检索结果-内蒙古大学图书馆

arXiv 2019年

作者： Huber, Daniel Basu, Sarbani Beck, Paul Bedding, Timothy R. Buzasi, Derek Cantiello, Matteo Chaplin, William J. Christiansen, Jessie L. Cunha, Katia Egeland, Ricky Fuller, Jim García, Rafael A. Gies, Douglas R. Guzik, Joyce Hekker, Saskia Hermes, J.J. Jackiewicz, Jason Johnson, Jennifer Kawaler, Steve Metcalfe, Travis Mosser, Benoit Ness, Melissa Pinsonneault, Marc Piro, Anthony L. Aguirre, Victor Silva Soderblom, David Tayar, Jamie Brummelaar, Theo Ten Roettenbacher, Rachael Sobeck, Jennifer Trampedach, Regner Van Belle, Gerard Van Saders, Jennifer Stello, Dennis Institute for Astronomy University of Hawai'i Yale University Instituto de Astrofisica de Canarias University of Sydney Florida Gulf Coast University Center for Computational Astrophysics University of Birmingham Caltech/IPAC-NExScI University of Arizona NCAR High Altitude Observatory California Institute of Technology Astronomy Division CEA Georgia State University Los Alamos National Laboratory Max Planck Institute for Solar System Research Boston University New Mexico State University Ohio State University Iowa State University Space Science Institute Observatoire de Paris Columbia University Flatiron Institute Carnegie Observatories Aarhus University Space Telescope Science Institute Keivan Stassun Vanderbilt University University of Washington Lowell Observatory University of New South Wales

Asteroseismology is the only observational tool in astronomy that can probe the interiors of stars, and is a benchmark method for deriving fundamental properties of stars and exoplanets. Over the coming decade, space-based and ground-based observations will provide a several order of magnitude increase of solar-like oscillators, as well as a dramatic increase in the number and quality of classical pulsator observations, providing unprecedented possibilities to study stellar physics and galactic stellar populations. In this white paper, we describe key science questions and necessary facilities to continue the asteroseismology revolution into the 2020's. Copyright © 2019, The Authors. All rights reserved.

关键词： Stars

来源：评论

学校读者我要写书评

暂无评论

Why torus-unstable solar filaments experience failed eruption?

arXiv

引用

arXiv 2019年

作者： Zhou, Zhenjun Cheng, Xin Zhang, Jie Wang, Yuming Wang, Dong Liu, Lijuan Zhuang, Bin Cui, Jun School of Atmospheric Sciences Sun Yat-sen University Zhuhai Guangdong519000 China CAS Key Laboratory of Solar Activity National Astronomical Observatories Beijing100012 China CAS Center for Excellence in Comparative Planetology China School of Astronomy and Space Science Nanjing University Nanjing210093 China Max Planck Institute for Solar System Research Gottingen37077 Germany Department of Physics and Astronomy George Mason University FairfaxVA22030 United States CAS Key Laboratory of Geospace Environment Department of Geophysics and Planetary Sciences University of Science and Technology of China Hefei Anhui230026 China Department of Mathematics and Physics Anhui Jianzhu University HefeiAnhui230601 China

To investigate the factors that control the success and/or failure of solar eruptions, we study the magnetic field and 3-Dimensional (3D) configuration of 16 filament eruptions during 2010 July - 2013 February. All these events, i.e., erupted but failed to be ejected to become a coronal mass ejection (CME), are failed eruptions with the filament maximum height exceeding 100Mm. The magnetic field of filament source regions is approximated by a potential field extrapolation method. The filament 3D configuration is reconstructed from three vantage points by the observations of STEREO Ahead/Behind and SDO spacecraft. We calculate the decay index at the apex of these failed filaments and find that in 7 cases, their apex decay indexes exceed the theoretical threshold (ncrit = 1.5) of the torus instability. We further determine the orientation change or rotation angle of each filament top during the eruption. Finally, the distribution of these events in the parameter space of rotation angle versus decay index is established. Four distinct regimes in the parameter space are empirically identified. We find that, all the torus-unstable cases (decay index n > 1.5), have a large rotation angles ranging from 50◦ − 130◦. The possible mechanisms leading to the rotation and failed eruption are discussed. These results imply that, besides the torus instability, the rotation motion during the eruption may also play a significant role in solar eruptions. Copyright © 2019, The Authors. All rights reserved.

