检索结果-内蒙古大学图书馆

arXiv 2023年

作者： Wang, Pei Li, Jian Ji, Long Hou, Xian Gügercinoğlu, Erbil Li, Di Torres, Diego F. Chen, Yutong Niu, Jiarui Zhu, Wei-Wei Zhang, Bing Liang, En-Wei Zhang, Li Ge, Mingyu Dai, Zigao Lin, Lin Han, Jinlin Feng, Yi Niu, Chenhui Zhang, Yongkun Zhou, Dejiang Xu, Heng Zhang, Chunfeng Jiang, Jinchen Miao, Chenchen Yuan, Mao Wang, Weiyang Zhou, Dengke Fang, Jianhua Yue, Youling Wu, Yunsheng Wang, Yabiao Wang, Chengjie Gan, Zhenye Li, Yuxi Sun, Zhongyi Chi, Mingmin Zhang, Junshuo Cao, Jinhuang Lu, Wanjin Wang, Yidan National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Institute for Frontiers in Astronomy and Astrophysics Beijing Normal University Beijing102206 China CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei230026 China School of Astronomy and Space Science University of Science and Technology of China Hefei230026 China School of Physics and Astronomy Sun Yat-Sen University Zhuhai519082 China Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Istanbul University Faculty of Science Department of Astronomy and Space Sciences Beyazıt Istanbul34119 Turkey Department of Astronomy Tsinghua University Beijing100084 China Campus UAB Carrer de Can Magrans Barcelona08193 Spain Castelldefels Barcelona08860 Spain BarcelonaE-08010 Spain University of Chinese Academy of Sciences Beijing100049 China Department of Physics and Astronomy University of Nevada Las Vegas Las VegasNV89154 United States Guangxi Key Laboratory for Relativistic Astrophysics School of Physical Science and Technology Guangxi University Nanning530004 China Department of Astronomy Key Laboratory of Astroparticle Physics of Yunnan Province Yunnan University Kunming650091 China Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China Zhejiang Lab Zhejiang Hangzhou311121 China Institute of Astrophysics Central China Normal University Wuhan430079 China Department of Astronomy Peking University Beijing100871 China National Space Science Center Chinese Academy of Sciences Beijing101400 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Tencent Youtu Lab Shanghai201103 China Fudan University Shanghai200438 China

Magnetars are neutron stars with extremely strong magnetic fields, frequently powering high-energy activity in X-rays. Pulsed radio emission following some X-ray outbursts have been detected (Camilo et al. 2006, 2007), albeit its physical origin is unclear. It has long been speculated that the origin of magnetars' radio signals is different from those from canonical pulsars, although convincing evidence is still lacking. Five months after magnetar SGR 1935+2154's X-ray outburst and its associated Fast Radio Burst (FRB) 20200428, a radio pulsar phase was discovered. Here we report the discovery of X-ray spectral hardening associated with the emergence of periodic radio pulsations from SGR 1935+2154 and a detailed analysis of the properties of the radio pulses. The observations suggest that radio emission originates from the outer magnetosphere of the magnetar, and the surface heating due to the bombardment of inward-going particles from the radio emission region is responsible for the observed X-ray spectral hardening. Copyright © 2023, The Authors. All rights reserved.

关键词： Radiation hardening

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Spot model for identifications of periods in asynchronous polars

arXiv

引用

arXiv 2020年

作者： Wang, Qishan Qian, Shengbang Han, Zhongtao Fang, Xiaohui Zang, Lei Liu, Wei 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 University of Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Science 20A Datun Road Chaoyang Distric Beijing100012 China Guizhou Provincial Key Laboratory of Radio Data Processing School of Physics and Electronic Sciences Guizhou Normal University Guiyang550001 China

We improved the discless accretion models of Wynn & King, considering the effects of the changing aspect due to the white dwarf spin and the variable feeding intensity caused by the asynchronism, and set up a more general spot model which is not sensitive to the different forms of these effects and can be applied for the period analysis of the optical and X-ray light curve. The spot model can produce the power spectra compatible with the observations, and its simulations limit the ratio Pspin/Porb Copyright © 2020, The Authors. All rights reserved.

