检索结果-内蒙古大学图书馆

arXiv 2017年

作者： Hong, Shanwei Xiong, Dingrong Bai, Jinming Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China University of Chinese Academy of Sciences Beijing100049 China Department of Mathematics and Computer Science Lijiang Teachers College Lijiang674199 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China

We have monitored the BL Lacertae object S5 0716+714 in the optical bands during 2012 January and February with long time spans on intraday timescales (>5 hr) and high time resolutions. During this monitoring period, the object shows violent flaring activity both in short and intraday timescales. The object has high value of duty cycle. The light curves detected as intraday variability (IDV) show variability of various shapes. The variability amplitude is from 12.81 per cent to 33.22 per cent, and the average value 19.92 ± 5.87 per cent. The overall magnitude variabilities are ΔB = 1m.24, ΔV = 1m.42, ΔR = 1m.3, ΔI = 1m.23 respectively. During the observations, the average change rate is = 0.035 ± 0.009 Mag/h during the ascent and = 0.035 ± 0.014 Mag/h during the descent. However, different cases are found on certain nights. There are good inter-bands correlations but not significant time lags for intraday and short timescales. The results of the autocorrelation function show that the variability timescales range from 0.054 day to 0.134 day. Most of nights show bluer when brighter (BWB) chromatic trend;a weak redder with brighter (RWB) trend is found;a few nights show no correlations between magnitude and color index. The BWB trend appears in the short timescales. During the flare the spectral index exhibits a clockwise loop for inter-nights. A shock-in-jet model and the shock wave propagating along a helical path are likely to explain the variability and color index variability. Copyright © 2017, The Authors. All rights reserved.

关键词： Shock waves

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The orbital period – mass ratio relation of wide sdB+MS binaries and its application to the stability of RLOF.

arXiv

引用

arXiv 2018年

作者： Vos, Joris Vucković, Maja Chen, Xuefei Han, Zhanwen Boudreaux, Thomas Barlow, Brad N. Østensen, Roy Németh, Péter Instituto de Física y Astronomía Universidad de Valparaiso Gran Bretaña 1111 Playa Ancha Valparaíso2360102 Chile Institut für Physik und Astronomie Universität Potsdam Karl-Liebknecht-Str. 24/25 Golm14476 Germany Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Department of Physics High Point University One University Parkway High PointNC27268 United States Department of Physics Astronomy and Materials Science Missouri State University SpringfieldMO65804 United States Astronomical Institute of the Czech Academy of Sciences OndřejovCZ-25165 Czech Republic *** Malomsok8533 Hungary

Wide binaries with hot subdwarf-B (sdB) primaries and main sequence companions are thought to form only through stable Roche lobe overflow (RLOF) of the sdB progenitor near the tip of the red giant branch (RGB). We present the orbital parameters of eleven new long period composite sdB binaries based on spectroscopic observations obtained with the UVES, FEROS and CHIRON spectrographs. Using all wide sdB binaries with known orbital parameters, 23 systems, the observed period distribution is found to match very well with theoretical predictions. A second result is the strong correlation between the orbital period (P) and the mass ratio (q) in the observed wide sdB binaries. In the P-q plane two distinct groups emerge, with the main group (18 systems) showing a strong correlation of lower mass ratios at longer orbital periods. The second group are systems that are thought to be formed from higher mass progenitors. Based on theoretical models, a correlation between the initial mass ratio at the start of RLOF and core mass of the sdB progenitor is found, which defines a mass-ratio range at which RLOF is stable on the RGB. Copyright © 2018, The Authors. All rights reserved.

关键词： Giant stars

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ET White Paper: To Find the First Earth 2.0

arXiv

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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

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Binary population synthesis for the core-degenerate scenario of type Ia supernova progenitors

引用

Research in Astronomy and Astrophysics 2015年第10期15卷 1701-1712页

作者： Wei-Hong Zhou Bo Wang Xiang-Cun Meng Dong-Dong Liu Gang Zhao Key Laboratory of Optical Astronomy National Astronomical ObservatoriesChinese Academy of Sciences University of Chinese Academy of Sciences Yunnan Minzu University Yunnan Observatories Chinese Academy of Sciences Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences

The core-degenerate （CD） scenario has been suggested to be a possible progenitor model of type Ia supernovae （SNe Ia）, in which a carbon-oxygen white dwarf merges with the hot CO core of a massive asymptotic giant branch star dur- ing their common-envelope phase. However, the SN Ia birthrates for this scenario are still uncertain. We conducted a detailed investigation into the CD scenario and then gave the birthrates for this scenario using a detailed Monte Carlo binary pop- ulation synthesis approach. We found that the delay times of SNe Ia from this sce- nario are -70 Myr- 1400 Myr, which means that the CD scenario contributes to young SN Ia populations. The Galactic SN Ia birthrates for this scenario are in the range of ~7.4×10^-5 yr^-1- 3.7 × 10^-4 yr^-1, which roughly accounts for -2%-10% of all SNe Ia. This indicates that, under the assumptions made here, the CD scenario only contributes a small portion of all SNe Ia, which is not consistent with the results of Ilkov ＆ Soker.

