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Phosphorus oxoanion-intercalated layered double hydroxides for high-performance oxygen evolution

Nano Research 2017年第5期10卷 1732-1739页

作者： Ma luo zhao Cai Cheng Wang yongmin Bi li Qian yongchao Hao li li Yun Kuang Yaping li Xiaodong Lei Ziyang HUO Wen liu Hailiang Wang Xiaoming Sun Xue Duan State Key Laboratory of Chemical Resource Engineering College of Energy Beijing Advanced Innovation Center for Soft Matter Science and Engineering Beijing University of Chemical Technology Beijing 100029 China Department of Chemistry and Energy sciences Institute Yale University 810 West Campus Drive West Haven CT 06516 USA chinese Research academy of Environmental sciences Beijing 100012 China Queensland Micro- and Nanotechnology Centre Griffith University Brisbane QLD4109 Australia These authors contributed equally to this work.

Rational design and controlled fabrication of efficient and cost-effective electrodes for the oxygen evolution reaction （OER） are critical for addressing the unpre- cedented energy crisis. Nickel-iron layered double hydroxides （NiFe-LDHs） with specific interlayer anions （i.e. phosphate, phosphite, and hypophosphite） were fabricated by a co-predpitation method and investigated as oxygen evolution electrocatalysts. Intercalation of the phosphorus oxoanion enhanced the OER activity in an alkaline solution; the optimal performance （i.e., a low onset potential of 215 mV, a small Tafel slope of 37.7 mV/dec, and stable electrochemical behavior） was achieved with the hypophosphite-intercalated NiFe-LDH catalyst, demonstrating dramatic enhancement over the traditional carbonate-intercalated NiFe-LDH in terms of activity and durability. This enhanced performance is attributed to the interaction between the intercalated phosphorous oxoanions and the edge-sharing MO6 （M = Ni, Fe） layers, which modifies the surface electronic structure of the Ni sites. This concept should be inspiring for the design of more effective LDH-based oxygen evolution electrocatalvsts.

关键词： layered double hydroxide oxygen evolution reaction phosphate phosphite hypophosphite

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The Chemical Composition of the Field Zero-Age Star HD 77407

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chinese Journal of Astronomy and Astrophysics 2007年第3期7卷 405-414页

作者： Xue-liang Zhu Jian-Rong Shi Gang zhao Ji li Qing-Xiang Nie College of Physics and Electronics Shandong Normal University Jinan 250014 national astronomical observatories Chinese Academy of Sciences Beijing 100012 Department of Physics Hebei Normal University Shijiazhuang 050016

High-resolution optical spectra of the zero age star HD77407 are analysed and its li, C, O, Na, Mg, Al, Si, K, Ca, Sc, Ti, V, Co, Ni and Ba contents are determined using spectral synthesis method. The temperature of the star is determined by fitting the Hα line wings. The parameters derived for this star are Teff=5900 K, log g=4.47 and [Fe/H] = ＋0.07. It is found that the derived iron content is slightly higher than what is given in the published literature. This star shows a relative overabundances of Ca and Ba, and underabundances of Na, V and Ni with respect to the solar mix. Activity of the star is indicated by the filled in Hα and Ca Ⅱ triplet line cores. It has been confirmed that our spectroscopic approach yields fairly reliable and consistent results for active stars.

关键词： stars abundances- stars ZAMS - stars individual HD77407

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Deep Learning Applications Based on WISE Infrared Data:Classification of Stars,Galaxies and Quasars

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Research in Astronomy and Astrophysics 2023年第8期23卷 164-177页

作者： Guiyu zhao Bo Qiu A-li luo Xiaoyu Guo lin Yao Kun Wang Yuanbo liu School of Electronic and Information Engineering Hebei University of TechnologyTianjin 300401China CAS Key Laboratory of Optical Astronomy National Astronomical ObservatoriesBeijing 100101China University of chinese academy of sciences Beijing 100049China

The Wide-field Infrared Survey Explorer(WISE)has detected hundreds of millions of sources over the entire ***,classifying them reliably is a great challenge due to degeneracies in WISE multicolor space and low detection levels in its two longest-wavelength *** this paper,the deep learning classification network,IICnet(Infrared Image Classification network),is designed to classify sources from WISE images to achieve a more accurate classification *** shows good ability on the feature extraction of the WISE *** demonstrate that the classification results of IICnet are superior to some other methods;it has obtained 96.2%accuracy for galaxies,97.9%accuracy for quasars,and 96.4%accuracy for stars,and the Area Under Curve of the IICnet classifier can reach more than 99%.In addition,the superiority of IICnet in processing infrared images has been demonstrated in the comparisons with VGG16,GoogleNet,ResNet34,Mobile Net,EfficientNetV2,and RepVGG-fewer parameters and faster *** above proves that IICnet is an effective method to classify infrared sources.

