检索结果-内蒙古大学图书馆

arXiv 2018年

作者： Yan, Dahai Zhou, Jianeng Zhang, Pengfei Zhu, Qianqian Wang, Jiancheng Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatory Chinese Academy of Sciences Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing210008 China Key Laboratory of Astroparticle Physics of Yunnan Province Yunnan University Kunming650091 China Department of General Studies Nanchang Institute of Science & Technology Nanchang330108 China

The mechanism for producing gamma-ray quasi-periodic oscillation (QPO) in blazar is unknown. One possibility is the geometric model, in which without the need for intrinsic quasi-periodic variation, the relativistic Doppler factor changes periodically, resulting in observed gamma-ray QPO. We propose a method to test this geometric model. We analyze the Fermi-LAT data of PG 1553+113 spanning from 2008 August until 2018 February. According to 29 four-month average spectral energy distributions (SEDs) in the energy range of 0.1-300 GeV, we split the Fermi-LAT energy range into three bands: 0.1-1 GeV, 1-10 GeV, and 10-300 GeV. The spectrum in each energy range can be successfully fitted by a power-law. The light curves and photon indices in the three energy ranges are obtained. Then, light curves in three narrow energy ranges, i.e., 0.2-0.5 GeV, 2-5 GeV and 20- 40 GeV, are constructed, and the relative variability amplitudes in the three narrow energy ranges are calculated. A discrete- correlation analysis is performed for the light curves. Our results indicate that (i) the light curves in the different energy ranges follow the same pattern showed in the light curve above 0.1 GeV;(ii) the three groups of photon indices in the energy ranges of 0.1-1 GeV, 1-10 GeV, and 10-300 GeV keep nearly constant;(iii) the ratio between relative variability amplitudes in different narrow energy ranges are equal (within their errors) to the prediction by the Doppler e ect. Our results support the scenario of the relativistic boost producing the gamma-ray QPO for PG 1553+113. Copyright © 2018, The Authors. All rights reserved.

关键词： Germanium alloys

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TESS Asteroseismic Analysis of HD76920: The Giant Star Hosting An Extremely Eccentric Exoplanet

arXiv

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arXiv 2023年

作者： Jiang, Chen Wu, Tao Feinstein, Adina D. Stassun, Keivan G. Bedding, Timothy R. Veras, Dimitri Corsaro, Enrico Buzasi, Derek L. Stello, Dennis Li, Yaguang Mathur, Savita García, Rafael A. Breton, Sylvain N. Lundkvist, Mia S. Mikolajczyk, Przemyslaw J. Gehan, Charlotte Campante, Tiago L. Bossini, Diego Kane, Stephen R. Ong, Jia Mian Joel Yildiz, Mutlu Kayhan, Cenk Orhan, Zeynep Çelik Örtel, Sibel Zhang, Xinyi Cunha, Margarida S. De Moura, Bruno Lustosa Yu, Jie Huber, Daniel Ou, Jian-Wen Wittenmyer, Robert A. Gizon, Laurent Chaplin, William J. Max-Planck-Institut für Sonnensystemforschung Justus-von-Liebig-Weg 3 Göttingen37077 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 University of Chinese Academy of Sciences Beijing100049 China Institute of Theoretical Physics Shanxi University Taiyuan030006 China Department of Astronomy and Astrophysics University of Chicago 5640 S. Ellis Ave ChicagoIL60637 United States Department of Physics and Astronomy Vanderbilt University NashvilleTN37235 United States School of Physics University of Sydney NSW2006 Australia Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus C8000 Denmark Centre for Exoplanets and Habitability University of Warwick CoventryCV4 7AL United Kingdom Centre for Space Domain Awareness University of Warwick CoventryCV4 7AL United Kingdom Department of Physics University of Warwick CoventryCV4 7AL United Kingdom Inaf - Osservatorio Astrofisico di Catania via S. Sofia 78 Catania95123 Italy Department of Chemistry & Physics Florida Gulf Coast University 10501 FGCU Boulevard S. Fort MyersFL33965 United States School of Physics University of New South Wales NSW2052 Australia Tenerife La LagunaE-38205 Spain Departamento de Astrofísica Tenerife La LagunaE-38206 Spain Université Paris-Saclay Université Paris Cité Cea Cnrs Aim Gif-sur-Yvette91191 France Département d'Astrophysique/aim CEA/IRFU CNRS/INSU Univ. Paris-Saclay Univ. de Paris Gif-sur-Yvette91191 France Astronomical Observatory University of Warsaw Al. Ujazdowskie 4 Warsaw00-478 Poland Astronomical Institute University of Wroclaw Mikolaja Kopernika 11 Wroclaw51-622 Poland Instituto d