关键词： Magnetic fields

来源：评论

学校读者我要写书评

暂无评论

Summary on Network Security Visual Analysis 7

Summary on Network Security Visual Analysis

引用

2016 IEEE 7th International Conference on Software Engineering and Service science

作者： Yao Zhonghua Wu Lingda Science and Technology on Complex Electronic System Simulation Laboratory Equipment Academy

ISBN: (纸本)9781467399050

Visual analysis on network security is a new area,it consists methods and technology of visualization and network security analysis,which has new *** on network security visualization have done certain extent research and accumulated *** with the rapid development of visual analysis,visual network security analysis achieved rich results in recent ***,there is less study on basic research framework and principle of security visualization analysis,this dissertation summarizes concerned problems in the field of security analysis,data sources,visual analysis techniques and related overview of visual analysis *** analysis of these systems,network security visualization on the research questions can be tested and directions for future research can be provided.

关键词： network security visual analysis review

来源：评论

学校读者我要写书评

暂无评论

Traffic-aware Two-stage queueing communication networks: Queue analysis and energy saving

arXiv

引用

arXiv 2019年

作者： Qi, Nan Miridakis, Nikolaos I. Xiao, Ming Tsiftsis, Theodoros A. Yao, Rugui Jin, Shi Key Laboratory of Dynamic Cognitive System of Electromagnetic Spectrum Space Ministry of Industry and Information Technology Nanjing University of Aeronautics and Astronautics Nanjing210016 China National Mobile Communications Research Laboratory Southeast University Nanjing210096 China School of Electrical and Information Engineering Institute of Physical Internet Jinan University Zhuhai519070 China Department of Electrical and Electronic Engineering University of West Attica Aegaleo12244 Greece School of Electrical Engineering of KTH Royal Institute of Technology Stockholm Sweden School of Intelligence Science and Engineering Jinan University Zhuhai519070 China School of Electronics and Information Northwestern Polytechnical University China National Mobile Communications Research Lab Southeast University Nanjing China

To boost energy saving for the general delay-tolerant IoT networks, a two-stage and single-relay queueing communication scheme is investigated. Concretely, a traffic-aware Nthreshold and gated-service policy are applied at the relay. As two fundamental and significant performance metrics, the mean waiting time and long-term expected power consumption are explicitly derived and related with the queueing and service parameters, such as packet arrival rate, service threshold and channel statistics. Besides, we take into account the electrical circuit energy consumptions when the relay server and access point (AP) are in different modes and energy costs for mode transitions, whereby the power consumption model is more practical. The expected power minimization problem under the mean waiting time constraint is formulated. Tight closed-form bounds are adopted to obtain tractable analytical formulae with less computational complexity. The optimal energy-saving service threshold that can flexibly adjust to packet arrival rate is determined. In addition, numerical results reveal that: 1) sacrificing the mean waiting time not necessarily facilitates power savings;2) a higher arrival rate leads to a greater optimal service threshold;and 3) our policy performs better than the current state-of-the-art. Copyright © 2019, The Authors. All rights reserved.

关键词： Queueing theory

来源：评论

学校读者我要写书评

暂无评论

Research on the Resource Scheduling Architecture for Service-oriented space-based Information systems

Research on the Resource Scheduling Architecture for Service...

引用

2017 2nd International Conference on Computer Engineering,Information science and Internet technology(CII 2017)

作者： CHENGXIANG LIU WEI XIONG CHAO GUO Department of Graduate Management Equipment Academy Science and Technology on Complex Electronic System Simulation Laboratory Equipment Academy

On the basis of integrating each subsystem in topological structure,implementation function,operation mode and institutional mechanism,this paper has established a comprehensive service system which could manage various heterogeneous resources and handle kinds of complex missions within the architecture to carry out the research of the resource scheduling architecture for service-oriented space-based information ***,this paper analyzes the characteristics of space-based information system from two aspects of diversity and *** on the research,this paper studies the organizational structure of resource scheduling of space-based information system to realize the unified management and scheduling of service-oriented diversification resources following the sequence from resources to ***,this paper has proposed a resource scheduling mode for the service-oriented space-based information system to realize the mapping from resources to missions,and it also has used that mode to block differentiated user requirements and the dynamic changes of the *** the end,the paper has put forward the implementation plan of the resource scheduling for service-oriented space-based information system,and it also provides a reference for the next construction of the space-based information system.