关键词： White dwarfs

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Spectroscopic monitoring of blazar S5 0716+714: brightness-dependent Spectral Behavior

arXiv

引用

arXiv 2020年

作者： Feng, Hai-Cheng Yang, Sen Yang, Zi-Xu Liu, H.T. Bai, J.M. Li, Sha-Sha Zhao, X.H. Zhang, Jin Li, Y.B. Xiao, M. Xin, Y.X. Xing, L.F. Lu, K.X. Xu, L. Wang, J.G. Wang, C.J. Zhang, X.L. Zhang, J.J. Lun, B.L. He, S.S. Yunnan Observatories Chinese Academy of Sciences KunmingYunnan650011 China University of Chinese Academy of Sciences Beijing100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences KunmingYunnan650011 China Key Laboratory for Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences 19B Yuquan Road Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory of Space Astronomy and Technology National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China

In this paper, we report the new results of spectroscopic observations of γ-ray blazar S5 0716+714 from 2019 September to 2020 March with the 2.4 m optical telescope at Lijiang Observatory of Yunnan Observatories. The median cadence of observations is ∼ 1 day. During the second observation period (Epoch2), the observational data reveal an extremely bright state and a bluer-when-brighter (BWB) chromatism. The BWB trend of Epoch2 differs significantly from that of the first observation period (Epoch1). A significantly brightness-dependent BWB chromatism emerges in the total data of Epoch1 and Epoch2. The BWB trend becomes weaker towards the brighter states, and likely becomes saturated at the highest state. Based on a log-parabolic function, a power-law of synchrotron peak flux and frequency νp, and a power-law of the curvature of synchrotron spectrum and its νp, simulation well reproduces the brightness-dependent BWB trend of S5 0716+714. The BWB trend is seemingly controlled by the shift of νp with respect to the observational window, and effectively may be dominated by the variations of electron average energy and magnetic field in emitting region. Copyright © 2020, The Authors. All rights reserved.

关键词： Luminance

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The contact binary V344 Lacertae: Is it a triple system?

arXiv

引用

arXiv 2020年

作者： Liang, Liu Shengbang, Qian Kai, Li Jiajia, He Linjia, Li Ergang, Zhao Xuzhi, Li 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 Yuquan Road 19# Sijingshang Block Beijing100049 China Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment Institute of Space Sciences Shandong University Weihai264209 China

The V RI passbands light curves of V344 Lac were presented and analyzed by using the latest version of the W-D code. The observed spectrum reveals that V344 Lac is not an A3 type but would be a later F type star according to the yielded temperature. The results of solution show that V344 Lac is an A-subtype contact binary, with a mediate photometric mass ratio of 0.387 ± 0.003 and a mediate contact factor of 44.6 ± 3.0%. Based on the parallax given by Gaia, the parameters of the components are estimated as: M1 = 1.16 M☉, M2 = 0.45 M☉, R1 = 1.31 R☉, R2 = 0.88 R☉, L1 = 2.512 L☉, L2 = 1.057 L☉. The period investigation indicates that V344 Lac may have an eccentric orbital oscillation, with P3 = 12.4 ± 0.5 yr, A3 = 0.0020 ± 0.0002 d, and e = 0.38 ± 0.16. Analysis shows such oscillation would be caused by a magnetic activity which can be explained by the Applegate mechanism. Meanwhile, according to the value of l3 and the estimated physical parameters of V344 Lac, the mass of the third companion may be 0.79M☉. This third body could be a wide company. Copyright © 2020, The Authors. All rights reserved.

关键词： Parameter estimation

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Effects of Binary Interactions on the Early-type Galaxy Chemical evolution and Gas Cooling Functiontwo

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Chinese Astronomy and Astrophysics 2018年第4期42卷 527-537页

作者： Lang, Wang Yunnan Astronomical Observatories Chinese Academy of Sciences Kunming 650011 China University of Chinese Academy of Sciences Beijing 100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing 100012 China

In the galaxy parameter fitting by means of stellar population synthesis, it is found that compared with the evolutionary population synthesis (EPS) model without binary interactions, the stellar age and metallicity of a galaxy derived from the EPS model with binary interactions are larger. But, we are still unclear how the binary interactions affect the galaxy evolution. For the early-type galaxies with the UV-excess phenomenon, there are two main-stream explanations: recent star formation (RSF) and binary interactions. In this study, we obtain the mass return rate and chemical yield for the stellar populations with and without binary interactions. In combination with the galaxy chemical evolution and photoionization models, we study the effects of binary interactions on the chemical evolution and metallicity evolution for the early-type galaxies with the UV-excess phenomenon under the two formation mechanisms. We find that the inclusion of binary interactions can raise the ejected mass, metallicity, alpha element, and accelerate the gas cooling. These can reasonably explain the conclusions made by the EPS models. Moreover, we find that the gas cooling is more efficient under the UV-excess formation mechanism by the binary interactions rather than the RSF, and the ratio of element abundance is different for the two mechanisms, which can be further used to distinguish these two mechanisms. © 2018