The Transiting Exoplanet Survey Satellite (TESS) mission searches for new exoplanets. The observing strategy of TESS results in high-precision photometry of millions of stars across the sky, allowing for detailed asteroseismic studies of individual systems. In this work, we present a detailed asteroseismic analysis of the giant star HD 76920 hosting a highly eccentric giant planet (e = 0.878) with an orbital period of 415 days, using 5 sectors of TESS light curve that cover around 140 days of data. Solar-like oscillations in HD 76920 are detected around 52 μHz by TESS for the first time. By utilizing asteroseismic modeling that takes classical observational parameters and stellar oscillation frequencies as constraints, we determine improved measurements of the stellar mass (1.22 ± 0.11Mo), radius (8.68 ± 0.34 Ro), and age (5.2 ± 1.4 Gyr). With the updated parameters of the host star, we update the semi-major axis and mass of the planet as a = 1.165 ± 0.035 au and Mpsin i = 3.57 ± 0.22 MJup. With an orbital pericenter of 0.142±0.005 au, we confirm that the planet is currently far away enough from the star to experience negligible tidal decay until being engulfed in the stellar envelope. We also confirm that this event will occur within about 100 Myr, depending on the stellar model used. © 2023, CC BY.

关键词： Satellites

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JWST NIRSpec+MIRI Observations of the nearby Type IIP supernova 2022acko

arXiv

引用

arXiv 2024年

作者： Shahbandeh, M. Ashall, C. Hoeflich, P. Baron, E. Fox, O. Mera, T. DerKacy, J. Stritzinger, M.D. Shappee, B. Law, D. Morrison, J. Pauly, T. Pierel, J. Medler, K. Andrews, J. Baade, D. Bostroem, A. Brown, P. Burns, C. Burrow, A. Cikota, A. Cross, D. Davis, S. de Jaeger, T. Do, A. Dong, Y. Dominguez, I. Galbany, L. Janzen, D. Jencson, J. Hoang, E. Hsiao, E. Karamehmetoglu, E. Khaghani, B. Krisciunas, K. Kumar, S. Lu, J. Lundquist, M. Maund, J. Mazzali, P. Morrell, N. Patat, F. Pearson, J. Pfeffer, C. Phillips, M. Rest, A. Retamal, N. Stangl, S. Shrestha, M. Stevens, C. Suntzeff, N. Telesco, C. Tucker, M. Wang, L. Yang, Y. Cai, Y.-Z. Camacho-Neves, Y. Elias-Rosa, N. Foley, R. Jha, S. Kwok, L. Larison, C. LeBaron, N. Moran, S. Rho, J. Salmaso, I. Schmidt, J. Tinyanont, S. Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218-2410 United States Department of Physics Virginia Tech BlacksburgVA24061 United States Department of Physics Florida State University 77 Chieftan Way TallahasseeFL32306 United States Planetary Science Institute 1700 East Fort Lowell Road Suite 106 TucsonAZ85719-2395 United States Hamburger Sternwarte Gojenbergsweg 112 HamburgD-21029 Germany Dept of Physics & Astronomy University of Oklahoma 440 W. Brooks Rm 100 NormanOK United States Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Institute for Astronomy University of Hawai’i at Manoa 2680 Woodlawn Dr. Hawai’i HI96822 United States Astrophysics Research Institute Liverpool John Moores University United Kingdom Gemini Observatory NSF’s NOIRLab 670 North A‘ohoku Place HiloHI96720-2700 United States Karl-Schwarzschild-Str. 2 Garching b. München85748 Germany Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721-0065 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Texas A&M University Department of Physics and Astronomy College StationTX77843 United States Observatories of the Carnegie Institution for Science 813 Santa Barbara Street PasadenaCA91101 United States Homer L. Dodge Department of Physics and Astronomy University of Oklahoma 440 W. Brooks Rm 100 NormanOK73019-2061 United States Gemini Observatory NSF’s NOIRLab Casilla 603 La Serena Chile Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain Private Astronomer Laboratoire de Physique Nucléaire et de Hautes Énergies Paris75005 France Department of Physics University of California 1 Shields Avenue DavisCA95616-5270 United States Universidad de Granada Granada18071 Spain BarcelonaE-08034 Spain Department of Physics and Engineering Physics University of Saskatchewan 116 Science Place SaskatoonSKS7N 5E