关键词： binaries： close -- stars： evolution -- supernovae： general

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BROAD ABSORPTION LINE DISAPPEARANCE/EMERGENCE IN MULTIPLE IONS IN A WEAK EMISSION-LINE QUASAR

arXiv

引用

arXiv 2018年

作者： Yi, W. Vivek, M. Brandt, W.N. Wang, T. Timlin, J. Filiz Ak, N. Schneider, D.P. Fynbo, J.P.U. Ni, Q. Vito, F. Indahl, B.L. Sameer Department of Astronomy & Astrophysics Pennsylvania State University 525 Davey Lab University ParkPA16802 United States Yunnan Observatories Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Institute for Gravitation and the Cosmos Pennsylvania State University University ParkPA16802 United States Department of Physics Pennsylvania State University University ParkPA16802 United States CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China China Faculty of Sciences Department of Astronomy and Space Sciences Erciyes University Kayseri38039 Turkey Astronomy and Space Sciences Observatory and Research Center Erciyes University Kayseri38039 Turkey Niels Bohr Institute University of Copenhagen DTU-Space Technical University of Denmark Juliane Maries Vej 30 DK-2100 Copenhagen Ø Kgs. LyngbyDK-2800 Denmark Instituto de Astrofsica and Centro de Astroingeniera Facultad de Fsica Pontificia Universidad Catolica de Chile Casilla 306 Santiago 22 Chile Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100012 China Department of Astronomy University of Texas AustinTX78712 United States

We report the discovery of disappearance of Mg ii, Al iii, C iv, and Si iv broad absorption lines (BALs) at the same velocity (0.07c), accompanied by a new C iv BAL emerging at a higher velocity (up to 0.11c), in the quasar J0827+4252 at z = 2.038. This is the first report of BAL disappearance (i) over Mg ii, Al iii, C iv, and Si iv ions and (ii) in a weak emission-line quasar (WLQ). The discovery is based on four spectra from the SDSS and one follow-up spectrum from HET/LRS2. The simultaneous C iv BAL disappearance and emergence at different velocities, together with no variations in the CRTS light curve, indicate that ionization changes in the absorbing material are unlikely to cause the observed BAL variability. Our analyses reveal that transverse motion is the most likely dominant driver of the BAL disappearance/emergence. Given the presence of mildly relativistic BAL outflows and an apparently large C iv emission-line blueshift that is likely associated with strong bulk outflows in this WLQ, J0827+4252 provides a notable opportunity to study extreme quasar winds and their potential in expelling material from inner to large-scale regions. Copyright © 2018, The Authors. All rights reserved.

关键词： Galaxies

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A 20-second cadence view of solar-type stars and their planets with TESS: Asteroseismology of solar analogs and a re-characterization of π