关键词： methods data analysis-techniques image processing-infrared general

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Evidence for particle acceleration approaching PeV energies in the W51 complex

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Science Bulletin 2024年第18期69卷 2833-2841页

作者： LHAASO Collaboration Zhen Cao F.Aharonian Axikegu Y.X.Bai Y.W.Bao D.Bastieri X.J.Bi Y.J.Bi W.Bian A.V.Bukevich Q.Cao W.Y.Cao Zhe Cao J.Chang J.F.Chang A.M.Chen E.S.Chen H.X.Chen liang Chen lin Chen Long Chen M.J.Chen M.L.Chen Q.H.Chen S.Chen S.H.Chen S.Z.Chen T.L.Chen Y.Chen N.Cheng Y.D.Cheng M.Y.Cui S.W.Cui X.H.Cui Y.D.Cui B.Z.Dai H.L.Dai Z.G.Dai Danzengluobu X.Q.Dong K.K.Duan J.H.Fan Y.Z.Fan J.Fang J.H.Fang K.Fang C.F.Feng H.Feng L.Feng S.H.Feng X.T.Feng Y.Feng Y.L.Feng S.Gabici B.Gao C.D.Gao Q.Gao W.Gao W.K.Gao M.M.Ge L.S.Geng G.Giacinti G.H.Gong Q.B.Gou M.H.Gu F.L.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han M.Hasan H.H.He H.N.He J.Y.He Y.He Y.K.Hor B.W.Hou C.Hou X.Hou H.B.Hu Q.Hu S.C.Hu D.H.Huang T.Q.Huang W.J.Huang X.T.Huang X.Y.Huang Y.Huang X.L.Ji H.Y.Jia K.Jia K.Jiang X.W.Jiang Z.J.Jiang M.Jin M.M.Kang I.Karpikov D.Kuleshov K.Kurinov B.B.li C.M.li Cheng li Cong li D.li F.li H.B.li H.C.li Jian li Jie li K.li S.D.li W.L.li W.L.li X.R.li Xin li Y.Z.li Zhe li Zhuo li E.W.liang Y.F.liang S.J.lin B.liu C.liu D.liu D.B.liu H.liu H.D.liu J.liu J.L.liu M.Y.liu R.Y.liu S.M.liu W.liu Y.liu Y.N.liu Q.luo Y.luo H.K.Lv B.Q.Ma L.L.Ma X.H.Ma J.R.Mao Z.Min W.Mitthumsiri H.J.Mu Y.C.Nan A.Neronov L.J.Ou P.Pattarakijwanich Z.Y.Pei J.C.Qi M.Y.Qi B.Q.Qiao J.J.Qin A.Raza D.Ruffolo A.Sáiz M.Saeed D.Semikoz L.Shao O.Shchegolev X.D.Sheng F.W.Shu H.C.Song Yu.V.Stenkin V.Stepanov Y.Su D.X.Sun Q.N.Sun X.N.Sun Z.B.Sun J.Takata P.H.T.Tam Q.W.Tang R.Tang Z.B.Tang W.W.Tian C.Wang C.B.Wang G.W.Wang H.G.Wang H.H.Wang J.C.Wang Kai Wang Kai Wang L.P.Wang L.Y.Wang P.H.Wang R.Wang W.Wang X.G.Wang X.Y.Wang Y.Wang Y.D.Wang Y.J.Wang Z.H.Wang Z.X.Wang Zhen Wang Zheng Wang D.M.Wei J.J.Wei Y.J.Wei T.Wen C.Y.Wu H.R.Wu Q.W.Wu S.Wu X.F.Wu Y.S.Wu S.Q.Xi J.Xia G.M.Xiang D.X.Xiao G.Xiao Y.L.Xin Y.Xing D.R.Xiong Z.Xiong D.L.Xu R.F.Xu R.X.Xu W.L.Xu L.Xue D.H.Yan J.Z.Yan T.Yan C.W.Yang C.Y.Yang F.Yang F.F.Yang L.L.Yang M.J.Yang R.Z.Yang W.X.Yang Y.H.Yao Z.G.Yao L.Q.Yin N.Yin X.H.You Z.Y.You Y.H.Yu Q.Yuan H.Yue H.D.Zeng T.X.Zeng W.Zeng M.Zha B.B.Zhang F.Zhang H.Zhang 不详 Key Laboratory of Particle Astrophysics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of chinese academy of sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduChina Dublin Institute for Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-Planck-Institut for Nuclear Physics P.O.Box 103980Heidelberg 69029Germany School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Center for Astrophysics Guangzhou UniversityGuangzhou 510006China Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China Institute for Nuclear Research of Russian academy of sciences Moscow 117312Russia Hebei Normal University Shijiazhuang 050024China University of Science and Technology of China Hefei 230026China State Key Laboratory of Particle Detection and Electronics China Key Laboratory of Dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Research Center for astronomical Computing Zhejiang LaboratoryHangzhou 311121China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China School of Physics and Astronomy Yunnan UniversityKunming 650091China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000China national astronomical observatories Chinese Academy of SciencesBeijing 100101China School of Physics and Astronomy(Zhuhai)&School of Physics(Guangzhou)&Sino-French Institute of Nuclear Engineering and Technology(Zhuhai) Sun Yat-sen UniversityZhuhai 519000&Guangzhou 510275GuangdongChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China APC UniversitéParis Cité