We present JWST spectral and photometric observations of the Type IIP supernova (SN) 2022acko at ∼50 days past explosions. These data are the first JWST spectral observations of a core-collapse SN. We identify ∼ 30 different H i features, other features associated with products produced from the CNO cycle, and s-process elements such as Sc ii, Ba ii. By combining the JWST spectra with ground-based optical and NIR spectra, we construct a full Spectral Energy Distribution from 0.4 to 25 μm and find that the JWST spectra are fully consistent with the simultaneous JWST photometry. The data lack signatures ofCO formation and we estimate a limit on the CO mass of −8M☉. We demonstrate how the CO fundamental band limits can be used to probe underlying physics during the stellar evolution, explosion, and the environment. The observations indicate little mixing between the H envelope and C/O core in the ejecta and show no evidence for dust. The data presented here set a critical baseline for future JWST observations, where possible molecular and dust formation may be seen. © 2024, CC BY.

关键词： Supernovae

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Expanded solutions of force-free electrodynamics on general Kerr black holes

arXiv

引用

arXiv 2017年

作者： Li, Huiquan Wang, Jiancheng Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China

In this work, expanded solutions of force-free magnetospheres on general Kerr black holes are derived through a radial distance expansion method. From the regular conditions both at the horizon and at spatial infinity, two previously known asymptotical solutions (one of them is actually an exact solution) are identified as the only solutions that satisfy the same conditions at the two boundaries. Taking them as initial conditions at the boundaries, expanded solutions up to the first few orders are derived by solving the stream equation order by order. It is shown that our extension of the exact solution can (partially) cure the problems of the solution: it leads to magnetic domination and a mostly timelike current for restricted parameters. Copyright © 2017, The Authors. All rights reserved.

关键词： Magnetosphere

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MULTI-WAVELENGTH OBSERVATIONS OF A NEW REDBACK MILLISECOND PULSAR CANDIDATE: 3FGL J0954.8−3948

arXiv

引用

arXiv 2018年

作者： Li, Kwan-Lok Hou, Xian Strader, Jay Takata, Jumpei Kong, Albert K.H. Chomiuk, Laura Swihart, Samuel J. Hui, Chung Yue Cheng, K.S. Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China School of physics Huazhong University of Science and Technology Wuhan430074 China Institute of Astronomy National Tsing Hua University Hsinchu30013 Taiwan Department of Astronomy and Space Science Chungnam National University Daejeon34134 Korea Republic of Department of Physics University of Hong Kong Pokfulam Road Hong Kong