arXiv

引用

arXiv 2021年

作者： Huber, Daniel White, Timothy R. Metcalfe, Travis S. Chontos, Ashley Fausnaugh, Michael M. Ho, Cynthia S.K. van Eylen, Vincent Ball, Warrick H. Basu, Sarbani Bedding, Timothy R. Benomar, Othman Bossini, Diego Breton, Sylvain Buzasi, Derek L. Campante, Tiago L. Chaplin, William J. Christensen-Dalsgaard, Jørgen Cunha, Margarida S. Deal, Morgan García, Rafael A. Muñoz, Antonio García Gehan, Charlotte González-Cuesta, Lucía Jiang, Chen Kayhan, Cenk Kjeldsen, Hans Lundkvist, Mia S. Mathis, Stéphane Mathur, Savita Monteiro, Mário J.P.F.G. Nsamba, Benard Ong, Jia Mian Joel Pakštiene, Erika Serenelli, Aldo M. Aguirre, Victor Silva Stassun, Keivan G. Stello, Dennis Stilling, Sissel Norgaard Winther, Mark Lykke Wu, Tao Barclay, Thomas Daylan, Tansu Günther, Maximilian N. Hermes, J.J. Jenkins, Jon M. Latham, David W. Levine, Alan M. Ricker, George R. Seager, Sara Shporer, Avi Twicken, Joseph D. Vanderspek, Roland K. Winn, Joshua N. Institute for Astronomy University of Hawai‘i 2680 Woodlawn Drive HonoluluHI96822 United States School of Physics University of Sydney NSW2006 Australia Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark White Dwarf Research Corporation 9020 Brumm Trail GoldenCO80403 United States Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology 77 Massachusetts Ave. CambridgeMA02139 United States Mullard Space Science Laboratory University College London Holmbury St Mary Dorking Surrey RH5 6NT United Kingdom School of Physics and Astronomy University of Birmingham BirminghamB15 2TT United Kingdom Department of Astronomy Yale University P.O. Box 208101 New HavenCT06520-8101 United States Center for Space Science New York University Abu Dhabi United Arab Emirates Division of Solar and Plasma Astrophysics NAOJ Mitaka Tokyo Japan Instituto de Astrofísica e Ciências do Espaço Universidade do Porto CAUP Rua das Estrelas Porto4150-762 Portugal AIM CEA CNRS Université Paris-Saclay Université Paris Diderot Sorbonne Paris Cité Gif-sur-YvetteF-91191 France Dept. of Chemistry & Physics Florida Gulf Coast University 10501 FGCU Blvd. S. Fort MyersFL33965 United States Departamento de Física e Astronomia Faculdade de Ciências da Universidade do Porto Rua do Campo Alegre s/n Porto4169-007 Portugal Max-Planck-Institut für Sonnensystemforschung Justus-von-Liebig-Weg 3 Göttingen37077 Germany Tenerife La Laguna38205 Spain Departamento de Astrofísica Tenerife La LagunaE-38206 Spain Department of Astronomy and Space Sciences Science Faculty Erciyes University Melikgazi Kayseri38030 Turkey Institute of Theoretical Physics and Astronomy Vilnius University Sauletekio av. 3 Vilnius10257 Lithuania Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Str. 1 GarchingD-85748 Germany Instituto de Astrofísica e Ciências do Espaço Universidade d

We present an analysis of the first 20-second cadence light curves obtained by the TESS space telescope during its extended mission. We find a precision improvement of 20-second data compared to 2-minute data for bright stars when binned to the same cadence (≈ 10-25% better for T . 8 mag, reaching equal precision at T ≈ 13 mag), consistent with pre-flight expectations based on differences in cosmic ray mitigation algorithms. We present two results enabled by this improvement. First, we use 20-second data to detect oscillations in three solar analogs (γ Pav, ζ Tuc and π Men) and use asteroseismology to measure their radii, masses, densities and ages to ≈ 1%, ≈ 3%, ≈ 1% and ≈ 20% respectively, including systematic errors. Combining our asteroseismic ages with chromospheric activity measurements we find evidence that the spread in the activity-age relation is linked to stellar mass and thus convection-zone depth. Second, we combine 20-second data and published radial velocities to re-characterize π Men c, which is now the closest transiting exoplanet for which detailed asteroseismology of the host star is possible. We show that π Men c is located at the upper edge of the planet radius valley for its orbital period, confirming that it has likely retained a volatile atmosphere and that the "asteroseismic radius valley’ remains devoid of planets. Our analysis favors a low eccentricity for π Men c (2,1 . 2400) if it formed via high-eccentricity migration. Combined, these early results demonstrate the strong potential of TESS 20-second cadence data for stellar astrophysics and exoplanet science. Copyright © 2021, The Authors. All rights reserved.

关键词： Extrasolar planets

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Carbon stars identified from LAMOST DR4 using machine learning

arXiv

引用

arXiv 2017年

作者： Li, Yin-Bi Luo, A-Li Du, Chang-De Zuo, Fang Wang, Meng-Xin Zhao, Gang Jiang, Bi-Wei Zhang, Hua-Wei Liu, Chao Qin, Li Wang, Rui Du, Bing Guo, Yan-Xin Wang, Bo Han, Zhan-Wen Xiang, Mao-Sheng Huang, Yang Chen, Bing-Qiu Chen, Jian-Jun Kong, Xiao Hou, Wen Song, Yi-Han Wang, You-Fen Wu, Ke-Fei Zhang, Jian-Nan Zhang, Yong Wang, Yue-Fei Cao, Zi-Huang Hou, Yong-Hui Zhao, Yong-Heng Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China University of Chinese Academy of Sciences Beijing100049 China Beijing100190 China Department of Astronomy Beijing Normal University Beijing100875 China Department of Astronomy School of Physics Peking University Beijing100871 China Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories Chinese Academy of Sciences Kunming650216 China South-Western Institute for Astronomy Research Yunnan University Kunming650500 China LAMOST Fellow Nanjing Institute of Astronomical Optics & Technology National Astronomical Observatories Chinese Academy of Sciences Nanjing210042 China