关键词： Abundances—galaxies evolution Galaxies ISM—galaxies

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evolution of Dipolar Mixed-mode Coupling Factor in Red Giant Stars: Impact of Buoyancy Spike

arXiv

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arXiv 2022年

作者： Jiang, Chen Cunha, Margarida Christensen-Dalsgaard, Joergen Zhang, Qiansheng S. Gizon, Laurent Max-Planck-Institut für Sonnensystemforschung Justus-von-Liebig-Weg 3 Göttingen37077 Germany Instituto de Astrofísica e Ciências do Espaço Universidade do Porto CAUP Rua das Estrelas Porto4150-762 Portugal Stellar Astrophysics Centre Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Yunnan Observatories 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 Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China University of Chinese Academy of Sciences Beijing100049 China Institut für Astrophysik Georg-August-Universität Göttingen Friedrich-Hund-Platz 1 Göttingen37077 Germany Center for Space Science NYUAD Institute New York University Abu Dhabi Abu Dhabi United Arab Emirates

Mixed modes observed in red giants allow for investigation of the stellar interior structures. One important feature in these structures is the buoyancy spike caused by the discontinuity of the chemical gradient left behind during the first dredge-up. The buoyancy spike emerges at the base of the convective zone in low-luminosity red giants and later becomes a glitch when the g-mode cavity expands to encompass the spike. Here, we study the impact of the buoyancy spike on the dipolar mixed modes using stellar models with different properties. We find that the applicability of the asymptotic formalisms for the coupling factor, q, varies depending on the location of the evanescent zone, relative to the position of the spike. Significant deviations between the value of q inferred from fitting the oscillation frequencies and either of the formalisms proposed in the literature are found in models with a large frequency separation in the interval 5 to 15 µHz, with evanescent zones located in a transition region which may be thin or thick. However, it is still possible to reconcile q with the predictions from the asymptotic formalisms, by choosing which formalism to use according to the value of q. For stars approaching the luminosity bump, the buoyancy spike becomes a glitch and strongly affects the mode frequencies. Fitting the frequencies without accounting for the glitch leads to unphysical variations in the inferred q, but we show that this is corrected when properly accounting for the glitch in the fitting. Copyright © 2022, The Authors. All rights reserved.

关键词： Buoyancy

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Tianyu: search for the second solar system and explore the dynamic universe

arXiv

引用

arXiv 2024年

作者： Feng, Fabo Rui, Yicheng Du, Zhimao Lin, Qing Zhang, Congcong Zhou, Dan Cui, Kaiming Ogihara, Masahiro Yang, Ming Lin, Jie Cai, Yongzhi Yang, Taozhi Pang, Xiaoying Jian, Mingjie Li, Wenxiong Guo, Hengxiao Shi, Xian Shi, Jianchun Li, Jianyang Guo, Kangrou Yao, Song Chen, Aming Jia, Peng Tan, Xianyu Jenkins, James S. Jiang, Hongxuan Zhang, Mingyuan Li, Kexin Xiao, Guangyao Zheng, Shuyue Xuan, Yifan Zheng, Jie He, Min Jones, Hugh R.A. Song, Cuiying Tsung-Dao Lee Institute Shanghai Jiao Tong University Shengrong Road 520 Shanghai201210 China School of Physics and Astronomy Shanghai Jiao Tong University 800 Dongchuan Road Shanghai200240 China Shanghai200127 China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China College of Surveying and Geo-Informatics Tongji University Shanghai20009 China CAS Key laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei230026 China School of Astronomy and Space Sciences University of Science and Technology of China Hefei230026 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Yunnan Observatories Chinese Academy of Sciences Kunming650216 China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China School of Physics Xi’an Jiaotong University Xi’an710049 China Department of Physics Xi’an Jiaotong-Liverpool University 111 Ren’ai Road Dushu Lake Science and Education Innovation District Suzhou215123 China Shanghai Key Laboratory for Astrophysics Shanghai Normal University 100 Guilin Road Shanghai200234 China Department of Astronomy Stockholm University AlbaNova University Center Roslagstullsbacken 21 Stockholm114 21 Sweden National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China School of Atmospheric Sciences Sun Yat-sen University Zhuhai519082 China College of Electronic Information and Optical Engineering Taiyuan University of Technology Taiyuan030024 China Instituto de Estudios Astrofísicos Facultad de Ingeniería y Ciencias Universidad Diego Portales Av. Ejército 441 Santiago Chile Casilla 36-D Santiago Chile Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment School of Space Science and Physics Institute of Space Sciences Shandong University Shandong Weihai264209 China CAS K