We present a multi-wavelength study of the unassociated Fermi-LAT source, 3FGL J0954.8−3948, which is likely the γ-ray counterpart of a 9.3-hour binary in the field. With more than 9 years of Pass 8 LAT data, we updated the γ-ray spectral properties and the LAT localization of the γ-ray source. While the binary lies outside the cataloged 95% error ellipse, the optimized LAT ellipse is 0.1 degrees closer and encloses the binary. The system is likely spectrally hard in X-rays (photon index ΓX = 1.4−+11..20) with orbital modulations detected in optical, UV, and possibly X-rays. A steep spectrum radio counterpart (spectral index α ≈ −1.6) is also found in the TIFR GMRT Sky Survey (TGSS), implying that it is a pulsar system. We obtained a series of SOAR and Gemini spectroscopic observations in 2017/2018, which show a low-mass secondary orbiting in a close circular orbit with K2 = 272 ± 4 km s−1 under strong irradiation by the primary compact object. All the observations as well as the modelling of the X/γ-ray high-energy emission suggest that 3FGL J0954.8−3948 is a redback millisecond pulsar in a rotation-powered state. Copyright © 2018, The Authors. All rights reserved.

关键词： Pulsars

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Observations of a fast-expanding and uv-bright type ia supernova SN 2013gs

arXiv

引用

arXiv 2019年

作者： Zhang, Tianmeng Wang, Xiaofeng Zhao, Xulin Xu, Dong Reguitti, Andrea Zhang, Jujia Pastorello, Andrea Tomasella, Lina Ochner, Paolo Tartaglia, Leonardo Benetti, Stefano Turatto, Massimo Harutyunyan, Avet Elias-Rosa, Nancy Huang, Fang Zhang, Kaicheng Chen, Juncheng Jiang, Zhaoji Ma, Jun Nie, Jundan Peng, Xiyan Zhou, Xu Zhou, Zhimin Zou, Hu Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China School of Astronomy and Space Science University of Chinese Academy of Sciences Tsinghua University Beijing100084 China School of Science Tianjin University of Technology Tianjin300384 China National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China Dipartimento di Fisica e Astronomia G. Galilei Universita’ di Padova Vicolo dell’Osservaotio 3 Padova35122 Italy Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China INAF-Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 Padova35122 Italy Department of Astronomy Stockholm University StockholmSE 10691 Sweden INAF-Fundacion Galileo Galilei Rambla Jose Ana Fernandez Perez 7 Brena BajaE-38712 Spain Department of Astronomy School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China

In this paper, we present extensive optical and ultraviolet (UV) observations of the type Ia supernova (SN Ia) 2013gs discovered during the Tsinghua-NAOC Transient Survey. The photometric observations in the optical show that the light curves of SN 2013gs is similar to that of normal SNe Ia, with an absolute peak magnitude of MB = −19.25 ± 0.15 mag and a post-maximum decline rate ∆m15(B) = 1.00 ± 0.05 mag. Gehrels Swift UVOT observations indicate that SN 2013gs shows unusually strong UV emission (especially in the uvw1 band) at around the maximum light (Muvw1 ∼ −18.9 mag). The SN is characterized by relatively weak Fe ii iii absorptions at ∼ 5000Å in the early spectra and a larger expansion velocity (vSi ∼ 13,000 km s−1 around the maximum light) than the normal-velocity SNe Ia. We discuss the relation between the uvw1−v color and some observables, including Si ii velocity, line strength of Si ii λ6355, Fe ii/iii lines and ∆m15(B). Compared to other fast-expanding SNe Ia, SN 2013gs exhibits Si and Fe absorption lines with similar strength and bluer uvw1 − v color. We briefly discussed the origin of the observed UV dispersion of SNe Ia. Copyright © 2019, The Authors. All rights reserved.

关键词： Supernovae

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He-accreting carbon-oxygen white dwarfs and type Ia supernovae

arXiv

引用

arXiv 2017年

作者： Wang, Bo Podsiadlowski, Philipp Han, Zhanwen Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories CAS Kunming650216 China Center for Astronomical Mega-Science CAS Beijing100012 China Department of Astronomy Oxford University OxfordOX1 3RH United Kingdom

