检索结果-内蒙古大学图书馆

arXiv 2019年

作者： Yi, Weimin Zuo, Wenwen Yang, Jinyi Wang, Feige Timlin, John Grier, Catherine Wu, Xue-Bing Fan4, Xiaohui Bai, Jin-Ming Yunnan Observatories Kunming650216 China Department of Astronomy and Astrophysics Pennsylva-Nia State University 525 Davey Lab PA16802 United States Shanghai Astronomical Observatory Shanghai200030 China University of Arizona Steward Observatory 933 North Cherry Avenue TucsonAZ85721-0065 United States Kavli Institute for Astronomy and Astrophysics Peking Uni-versity Beijing100871 China Department of Astronomy Peking University Yi He Yuan Lu 5 Hai Dian District Beijing100871 China Cas Key Laboratory for Research in Galaxies and Cosmol-Ogy Department of Astronomy University of Science and Tech-Nology of China China Key Laboratory for Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China

We present an observational study of 22 broad absorption line quasars (BAL QSOs) at 3 z 5 based on optical/near-IR spectroscopy, aiming to investigate quasar winds and their effects. The near-IR spectroscopy covers the Hβ and/or Mg ii broad emission lines (BELs) for these quasars, allowing us to estimate their central black hole (BH) masses in a robust way. We found that our BAL QSOs on average do not have a higher Eddington ratio than that from non-BAL QSOs matched in redshift and/or luminosity. In a subset consisting of seven strong BAL QSOs possessing subrelativistic BAL outflows, we see the prevalence of large C iv-BEL blueshift (∼3100 km s-1) and weak [O iii] emission (particularly the narrow [O iii]λ5007 component), indicative of nuclear outflows affecting the narrow emission-line (NEL) regions. In another subset consisting of thirteen BAL QSOs having simultaneous observations of Mg ii and Hβ, we found a strong correlation between 3000 °A and 5000 °A monochromatic luminosity, consistent with that from non-BAL QSOs matched in redshift and luminosity;however, there is no correlation between Mg ii and Hβ in FWHM, likely due to nuclear outflows influencing the BEL regions. Our spectroscopic investigations offer strong evidence that the presence of nuclear outflows plays an important role in shaping the BEL/NEL regions of these quasars and possibly, regulating the growth of central supermassive black holes (SMBHs). We propose that BEL blueshift and BAL could be different manifestations of the same outflow system viewed at different sightlines and/or phases. Copyright © 2019, The Authors. All rights reserved.

关键词： Electromagnetic wave emission

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DISCOVERY AND TIMING OF MILLISECOND PULSARS IN THE GLOBULAR CLUSTER M5 (NGC 5904) WITH FAST AND ARECIBO

arXiv

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arXiv 2023年

作者： Zhang, Lei Freire, Paulo C.C. Ridolfi, Alessandro Pan, Zhichen Zhao, Jiaqi Heinke, Craig O. Chen, Jianxing Cadelano, Mario Pallanca, Cristina Hou, Xian Fu, Xiaoting Dai, Shi Gügercinoglu, Erbil Guo, Meng Hessels, Jason Hu, Jiale Li, Guodong Ni, Mengmeng Pan, Jingshan Ransom, Scott M. Ruan, Qitong Stairs, Ingrid Tsai, Chao-Wei Wang, Pei Wang, Long Wang, Na Wu, Qingdong Yuan, Jianping Zhang, Jie Zhu, Weiwei Zhang, Yongkun Li, Di National Astronomical Observatories Chinese Academy of Sciences A20 Datun Road Chaoyang District Beijing100101 China Centre for Astrophysics and Supercomputing Swinburne University of Technology P.O. Box 218 HawthornVIC3122 Australia Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53121 Germany INAF - Osservatorio Astronomico di Cagliari Via della Scienza 5 CA SelargiusI-09047 Italy Guizhou Radio Astronomical Observatory Guizhou University Guiyang550025 China College of Astronomy and Space Sciences University of Chinese Academy of Sciences Chinese Academy of Sciences Beijing100101 China Key Laboratory of Radio Astronomy and Technology Chinese Academy of Sciences Beijing100101 China Department of Physics University of Alberta CCIS 4-183 EdmontonABT6G 2E1 Canada Dipartimento di Fisica e Astronomia "Augusto Righi" Alma Mater Studiorum Università di Bologna via Piero Gobetti 93/2 BolognaI-40129 Italy INAF-Osservatorio di Astrofisica e Scienze dello Spazio di Bologna Via Piero Gobetti 93/3 BolognaI-40129 Italy 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 Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China School of Science Western Sydney University Locked Bag 1797 PenrithNSW2751 Australia National Supercomputing Center in Jinan Qilu University of Technology 28666 East Jingshi Road Licheng District Jinan250103 China Jinan Institute of Supercomputing Technology 28666 East Jingshi Road Licheng District Jinan250103 China ASTRON The Netherlands Institute for Radio Astronomy Oude Hoogeveensedijk 4 Dwingeloo7991 PD Netherlands Anton Pannekoek Institute for Astronomy University o

We report on a comprehensive multi-wavelength study of the pulsars in the globular cluster (GC) M5, including the discovery of M5G, a new compact non-eclipsing "black widow" pulsar. Thanks to the analysis of 34 years of radio data taken with the FAST and Arecibo telescopes, we obtained new phase-connected timing solutions for four pulsars and improved those of the other three. These have resulted in, among other things: a) much improved proper motions for five pulsars, with transverse velocities (relative to the cluster) that are smaller than their respective escape velocities;b) 3-σ and 1.5-σ detections of Shapiro delays in M5F and M5D, respectively;c) greatly improved measurement of the periastron advance in M5B, whose value of ω = 0.01361(6)◦ implies that M5B is still likely to be a heavy (Equation presented) neutron star. The binary pulsars M5D, E and F are confirmed to be in low-eccentricity binary systems, the low-mass companions of which are newly identified to be He white dwarfs using Hubble Space Telescope data. Four pulsars are also found to be associated with X-ray sources. Similarly to the eclipsing pulsar M5C, M5G shows little or no non-thermal X-ray emission, indicative of weak synchrotron radiation produced by intra-binary shocks. All the seven pulsars known in M5 have short spin periods ( Copyright © 2023, The Authors. All rights reserved.