Giant planets like Jupiter and Saturn, play important roles in the formation and habitability of Earth-like planets. The detection of solar system analogs that have multiple cold giant planets is essential for our understanding of planet habitability and planet formation. Although transit surveys such as Kepler and Transiting Exoplanet Survey Satellite (TESS) have discovered thousands of exoplanets, these missions are not sensitive to long period planets due to their limited observation baseline. The Tianyu project, comprising two 1-meter telescopes (Tianyu-I and II), is designed to detect transiting cold giant planets in order to find solar system analogs. Featuring a large field of view and equipped with a high-speed CMOS camera, Tianyu-I will perform a high-precision photometric survey of about 100 million stars, measuring light curves at hour-long cadence. The candidates found by Tianyu-I will be confirmed by Tianyu-II and other surveys and follow-up facilities through multi-band photometry, spectroscopy, and high resolution imaging. Tianyu telescopes will be situated at an elevation about 4000 meters in Lenghu, chosen as the premier observation site in China. With a photometric precision of 0.1% for stars with V © 2024, CC BY.

关键词： Exoplanets

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Searching for multiple populations in star clusters using the China Space Station Telescope

arXiv

引用

arXiv 2022年

作者： Li, Chengyuan Zheng, Zhenya Li, Xiaodong Pang, Xiaoying Tang, Baitian Milone, Antonino P. Wang, Yue Wang, Haifeng Jiang, Dengkai School of Physics and Astronomy Sun Yat-sen University Daxue Road Guangdong Zhuhai519082 China CSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area Zhuhai519082 China CAS Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Shanghai200030 China Division of Optical Astronomical Technologies Shanghai Astronomical Observatory Shanghai200030 China Department of Physics Xi'an Jiaotong-Liverpool University 111 Ren'ai Road Jiangsu Suzhou215123 China Shanghai Key Laboratory for Astrophysics Shanghai Normal University 100 Guilin Road Shanghai200234 China Dipartimento di Fisica e Astronomia 'Galileo Galilei' Universita di Padova Vicolo dell'Osservatorio 3 PaduaI-35122 Italy Istituto Nazionale di Astrofisica Osservatorio Astronomico di Padova Vicolo dell'Osservatorio 5 PaduaIT-35122 Italy Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China GEPI Observatoire de Paris Université PSL CNRS Place Jules Janssen Meudon92195 France 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 Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China

Multiple stellar populations (MPs) in most star clusters older than 2 Gyr, as seen by lots of spectroscopic and photometric studies, have led to a significant challenge to the traditional view of star formation. In this field, space-based instruments, in particular the Hubble Space Telescope (HST), have made a breakthrough as they significantly improved the efficiency of detecting MPs in crowding stellar fields by images. The China Space Station Telescope (CSST) and the HST are sensitive to a similar wavelength interval, but it covers a field of view which is about 5-8 times wider than that of HST. One of its instruments, the Multi-Channel Imager (MCI), will have multiple filters covering a wide wavelength range from NUV to NIR, making the CSST a potentially powerful tool for studying MPs in clusters. In this work, we evaluate the efficiency of the designed filters for the MCI/CSST in revealing MPs in different color-magnitude diagrams (CMDs). We find that CMDs made with MCI/CSST photometry in appropriate UV filters are powerful tools to disentangle stellar populations with different abundances of He, C, N, O and Mg. On the contrary, the traditional CMDs are blind to multiple populations in globular clusters (GCs). We show that CSST has the potential of being the spearhead instrument for investigating MPs in GCs in the next decades. Copyright © 2022, The Authors. All rights reserved.

关键词： Space stations

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A seven-Earth-radius helium-burning star inside a 20.5-min detached binary