In this work, we present a catalog of 2651 carbon stars from the fourth Data Release (DR4) of the Large Sky Area Multi-object Fiber Spectroscopy Telescope (LAMOST). Using an efficient machine-learning algorithm, we find out these stars from more than seven million spectra. As a by-product, 17 carbon-enhanced metal-poor (CEMP) turnoff star candidates are also reported in this paper, and they are preliminarily identified by their atmospheric parameters. Except for 176 stars that could not be given spectral types, we classify the other 2475 carbon stars into five subtypes including 864 C-H, 226 C-R, 400 C-J, 266 C-N, and 719 barium stars based on a series of spectral features. Furthermore, we divide the C-J stars into three subtypes of CJ(H), C-J(R), C-J(N), and about 90% of them are cool N-type stars as expected from previous literature. Beside spectroscopic classification, we also match these carbon stars to multiple broadband photometries. Using ultraviolet photometry data, we find that 25 carbon stars have FUV detections and they are likely to be in binary systems with compact white dwarf companions. Copyright © 2017, The Authors. All rights reserved.

关键词： White dwarfs

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R-band host galaxy contamination of TeV γ-ray blazar Mrk 501: effects of the aperture size and seeing

arXiv

引用

arXiv 2017年

作者： Feng, Hai-Cheng Liu, Hong-Tao Zhao, Ying-He Bai, Jin-Ming Wang, Fang Fan, Xu-Liang Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China University of Chinese Academy of Sciences Beijing100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China School of Physics and Space Science China West Normal University Nanchong637009 China School of Physics Huazhong University of Science and Technology Wuhan430074 China

We simulated the R-band contribution of the host galaxy of TeV γ-ray BL Lac object Mrk 501 in different aperture sizes and seeing conditions . The intensive observations were run with the 1.02 m optical telescope at Yunnan Observatories from 2010 May 15 to 18. Based on the host subtraction data presented in Nilsson et al. (2007), the subtraction of host galaxy contamination results in significant seeing-brightness correlations. These correlations would lead to illusive large amplitude variations at short timescales, which will mask the intrinsic micro variability, thus gives rise to difficulty in detecting the intrinsic micro variability. Both aperture size and seeing condition influence the flux measurements, but aperture size impact the result more significantly. Based on the parameters of elliptical galaxy provided in Nilsson et al. (1999), we simulated the host contributions of Mrk 501 in the different aperture sizes and seeing conditions. Our simulation data of the host galaxy obviously weaken these significant seeing-brightness correlations for the host-subtracted brightness of Mrk 501, and can help us discover the intrinsic short timescale micro variability. The pure nuclear flux is ∼ 8.0 mJy in R band, i.e., AGN has a magnitude of R ∼ 13m· 96. Copyright © 2017, The Authors. All rights reserved.

关键词： Luminance

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Small fire smoke region location and recognition in satellite image

Small fire smoke region location and recognition in satellit...

引用

International Congress on Image and Signal Processing, BioMedical Engineering and Informatics (CISP-BMEI)

作者： Sheng Miao Kunrong Hu Hao Gao Xiaorui Wang Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming China Southwest Forestry University Kunming China Radio astronomy research group Yunnan observatory of Chinese academy of science Kunming China

ISBN: (纸本)9781509037117

Since ancient times, forest fires are an important threat to human beings, with the development of satellite technology, forest fires can be constantly monitored by satellite. But face to number of satellite pictures, its hard to detect fire location, especially the fire initial stage. An sub-region detection method has been proposed, this method supply fast partition domain detection method using information entropy, fast detect each sub-region whether there is smoke feature or not. Due to the satellite image has large region, our method first segment the image and then detect the smoke feature in each sub-region using information entropy. More than 50 pictures has been used to test this methods, shows this algorithm the effectiveness of small range fire detection.

关键词： Histograms Satellites Fires Entropy Satellite broadcasting Clouds Information entropy

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Strip Smoke and Cloud Recognition in Satellite Image

Strip Smoke and Cloud Recognition in Satellite Image

引用

International Congress on Image and Signal Processing, BioMedical Engineering and Informatics (CISP-BMEI)

作者： Sheng Miao Hong Lin Hao Gao Liang Dong Southwest Forestry University Kunming China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming China Radio astronomy research group Yunnan observatory of Chinese academy of science Kunming China

ISBN: (纸本)9781509037117

Forest fire detection based on the satellite image is an important method for fire warning. In the early stage of the forest fire, smoke is a key feature to detect. But both the smoke and cloud are mist shape, which has similar shape. For most smoke satellite image, The smoke is in the shape of a strip, for this feature, an method using edge detection to recognize smoke and cloud has been proposed. This algorithm detect the region covered with mist, and recognize the shape of the mist area using edge detection, to effectively recognize cloud and smoke. More than 30 images with cloud and strip smoke are used to test this method show the method can effectively detect strip smoke.

关键词： Shape Satellites Histograms Strips Image edge detection Satellite broadcasting

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