关键词： Service-oriented space-based information system Resource scheduling architecture

来源：评论

学校读者我要写书评

暂无评论

ET White Paper: To Find the First Earth 2.0

arXiv

引用

arXiv 2022年

作者： Ge, Jian Zhang, Hui Zang, Weicheng Deng, Hongping Mao, Shude Xie, Ji-Wei Liu, Hui-Gen Zhou, Ji-Lin Willis, Kevin Huang, Chelsea Howell, Steve B. Feng, Fabo Zhu, Jiapeng Yao, Xinyu Liu, Beibei Aizawa, Masataka Zhu, Wei Li, Ya-Ping Ma, Bo Ye, Quanzhi Yu, Jie Xiang, Maosheng Yu, Cong Liu, Shangfei Yang, Ming Wang, Mu-Tian Shi, Xian Fang, Tong Zong, Weikai Liu, Jinzhong Zhang, Yu Zhang, Liyun El-Badry, Kareem Shen, Rongfeng Tam, Pak-Hin Thomas Hu, Zhecheng Yang, Yanlv Zou, Yuan-Chuan Wu, Jia-Li Lei, Wei-Hua Wei, Jun-Jie Wu, Xue-Feng Sun, Tian-Rui Wang, Fa-Yin Zhang, Bin-Bin Xu, Dong Yang, Yuan-Pei Li, Wen-Xiong Xiang, Dan-Feng Wang, Xiaofeng Wang, Tinggui Zhang, Bing Jia, Peng Yuan, Haibo Zhang, Jinghua Wang, Sharon Xuesong Gan, Tianjun Wang, Wei Zhao, Yinan Liu, Yujuan Chen, Yonghe Wei, Chuanxin Kang, Yanwu Yang, Baoyu Qi, Chao Liu, Xiaohua Zhang, Quan Zhu, Yuji Zhou, Dan Zhang, Congcong Yu, Yong Zhang, Yongshuai Li, Yan Tang, Zhenghong Wang, Chaoyan Wang, Fengtao Li, Wei Cheng, Pengfei Shen, Chao Li, Baopeng Pan, Yue Yang, Sen Gao, Wei Song, Zongxi Wang, Jian Zhang, Hongfei Chen, Cheng Wang, Hui Zhang, Jun Wang, Zhiyue Zeng, Feng Zheng, Zhenhao Zhu, Jie Guo, Yingfan Zhang, Yihao Li, Yudong Wen, Lin Feng, Jie Chen, Wen Chen, Kun Han, Xingbo Yang, Yingquan Wang, Haoyu Duan, Xuliang Huang, Jiangjiang Liang, Hong Bi, Shaolan Gai, Ning Ge, Zhishuai Guo, Zhao Huang, Yang Li, Gang Li, Haining Li, Tanda Lu, Yuxi Lucy Rix, Hans-Walter Shi, Jianrong Song, Fen Tang, Yanke Ting, Yuan-Sen Wu, Tao Wu, Yaqian Yang, Taozhi Yin, Qing-Zhu Gould, Andrew Lee, Chung-Uk Dong, Subo Yee, Jennifer C. Shvartzvald, Yossi Yang, Hongjing Kuang, Renkun Zhang, Jiyuan Liao, Shilong Qi, Zhaoxiang Yang, Jun Zhang, Ruisheng Jiang, Chen Ou, Jian-Wen Li, Yaguang Beck, Paul Bedding, Timothy R. Campante, Tiago L. Chaplin, William J. Christensen-Dalsgaard, Jørgen García, Rafael A. Gaulme, Patrick Gizon, Laurent Hekker, Saskia Huber, Daniel Khanna, Shourya Mathur, Savita Miglio, Andrea Mosser, Benoît Ong, J.M. Joel Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai China Tsinghua University Beijing China Nanjing University Nanjing China Sun Yat-Sen University Zhuhai China Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai China Max Planck Institute for Solar System Research Göttingen Germany Max-Planck-Institute für Astronomie Heidelberg Germany Zhejiang University Hangzhou China University of Science and Technology of China Hefei China Taiyuan University of Technology Taiyuan China University of Maryland College ParkMD United States Boston University BostonMA United States Xinjiang Astronomical Observatory Chinese Academy of Sciences Xinjiang China Huazhong University of Science and Technology Wuhan China Purple Mountain Observatories Chinese Academy of Sciences Nanjing China Guizhou University Guiyang China National Astronomical Observatories Chinese Academy of Sciences Beijing China Yunnan University Kunming China Tel Aviv University Tel Aviv Israel Science Talent Training Center Gainesville United States Shanghai Institute of Technical Physics Chinese Academy of Sciences Shanghai China Xi'An Institute of Optics and Precision Mechanics Chinese Academy of Sciences Xi'An China Innovation Academy for Microsatellites Chinese Academy of Sciences Shanghai China Department of Astronomy The University of Geneva Versoix Switzerland University of Southern Queensland QLD Australia Research School of Astronomy & Astrophysics Australian National University ACT Australia Research School of Computer Science Australian National University ACT Australia Beijing Normal University Beijing China University of Cambridge Cambridge United Kingdom Dezhou University Dezhou China Jimei University Xiamen China Ohio State University ColumbusOH United States Korea Astronomy and Space Science Institute Daejon Korea Republic of Kavli Institute for Astronomy and Astrophysics Peking University Beijing China Center for Astrophysics Harvard