arXiv

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arXiv 2023年

作者： Lin, Jie Wu, Chengyuan Xiong, Heran Wang, Xiaofeng Németh, Péter Han, Zhanwen Li, Jiangdan Elias-Rosa, Nancy Salmaso, Irene Filippenko, Alexei V. Brink, Thomas G. Yang, Yi Chen, Xuefei Yan, Shengyu Zhang, Jujia Guo, Sufen Cai, Yongzhi Mo, Jun Xi, Gaobo Liu, Jialian Guo, Jincheng Xia, Qiqi Xiang, Danfeng Li, Gaici Li, Zhenwei Zheng, WeiKang Zhang, Jicheng Liu, Qichun Guo, Fangzhou Chen, Liyang Li, Wenxiong Physics Department Tsinghua Center for Astrophysics Tsinghua University Beijing100084 China CAS Key laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei230026 China School of Astronomy and Space Sciences University of Science and Technology of China Hefei230026 China Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China Research School of Astronomy & Astrophysics Australian National University Canberra2611 Australia Beijing Planetarium Beijing Academy of Sciences and Technology Beijing100044 China Astronomical Institute of the Czech Academy of Sciences Fričova 298 Ondřejov25165 Czech Republic *** Fő tér 1 Malomsok8533 Hungary INAF-Osservatorio Astronomico di Padova Vicolo dell'Osservatorio 5 Padova35122 Italy Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Dipartimento di Fisica e Astronomia "G. Galilei" Università degli Studi di Padova Vicolo dell'Osservatorio 3 Padova35122 Italy Department of Astronomy University of California BerkeleyCA94720-3411 United States School of Physical Science and Technology Xinjiang University Urumqi830046 China Institute for Frontiers in Astronomy and Astrophysics Beijing Normal University 100875 China Department of Astronomy Beijing Normal University Beijing100875 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China The School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel

Binary evolution theory predicts that the second common envelope (CE) ejection can produce low-mass (0.32 − 0.36 M☉) subdwarf B (sdB) stars inside ultrashort-orbital-period binary systems, as their helium cores are ignited under nondegenerate conditions. With the orbital decay driven by gravitational-wave (GW) radiation, the minimum orbital periods of detached sdB binaries could be as short as ∼ 20 minutes. However, only four sdB binaries with orbital periods below an hour have been reported so far, while none of them has an orbital period approaching the above theoretical limit. Here we report the discovery of a 20.5-minute-orbital-period ellipsoidal binary, TMTS J052610.43+593445.1, in which the visible star is being tidally deformed by an invisible carbon-oxygen white dwarf (WD) companion. The visible component is inferred to be an sdB star with a mass of ∼ 0.33 M☉, approaching that of helium-ignition limit, although a He-core WD cannot be completely ruled out. In particular, the radius of this low-mass sdB star is only 0.066 R☉, about seven Earth radii, possibly representing the most compact nondegenerate star ever known. Such a system provides a key clue to map the binary evolution scheme from the second CE ejection to the formation of AM CVn stars having a helium-star donor, and it will also serve as a crucial verification binary of space-borne GW detectors in the future. Copyright © 2023, The Authors. All rights reserved.

关键词： White dwarfs

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Reverberation mapping of changing-look active galactic nucleus NGC 3516

arXiv

引用

arXiv 2020年

作者： Feng, Hai-Cheng Hu, Chen Li, Sha-Sha Liu, H.T. Bai, J.M. Xing, Li-Feng Wang, Wei-Yang Yang, Zi-Xu Xiao, Ming Lu, Kai-Xing Yunnan Observatories Chinese Academy of Sciences KunmingYunnan650011 China University of Chinese Academy of Sciences Beijing100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences KunmingYunnan650011 China Key Laboratory for Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences 19B Yuquan Road Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory for Computational Astrophysics National Astronomical Observatories Chinese Academy of Sciences 20A Datun Road Beijing100101 China

The changes of broad emission lines should be a crucial issue to understanding the physical properties of changing-look active galactic nucleus (CL-AGN). Here, we present the results of an intensive and homogeneous 6-month long reverberation mapping (RM) monitoring campaign during a low-activity state of the CL-AGN Seyfert galaxy NGC 3516. Photometric and spectroscopic monitoring was carried out during 2018–2019 with the Lijiang 2.4 m telescope. The sampling is 2 days in most nights, and the average sampling is ∼3 days. The rest frame time lags of Hα and Hβ are τHα = 7.56+4.42−2.10 days and τHβ = 7.50+2.05−0.77 days, respectively. From a RMS Hβ line dispersion of σline = 1713.3 ± 46.7 km s−1 and a virial factor of fσ = 5.5, the central black hole mass of NGC 3516 is estimated to be MBH = 2.4+0.7−0.3 × 107M☉, which is in agreement with previous estimates. The velocity-resolved delays show that the time lags increase towards negative velocity for both Hα and Hβ. The velocity-resolved RM of Hα is done for the first time. These RM results are consistent with other observations before the spectral type change, indicating a basically constant BLR structure during the changing-look process. The CL model of changes of accretion rate seems to be favored by long-term Hβ variability and RM observations of NGC 3516. Copyright © 2020, The Authors. All rights reserved.

关键词： Galaxies

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