Theγ-ray emission from the W51 complex is widely acknowledged to be attributed to the interaction between the cosmic rays(CRs)accelerated by the shock of supernova remnant(SNR)W51C and the dense molecular clouds in the adjacent star-forming region,***,the maximum acceleration capability of W51C for CRs remains *** on observations conducted with the Large High Altitude Air Shower Observatory(LHAASO),we report a significant detection ofγrays emanating from the W51 complex,with energies from 2 to 200 *** LHAASO measurements,for the first time,extend theγ-ray emission from the W51 complex beyond 100 TeV and reveal a significant spectrum bending at tens of *** combining the"π^(0)-decay bump"featured data from Fermi-LAT,the broadbandγ-ray spectrum of the W51 region can be well-characterized by a simple pp-collision *** observed spectral bending feature suggests an exponential cutoff at~400 TeV or a power-law break at~200 TeV in the CR proton spectrum,most likely providing the first evidence of SNRs serving as CR accelerators approaching the PeV ***,two young star clusters within W51B could also be theoretically viable to produce the most energeticγrays observed by *** findings strongly support the presence of extreme CR accelerators within the W51 complex and provide new insights into the origin of Galactic CRs.

关键词： UHE c-ray Cosmic rays SNR W51C Star clusters

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A Critical Review of the Evidence for M32 being a Compact Dwarf Satellite of M31 rather than a More Distant Normal Galaxy

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chinese Journal of Astronomy and Astrophysics 2008年第4期8卷 369-384页

作者： C. Ke-shih Young Malcolm J. Currie Robert J. Dickens A-li luo Tong-Jie Zhang national astronomical observatories Chinese Academy of Sciences Beijing 100012 China Shanghai astronomical Observatory Chinese Academy of Sciences Shanghai 200030 China Department of Physics University of Hong Kong Hong Kong China School of Physics University of New South Wales Sydney 2052 Australia Rutherford Appleton Laboratory Chilton Didcot Oxfordshire OX 11 0QX Great Britain Department of Astronomy Beijing Normal University Beijing 100875 China

Since Baade＇s photographic study of M32 in the mid 1940s, it has been accepted as an established fact that M32 is a compact dwarf satellite of M31. The purpose of this paper is to report on the findings of our investigation into the nature of the existing evidence. We find that the case for M32 being a satellite of M31 rests upon Hubble Space Telescope （HST） based stellar population studies which have resolved red-giant branch （RGB） and red clump stars in M32 as well as other nearby galaxies. Taken in isolation, this recent evidence could be considered to be conclusive in favour of the existing view. However, the conventional scenario does not explain M32＇s anomalously high central velocity dispersion for a dwarf galaxy （several times that of either NGC 147, NGC 185 or NGC 205） or existing planetary nebula observations （which suggest that M32 is more than twice as distant as M31） and also requires an elaborate physical explanation for M32＇s inferred compactness. Conversely, we find that the case for M32 being a normal galaxy, of the order of three times as distant as M31, is supported by：（1） a central velocity dispersion typical of intermediate galaxies, （2） the published planetary nebula observations, and （3） known scaling relationships for normal early-type galaxies. However, this novel scenario cannot account for the high apparent luminosities of the RGB stars resolved in the M32 direction by HST observations. We are therefore left with two apparently irreconcilable scenarios, only one of which can be correct, but both of which suffer from potentially fatal evidence to the *** suggests that current understanding of some relevant fields is still very far from adequate.