The ET mission is a wide-field and ultra-high-precision photometric survey mission being developed in China. This mission is designed to measure, for the first time, the occurrence rate and the orbital distributions of Earth-sized planets. ET consists of seven 30 cm telescopes to be launched to the Earth-Sun's L2 point. Six of these are transit telescopes with a FOV of 500 square degrees. Staring in the direction that encompasses the original Kepler field for four continuous years, this monitoring will yield tens of thousands of transiting planets, including the elusive Earth twins orbiting solar-type stars. The seventh is a 30 cm microlensing telescope that will monitor an area of 4 square degrees toward the galactic bulge. Combined with simultaneous ground-based KMTNet observations, it will measure masses of hundreds of long-period and free-floating planets. Together, the transit and the microlensing telescopes will revolutionize our understanding of terrestrial planets across a large swath of orbital distances and free space. In addition, the survey data will also facilitate studies in the fields of asteroseismology, Galactic archaeology, time-domain sciences, and black holes in binaries. © 2022, CC BY-NC-ND.

关键词： Planets

来源：评论

学校读者我要写书评

暂无评论

Dynamical Accretion Flows - ALMAGAL: Flows along filamentary structures in high-mass star-forming clusters

arXiv

引用

arXiv 2024年

作者： Wells, M.R.A. Beuther, H. Molinari, S. Schilke, P. Battersby, C. Ho, P. Sánchez-Monge, Á. Jones, B. Scheuck, M.B. Syed, J. Gieser, C. Kuiper, R. Elia, D. Coletta, A. Traficante, A. Wallace, J. Rigby, A.J. Klessen, R.S. Zhang, Q. Walch, S. Beltrán, M.T. Tang, Y. Fuller, G.A. Lis, D.C. Möller, T. van der Tak, F. Klaassen, P.D. Clarke, S.D. Moscadelli, L. Mininni, C. Zinnecker, H. Maruccia, Y. Pezzuto, S. Benedettini, M. Soler, J.D. Brogan, C.L. Avison, A. Sanhueza, P. Schisano, E. Liu, T. Fontani, F. Rygl, K.L.J. Wyrowski, F. Bally, J. Walker, D.L. Ahmadi, A. Koch, P. Merello, M. Law, C.Y. Testi, L. Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany INAF-Istituto di Astrofisica e Planetologia Spaziale via Fosso del Cavaliere 100 Roma00133 Italy I. Physikalisches Institut Universität zu Köln Zülpicher Str. 77 Köln50937 Germany University of Connecticut Department of Physics 2152 Hillside Road Unit 3046 StorrsCT06269 United States Institute of Astronomy and Astrophysics Academia Sinica Taipei10617 Taiwan East Asian Observatory 660 N. A'ohoku Hilo Hawaii HI96720 United States Can Magrans s/n Bellaterra Barcelona08193 Spain Barcelona Spain Universität Heidelberg Zentrum für Astronomie Institut für Theoretische Astrophysik Heidelberg Germany Universität Heidelberg Interdisziplinäres Zentrum für Wis-senschaftliches Rechnen Heidelberg Germany Harvard-Smithsonian Center for Astrophysics 160 Garden St CambridgeMA02420 United States Center for Data and Simulation Science University of Cologne Germany INAF - Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 Firenze50125 Italy Jodrell Bank Centre for Astrophysics UK ALMA Regional Centre Node School of Physics & Astronomy University of Manchester M13 9PL United Kingdom Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States SRON Netherlands Institute for Space Research Landleven 12 Groningen9747 AD Netherlands Kapteyn Astronomical Intsitute University of Groningen Netherlands UK Astronomy Technology Centre Royal Observatory Edinburgh Blackford Hill EdinburghEH9 3HJ United Kingdom 520 Edgemont Rd CharlottesvilleVA22903 United States UK ALMA Regional Centre Node M13 9PL United Kingdom SKA Observatory Jodrell Bank Lower Withington MacclesfieldSK11 9FT United Kingdom National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Tokyo Mitaka181-8588 Japan 2-21-1 Osawa Tokyo Mitaka181-8588 Japan Dipartimento di Fisica Universita di Roma La Sapienza Piazzale