He accretion onto carbon-oxygen white dwarfs (COWDs) plays a fundamental role when studying the formation of type Ia supernovae (SNe Ia). Employing the MESA stellar evolution code, we calculated the long-term evolution of He-accreting CO WDs. Previous studies usually supposed that a WD can grow in mass to the Chandrasekhar limit in the stable He burning region and finally produce a SN Ia. However, in this study we find that off-centre carbon ignition occurs in the stable He burning region if the accretion rate is above a critical value (∼2.05 × 10-6Moyr-1), resulting in accretion-induced collapse rather than a SN Ia. If the accretion rate is below the critical value, explosive carbon ignition will eventually happen in the centre producing a SN Ia. Taking into account the possibility of off-centre carbon ignition, we have re-determined the initial parameter space that produces SNe Ia in the He star donor channel, one of the promising channels to produce SNe Ia in young populations. Since this parameter space is smaller than was found in the previous study ofWang et al. (2009), the SN Ia rates are also correspondingly smaller. We also determined the chemical abundance profile of the He-accreting WDs at the moment of explosive carbon ignition, which can be used as initial input for SN Ia explosion models. Copyright © 2017, The Authors. All rights reserved.

关键词： White dwarfs

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ALMA [N ii ] 205 µm Imaging Spectroscopy of the Lensed Submillimeter galaxy ID 141 at redshift 4.24

arXiv

引用

arXiv 2020年

作者： Cheng, Cheng Cao, Xiaoyue Lu, Nanyao Li, Ran Yang, Chentao Rigopoulou, Dimitra Charmandaris, Vassilis Gao, Yu Xu, Cong Kevin van der Werf, Paul Santos, Tanio Diaz Privon, George C. Zhao, Yinghe Cao, Tianwen Dai, Y. Sophia Huang, Jia-Sheng Sanders, David Wang, Chunxiang Wang, Zhong Zhu, Lei National Astronomical Observatories Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100101 China China-Chile Joint Center for Astronomy Camino El Observatorio 1515 Las Condes Santiago Chile Instituto de Física y Astronomía Universidad de Valparaíso Avda. Gran Bretaña 1111 Valparaíso Chile 20A Datun Road Chaoyang District Beijing100012 China School of Astronomy and Space Science University of Chinese Academy of Science 19 A Yuquan Rd Shijingshan District Beijing100049 China European Southern Observatory Alonso de CÃşrdova 3107 Casilla 19001 Vitacura Santiago Chile Astrophysics Department University of Oxford OxfordOX1 3RH United Kingdom Department of Physics University of Crete HeraklionGR-71003 Greece Institute of Astrophysics FORTH HeraklionGR-71110 Greece Department of Astronomy Xiamen University XiamenFujian361005 China Nanjing210033 China Leiden Observatory Leiden University P.O. Box 9513 Leiden2300 RA Netherlands Nucleo de Astronomia de la Facultad de Ingenieria Universidad Diego Portales Av. Ejercito Libertador 441 Santiago Chile Department of Astronomy University of Florida 211 Bryant Space Sciences Center GainesvilleFL32611 United States Yunnan Observatories Chinese Academy of Sciences Kun-ming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Center for Astronomical Mega-Science CAS 20A Datun Road Chaoyang District Beijing100012 China Institute for Astronomy University of Hawaii 2680 Woodlawn Drive HonoluluHI96822 United States

We present the Atacama Large Millimeter/submillimeter Array (ALMA) observation of the Submillimeter galaxy (SMG) ID 141 at z=4.24 in the [N ii ] 205 µm line (hereafter [N ii ]) and the underlying continuum at (rest-frame) 197.6 µm. Benefiting from lensing magnification by a galaxy pair at z=0.595, ID 141 is one of the brightest z > 4 SMGs. At the angular resolutions of ∼ 1.2″ to 1.5″ (1″∼6.9 kpc), our observation clearly separates, and moderately resolves the two lensed images in both continuum and line emission at S/N > 5 . Our continuum-based lensing model implies an averaged amplification factor of ∼ 5.8 and reveals that the de-lensed continuum image has the Sérsic index'0.95 and the Sérsic radius of ∼0.1800 (∼1.24 kpc). Furthermore, the reconstructed [N ii ] velocity field in the source plane is dominated by a rotation component with a maximum velocity of ∼300 km/s at large radii, indicating a dark matter halo mass of ∼1012M. This, together with the reconstructed velocity dispersion field being smooth and modest in value ( Copyright © 2020, The Authors. All rights reserved.

