators, allows to solve quickly the following problems: of more precise and prompt planning the expenses on carrying out geological and technical actions; of defining minimum admissible profitable level of an oil flow rate after carrying out geological and technical actions; of determining the most economically justified duration of the overhaul of the well; of organizing the projects of geological and technical measures according to their attractiveness. As a result of the implementation of the automated model, an efficiency matrix for a particular field was compiled that determines the impact of the necessary investments and planned flow rate on the economic indicators of the project. The use of this matrix made it possible to exclude several inefficient geological and technical measures from the plan. The method of ranking based on the calculation of the integrated efficiency coefficient has been developed. On its basis, the issue of making optimal management decisions taking into account the impact of risk assessment in the case of projects with the same economic efficiency is solved