关键词： galaxies:individual M32 - galaxies distances and redshifts - galaxies dwarf- galaxies elliptical and lenticular, cD - galaxies fundamental parameters

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Overview of the LAMOST survey in the first decade

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The Innovation 2022年第2期3卷 49-64页

作者： Hongliang Yan Haining li Song Wang Weikai Zong Haibo Yuan Maosheng Xiang Yang Huang Jiwei Xie Subo Dong Hailong Yuan Shaolan Bi Yaoquan Chu Xiangqun Cui licai Deng Jianning Fu Zhanwen Han Jinliang Hou Guoping li Chao liu Jifeng liu Xiaowei liu Ali luo Jianrong Shi Xuebing Wu Haotong Zhang Gang zhao yongheng zhao CAS Key Laboratory of Optical Astronomy National Astronomical ObservatoriesBeijing 100101China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China Department of Astronomy Beijing Normal UniversityBeijing 100875China Max-Planck Institute for Astronomy Königstuhl69117HeidelbergGermany South-Western Institute for Astronomy Research Yunnan UniversityKunming 650500China School of Astronomy and Space Science Nanjing UniversityNanjing 210093China Key Laboratory of Modern Astronomy and Astrophysics Ministry of EducationNanjing UniversityNanjing 210093China Kavli Institute for Astronomy and Astrophysics Peking UniversityBeijing 100871China University of Science and Technology of China Hefei 230026China national astronomical observatories/Nanjing Institute of astronomical Optics&Technology Chinese Academy of SciencesNanjing 210042China CAS Key Laboratory of astronomical Optics&Technology Nanjing Institute of Astronomical Optics&TechnologyNanjing 210042China Yunnan observatories Chinese Academy of SciencesKunming 650011China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Key Laboratory of Space Astronomy and Technology National Astronomical ObservatoriesCASBeijing 100101China WHU-NAOC Joint Center for Astronomy Wuhan UniversityWuhan 430072China Department of Astronomy School of PhysicsPeking UniversityBeijing 100871China

The Large Sky Area Multi-Object Fiber Spectroscopic Telescope(LAMOST),also known as the Guoshoujing Telescope,is a major national scientific facility for astronomical research located in Xinglong,*** with a pilot survey in 2011,LAMOST has been surveying the night sky for more than 10 *** LAMOST survey covers various objects in the Universe,from normal stars to peculiar ones.

关键词： China survey surveying

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A method of measuring the [α/Fe] ratios from the spectra of the LAMOST survey

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Research in Astronomy and Astrophysics 2016年第7期16卷 83-96页

作者： Ji li Chen Han Mao-Sheng Xiang Jian-Rong Shi Jing-Kun zhao Xiao-Wei liu Hua-Wei Zhang Hai-Bo Yuan Xuan Ci Xiao-Feng Zhang Yue-Xiang Wang Yang Huang yong Zhang yong-Hui Hou Yue-Fei Wang Zi-Huang Cao Department of Space Science and Astronomy Hebei Normal University Shijiazhuang 050024 China Department of Astronomy Peking University Beijing 100871 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing 100012 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing 100871 China Department of Astronomy Beijing Normal University Beijing 100875 China Nanjing Institute of astronomical Optics & Technology National Astronomical Observatories Chinese Academy of Sciences Nanjing 210042 China

The [α/Fe] ratios in stars are good tracers to probe the formation history of stellar populations and the chemical evolution of the Galaxy. The spectroscopic survey of LAMOST provides a good opportunity to determine [α/Fe] of millions of stars in the Galaxy. We present a method of measuring the [α/Fe]ratios from LAMOST spectra using the template-matching technique of the LSP3 pipeline. We use three test samples of stars selected from the ELODIE and MILES libraries, as well as the LEGUE survey to validate our method. Based on the test results, we conclude that our method is valid for measuring [α/Fe]from low-resolution spectra acquired by the LAMOST survey. Within the range of the stellar parameters Teff= [5000, 7500] K, log g = [1.0, 5.0] dex and [Fe/H]= [onsistent with values derived from high-resolution spectra,-1.5, ＋0.5] dex, our [α/Fe] measurements are c and the accuracy of our [α/Fe] measurements from LAMOST spectra is better than 0.1 dex with spectral signal-to-noise higher than 20.