关键词： Galaxies

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A uniformly selected sample of low-mass black holes in seyfert 1 galaxies. II. the sdss dr7 sample

arXiv

引用

arXiv 2018年

作者： Liu, He-Yang Yuan, Weimin Dong, Xiao-Bo Zhou, Hongyan Liu, Wen-Juan Key Laboratory of Space Astronomy and Technology National Astronomical Observatories Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China School of Astronomy and Space Sciences University of Chinese Academy of Sciences 19A Yuquan Road Beijing100049 China Yunnan Observatories Chinese Academy of Sciences Kunming Yunnan650011 China Key Laboratory for Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming Yunnan650011 China Polar Research Institute of China 451 Jinqiao Road Shanghai200136 China University of Sciences and Technology of China Chinese Academy of Sciences Hefei Anhui230026 China

A new sample of 204 low-mass black holes (LMBHs) in active galactic nuclei (AGNs) is presented with black hole masses in the range of (1-20) × 105 Mo. The AGNs are selected from a systematic search among galaxies in the seventh Data Release (DR 7) of the Sloan Digital Sky Survey (SDSS), by careful analyses of their optical spectra and precise measurement of spectral parameters. Combining them with our previous sample selected from the SDSS DR 4 makes it the largest LMBH sample so far, totaling over 500 objects. Some of the statistical properties of the combined LMBH AGN sample are briefly discussed, in the context of exploring the low-mass end of the AGN population. Their X-ray luminosities follow the extension of the previously known correlation with the [O III] luminosity. The effective optical-to-X-ray spectral indices αOX, albeit with a large scatter, are broadly consistent with the extension of the relation with the near-UV luminosity L2500Å. Interestingly, a correlation of αOX with black hole mass is also found in the sense that αOX is statistically flatter (stronger X-ray relative to optical) for lower black hole mass. Only 26 objects, mostly radio loud, were detected in radio at 20 cm in the FIRST survey, giving a radio loud fraction of 4%. The host galaxies of LMBHs have stellar masses in the range of 108.8-1012.4 Mo and optical colors typical of Sbc spirals. They are dominated by young stellar populations which seem to have undergone a continuous star formation history. Copyright © 2018, The Authors. All rights reserved.

关键词： Stars

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Photometric Investigation of the Contact Binary GU Ori with High Metallicity

arXiv

引用

arXiv 2018年

作者： Zhou, X. Qian, S.-B. Soonthornthum, B. Poshyachinda, S. Zhu, L.-Y. Liu, N.-P. Sarotsakulchai, T. Fang, X.-H. P.O. Box 110 Kunming650216 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P. O. Box 110 Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang Dis-trict Beijing100012 China University of the Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China National Astronomical Research Institute of Thailand 260 Moo 4 T. Donkaew A. MaerimChiangmai50180 Thailand

GU Ori was observed with the 1m telescope at Yunnan Observatories in 2005. To determine its physical properties, the Wilson-Devinney program is used. The results reveal that GU Ori is a W-subtype shallow contact binary with a more massive but cooler star 2. The mass of its two component stars are estimated to be M1 = 0.45M☉, M2 = 1.05M☉. The O’Connell effect was reported to be negative on the light curves observed in 2005. However, it changed to a positive one on the light curves observed from 2011 to 2012. The mean surface temperatures of star 2 (T2) determined by the two sets of light curves were different, which may result from stellar activities. The O - C diagram shows that the period of GU Ori is decreasing at a rate of dP/dt = −6.24 × 10−8day · year−1, which may be caused by mass transfer from star 2 to star 1 with a rate of dMdt2 = −2.98 × 10−8M☉/year. GU Ori is a contact binary with quite high metallicity. Copyright © 2018, The Authors. All rights reserved.

关键词： Photometry

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