Context. Investigation of the flow of material along filamentary structures towards the central core can help provide insight into high-mass star formation and evolution. Aims. Our main motivation is to answer the question: what are the properties of accretion flows in star-forming clusters? We use data from the ALMA Evolutionary Study of High Mass Protocluster Formation in the Galaxy (ALMAGAL) survey to study 100 ALMAGAL regions at ∼ 1′′ resolution located between ∼ 2 and 6 kpc distance. Methods. Making use of the ALMAGAL ∼ 1.3mm line and continuum data we estimate flow rates onto individual cores. We focus specifically on flow rates along filamentary structures associated with these cores. Our primary analysis is centered around position velocity cuts in H2CO (30,3 - 20,2) which allow us to measure the velocity fields, surrounding these cores. Combining this work with column density estimates we derive the flow rates along the extended filamentary structures associated with cores in these regions. Results. We select a sample of 100 ALMAGAL regions covering four evolutionary stages from quiescent to protostellar, Young Stellar Objects (YSOs), and Hii regions (25 each). Using dendrogram and line analysis, we identify a final sample of 182 cores in 87 regions. In this paper, we present 728 flow rates for our sample (4 per core), analysed in the context of evolutionary stage, distance from the core, and core mass. On average, for the whole sample, we derive flow rates on the order of ∼10−4 M☉yr−1 with estimated uncertainties of ±50%. We see increasing differences in the values among evolutionary stages, most notably between the less evolved (quiescent/protostellar) and more evolved (YSO/Hii region) sources and we also see an increasing trend as we move further away from the centre of these cores. We also find a clear relationship between the calculated flow rates and core masses ∼M2/3 which is in line with the result expected from the tidal-lobe accretion mechanism. T

关键词： Giant stars

来源：评论

学校读者我要写书评

暂无评论

Eden: Sensitivity analysis and transiting planet detection limits for nearby late red dwarfs

arXiv

引用

arXiv 2020年

作者： Gibbs, Aidan Bixel, Alex Rackham, Benjamin V. Apai, Dániel Schlecker, Martin Espinoza, Néstor Mancini, Luigi Chen, Wen-Ping Henning, Thomas Gabor, Paul Boyle, Richard Chavez, Jose Perez Mousseau, Allie Dietrich, Jeremy Socia, Quentin Jay Ip, Wing Ngeow, Chow-Choong Tsai, Anli Bhandare, Asmita Marian, Victor Baehr, Hans Brown, Samantha Häberle, Maximilian Keppler, Miriam Molaverdikhani, Karan Sarkis, Paula Steward Observatory University of Arizona 933 N. Cherry Avenue TucsonAZ85721 United States Department of Physics & Astronomy University of California Los Angeles Los AngelesCA90095 United States NASA Nexus For Exoplanetary System Science: Earths in Other Solar Systems Team Department of Earth Atmospheric and Planetary Sciences Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology 77 Massachusetts Ave. CambridgeMA02139 United States Lunar and Planetary Laboratory University of Arizona 1640 E. University Boulevard TucsonAZ85718 United States Max Planck Institute for Astronomy Konigstuhl 17 HeidelbergD-69117 Germany Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Department of Physics University of Rome Tor Vergata Via della Ricerca Scientifica 1 RomeI-00133 Italy INAF Osservatorio Astrofisico di Torino via Osservatorio 20 Pino TorineseI-10025 Italy I-84019 Italy Graduate Institute of Astronomy National Central University 300 Jhongda Road Zhongli Taoyuan32001 Taiwan Vatican Observatory Research Group University of Arizona 933 N Cherry Ave. TucsonAZ85721-0065 United States