关键词： Galaxy evolution stars abundances stars fundamental parameters techniques spectroscopy surveys methods data analysis

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The first data release(DR1) of the LAMOST regular survey

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Research in Astronomy and Astrophysics 2015年第8期15卷 1095-1124页

作者： A-li luo yong-heng zhao Gang zhao li-Cai Deng Xiao-Wei liu Yi-Peng Jing Gang Wang Hao-Tong Zhang Jian-Rong Shi Xiang-Qun Cui Yao-Quan Chu Guo-Ping li Zhong-Rui Bai Yue Wu Yan Cai Shu-Yun Cao Zi-Huang Cao Jeffrey L.Carlin Hai-Yuan Chen Jian-Jun Chen Kun-Xin Chen li Chen Xue-Lei Chen Xiao-Yan Chen Ying Chen Norbert Christlieb Jia-Ru Chu Chen-Zhou Cui Yi-Qiao Dong Bing Du Dong-Wei Fan Lei Feng Jian-Ning Fu Peng Gao Xue-Fei Gong Bo-Zhong Gu Yan-Xin Guo Zhan-Wen Han Bo-liang He Jin-liang Hou yong-Hui Hou Wen Hou Hong-Zhuan Hu Ning-Sheng Hu Zhong-Wen Hu Zhi-Ying Huo Lei Jia Fang-Hua Jiang Xiang Jiang Zhi-Bo Jiang Ge Jin Xiao Kong Xu Kong Ya-Juan Lei Ai-Hua li Chang-Hua li Guang-Wei li Hai-Ning li Jian li Qi li Shuang li Sha-Sha li Xin-Nan li Yan li Yin-Bi li Ye-Ping li Yuan liang Chien-Cheng lin Chao liu Gen-Rong liu Guan-Qun liu Zhi-Gang liu Wen-Zhi Lu Yu luo Yin-Dun Mao Heidi Newberg Ji-Jun Ni zhao-Xiang Qi yong-Jun Qi Shi-Yin Shen Huo-Ming Shi Jing Song Yi-Han Song Ding-Qiang Su Hong-Jun Su Zheng-Hong Tang Qing-Sheng Tao Yuan Tian Dan Wang Da-Qi Wang Feng-Fei Wang Guo-Min Wang Hai Wang Hong-Chi Wang Jian Wang Jia-Ning Wang Jian-ling Wang Jian-Ping Wang Jun-Xian Wang Lei Wang Meng-Xin Wang Shou-Guan Wang Shu-Qing Wang Xia Wang Ya-Nan Wang You Wang Yue-Fei Wang You-Fen Wang Peng Wei Ming-Zhi Wei Hong Wu Ke-Fei Wu Xue-Bing Wu Yu-Zhong Wu Xiao-Zheng Xing ling-Zhe Xu Xin-Qi Xu Yan Xu Tai-Sheng Yan De-Hua Yang Hai-Feng Yang Hui-Qin Yang Ming Yang Zheng-Qiu Yao yong Yu Hui Yuan Hai-Bo Yuan Hai-Long Yuan Wei-Min Yuan Chao Zhai En-Peng Zhang Hua-Wei Zhang Jian-Nan Zhang li-Pin Zhang Wei Zhang yong Zhang Yan-Xia Zhang Zheng-Chao Zhang Ming zhao Fang Zhou Xu Zhou Jie Zhu yong-Tian Zhu Si-Cheng Zou Fang Zuo national astronomical observatories Chinese Academy of Sciences Department of Astronomy Peking University Shanghai astronomical Observatory Chinese Academy of Sciences Nanjing Institute of astronomical Optics & Technology National Astronomical ObservatoriesChinese Academy of Sciences University of Science and Technology of China Department of Physics Applied Physics and AstronomyRensselaer Polytechnic InstituteTroyNY 12180USA Department of Physics and Astronomy Earlham CollegeRichmondIN 47374USA Universitt Heidelberg Zentrum für AstronomieLandessternwarteKnigstuhl 1269117 HeidelbergGermany Department of Astronomy Beijing Normal University Yunnan observatories Chinese Academy of Sciences Purple Mountain Observatory Chinese Academy of Sciences

The Large sky Area Multi-Object Fiber Spectroscopic Telescope（LAMOST） general survey is a spectroscopic survey that will eventually cover approximately half of the celestial sphere and collect 10 million spectra of stars, galaxies and QSOs. Objects in both the pilot survey and the first year regular survey are included in the LAMOST DR1. The pilot survey started in October 2011 and ended in June 2012, and the data have been released to the public as the LAMOST Pilot Data Release in August 2012. The regular survey started in September 2012, and completed its first year of operation in June 2013. The LAMOST DR1 includes a total of 1202 plates containing 2 955 336 spectra, of which 1 790 879 spectra have observed signalto-noise ratio（SNR） ≥ 10. All data with SNR ≥ 2 are formally released as LAMOST DR1 under the LAMOST data policy. This data release contains a total of 2 204 696 spectra, of which 1 944 329 are stellar spectra, 12 082 are galaxy spectra and 5017 are quasars. The DR1 not only includes spectra, but also three stellar catalogs with measured parameters： late A,FGK-type stars with high quality spectra（1 061 918 entries）, A-type stars（100 073 entries）, and M-type stars（121 522 entries）. This paper introduces the survey design, the observational and instrumental limitations, data reduction and analysis, and some caveats. A description of the FITS structure of spectral files and parameter catalogs is also provided.

关键词： techniques: spectroscopic survey—data release—catalog

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Newly Discovered Herbig-Haro Objects near Haro 4-255

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chinese Physics Letters 2000年第4期17卷 304-306页

作者： WANG Min zhao Bing YANG Ji DENG li-Cai CHEN Jian-Sheng Purple Mountain Observatory national astronomical observatories Chinese Academy of SciencesNanjing 210008 beijing astronomical Observatory National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100012 beijing Astrophysics Center Beijing 100871

We have performed CCD(charge coupled device)imaging toward the region near Haro 4-255 with a narrow band[SⅡ]filter and an intermediate band[BATC10]filter(BATC:the“beijing-Arizona-Taiwan-Connecticut”multi-color sky survey project)and have discovered two Herbig-Haro(HH)objects,HH469 and *** are identified to be driven by the Haro 4-255(far-infrared)source and the T Tauri star Haro 4-255,respectively.

关键词： Connect filter narrow

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A Photometric Study of the Near Contact Binary UU Lyncis

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chinese Journal of Astronomy and Astrophysics 2007年第2期7卷 251-257页

作者： li-Ying Zhu Sheng-Bang Qian 1,2 Soonthomthum Boonrucksar Jia-JiaHe Jin-zhao Yuan national astronomical observatories / Yunnan Observatory Chinese Academy of Sciences Kunming650011 United Laboratory of Optical Astronomy Chinese Academy of Sciences （ULOAC）. 100012 Beijing Graduate School of chinese academy of sciences ＂ Beijing 100049 Department of Physics Faculty of Science Chiang Mai University Chiang Mai 50200 Thailand

The near-contact binary UU Lyn with an F3V-type primary was observed in 2005 and 2006. With the latest version of the Wilson-Devinney code, the photometric elements were computed. The results reveal that UU Lyn is a marginal contact system with a large temperature difference of about 1900 K between the primary and secondary components. All available eclipse times, including new ones, were used in the analysis. The results show that the orbital period of this system undergoes a continuous decrease at a rate of dP/dt = -1.84 × 10^-8 d yr^-1. With the period decrease, UU Lyn may evolve from the present shortperiod marginal contact system into a contact system with true thermal contact. This target might just be undergoing the cycles predicted by the theory of thermal relaxation oscillations （TRO）. It is an interesting example resembling BL And, GW Tau, ZZ Aur, KQ Gem, CN And and AD Cnc, that lie in the key evolutionary stage.

关键词： techniques photometric- binaries eclipsing - stars individual UU Lyncis

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