Small planets are common around late-M dwarfs and can be detected through highly precise photometry by the transit method. Planets orbiting nearby stars are particularly important as they are often the best-suited for future follow-up studies. We present observations of three nearby M-dwarfs referred to as EIC-1, EIC-2, and EIC-3, and use them to search for transits and set limits on the presence of planets. On most nights our observations are sensitive to Earth-sized transiting planets, and photometric precision is similar to or better than TESS for faint late-M dwarfs of the same magnitude (I ≈ 15 mag). We present our photometry and transit search pipeline, which utilizes simple median detrending in combination with transit least squares based transit detection (Hippke & Heller 2019). For these targets, and transiting planets between one and two Earth radii, we achieve an average transit detection probability of∼60% between periods of 0.5 and 2 days, ∼30% between 2 and 5 days, and ∼10% between 5 and 10 days. These sensitivities are conservative compared to visual searches. Copyright © 2020, The Authors. All rights reserved.

关键词： Photometry

来源：评论

学校读者我要写书评

暂无评论

A development and application of maintainability evaluation system using immersive VR

引用

IOP Conference Series: Materials science and Engineering 2019年第1期658卷

作者： Meihui Wang Yongxiang Li Chuan Lyu Xi Liu School of Reliability and Systems Engineering Beihang University China State Key Laboratory of Virtual Reality Technology System Beihang University China Technology and Engineering Center for Space Utilization Chinese Academy of Science Beijing China Xi'an Modern Control Technology Research Institute Xi'an 710065 China

Immersing into virtual reality (VR) is a perception of being physically present in a non-physical world. Using immersive VR in maintenance brings great conveniences. For example, using virtual human operating in hazardous environment before the real person, which can prevent being hurt. In this paper, a system of immersive virtual maintenance (IVM) is presented. It is divided into three parts. The first part is Input, which contains the maintenance task and maintenance design. The second part is Method, with which making the virtual human and the users act in a unified way. The key to build IVM system is the interface between the motion capture system and virtual simulation software. The third part is Output, which presents the maintainability evaluation results. This paper focuses on how to build IVM system, the difficulties and solutions also be detailed. At last, a simple application is given

关键词：

来源：评论

学校读者我要写书评

暂无评论

Accurate spectral super-resolution from single RGB image using multi-scale CNN

arXiv

引用

arXiv 2018年

作者： Yan, Yiqi Zhang, Lei Li, Jun Zhang, Yanning Wei, Wei School of Electronics and Information Northwestern Polytechnical University Xi'an China School of Computer Science Northwestern Polytechnical University Xi'an China National Engineering Laboratory for Integrated Aero-Space-Ground-Ocean Big Data Application Technology China Guangdong Provincial Key Laboratory of Urbanization and Geo-simulation School of Geography and Planning Sun Yat-Sen University Guangzhou China

Different from traditional hyperspectral super-resolution ap-proaches that focus on improving the spatial resolution, spectral super-resolution aims at producing a high-resolution hyperspectral image from the RGB observation with super-resolution in spectral domain. However, it is challenging to accurately reconstruct a high-dimensional continuous spectrum from three discrete intensity values at each pixel, since too much information is lost during the procedure where the latent hyper-spectral image is downsampled (e.g., with ×10 scaling factor) in spectral domain to produce an RGB observation. To address this problem, we present a multi-scale deep convolutional neural network (CNN) to ex-plicitly map the input RGB image into a hyperspectral image. Through symmetrically downsampling and upsampling the intermediate feature maps in a cascading paradigm, the local and non-local image informa-tion can be jointly encoded for spectral representation, ultimately im-proving the spectral reconstruction accuracy. Extensive experiments on a large hyperspectral dataset demonstrate the effectiveness of the pro-posed method. Copyright © 2018, The Authors. All rights reserved.

关键词： Optical resolving power

来源：评论

学校读者我要写书评

暂无评论

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案：

请选择收藏分类：

通借通还

建议与咨询 留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案： 新增检索档案 确定 取消

请选择收藏分类： 新增自定义分类 确定 取消

通借通还

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

请选择保存的检索档案：

请选择收藏分类：