关键词： Pulsars

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Photometric and spectroscopic studies of superoutbursts of three dwarf novae independently identified by the SVOM/GWAC system in 2018

arXiv

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arXiv 2019年

作者： Wang, J. Li, H.L. Xin, L.P. Han, X.H. Meng, X.M. Brink, T.G. Cai, H.B. Dai, Z.G. Filippenko, A.V. Hsia, C.-H. Huang, L. Jia, L. Li, G.W. Li, Y.B. Liang, E.W. Lu, X.M. Mao, J. Qiu, P. Qiu, Y.L. Ren, J.J. Turpin, D. Wang, H.J. Wang, X.G. Wang, X.Y. Wu, C. Xu, Y. Yan, J.Z. Zhang, J.B. Zheng, W. Wei, J.Y. Guangxi Key Laboratory for Relativistic Astrophysics School of Physical Science and Technology Guangxi University Nanning530004 China Key Laboratory of Space Astronomy and Technology National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Department of Astronomy University of California BerkeleyCA94720-3411 United States School of Astronomy and Space Science Nanjing University Nanjing210000 China State Key Laboratory of Lunar and Planetary Sciences Macau University of Science and Technology Taipa999078 China Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100101 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Purple Mountain Observatory Chinese Academy of Sciences Nanjing210034 China

We report our photometric and spectroscopic follow-up observations of the superoutbursts of three dwarf novae (GWAC 180415A, GWAC 181017A and GWAC 181211A) identified independently by the Ground Wide-angle Cameras system, one of the ground-based instruments of the China-France SVOM mission. Based on a combination of our photometry and that taken from the AAVSO, our period analysis of the superhumps enables us to determine the mass ratios to be 0.0967-0.1163, 0.1879-0.1883 and 0.0981-0.1173 for GWAC 180415A, GWAC 181017A and GWAC 181211A, respectively. GWAC 180415A can be firmly identified as a WZ sge-type dwarf novae due to its long duration (∼ 2 weeks) multiple rebrightenings with amplitudes of 3-4 magnitudes, the early superhump associated with a double-wave modulation and the low mass ratio. The inferred low mass ratio and location in the Ε − Porb diagram suggest that GWAC 181211A is a WZ sge-type dwarf novae candidate. The measured Balmer decrements suggest the Balmer line emission is produced from an optical thick region in GWAC 180415A and GWAC 181017A, and from an optical thin region in GWAC 181211A. Copyright © 2019, The Authors. All rights reserved.

关键词： Photometry

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Supermassive black holes with high accretion rates in active galactic nuclei: X. Optical variability characteristics

arXiv

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arXiv 2019年

作者： Lu, Kai-Xing Huang, Ying-Ke Zhang, Zhi-Xiang Wang, Kai Du, Pu Hu, Chen Xiao, Ming Li, Yan-Rong Bai, Jin-Ming Bian, Wei-Hao Yuan, Ye-Fei Ho, Luis C. Wang, Jian-Min Yunnan Observatories Chinese Academy of Sciences Kunming Yunnan650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Key Laboratory for Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences 19B Yuquan Road Beijing100049 China Physics Department Nanjing Normal University Nanjing210097 China Department of Astronomy University of Science and Technology of China Hefei230026 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China National Astronomical Observatories of China Chinese Academy of Sciences 20A Datun Road Beijing100020 China

We compiled a sample of 73 active galactic nuclei (AGNs) with reverberation mapping (RM) observations from RM campaigns including our ongoing campaign of monitoring super-Eddington accreting massive black holes (SEAMBHs). This sample covers a large range of black hole (BH) mass (M•= 10,6-9Mo), dimensionless accretion rates (M = 10-2.7- 102.7) and 5100 Å luminosity (L5100= 1042-46erg s-1), allowing us to systematically study the AGN variability and their relations with BH mass, accretion rates, and optical luminosity. We employed the damped random walk (DRW) model to delineate the optical variability of continuum at 5100 Å and obtained damped variability timescale (τd) and amplitude (σd) using a Markov Chain Monte Carlo (MCMC) method. We also estimated the traditional variability amplitudes (Fvar), which provide a model-independent measure and therefore are used to test the DRW results. We found that AGN variability characteristics are generally correlated with (M•,M,L5100). These correlations are smooth from sub-Eddington to super-Eddington accretion AGNs, probably implying that the AGN variability may be caused by the same physical mechanism. Copyright © 2019, The Authors. All rights reserved.

关键词： Luminance

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Observing the changing surface structures of the active K giant σ Gem with SONG

arXiv

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arXiv 2020年

作者： Korhonen, Heidi Roettenbacher, R.M. Gu, S. Grundahl, F. Andersen, M.F. Henry, G.W. Jessen-Hansen, J. Antoci, V. Pallé, P.L. Alonso de Córdova 3107 Vitacura Santiago Chile Yale Center for Astronomy and Astrophysics Department of Physics Yale University New HavenCT06520 United States Yunnan Observatories Chinese Academy of Sciences Kunming Yunnan Province650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China Stellar Astrophysics Centre Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Center of Excellence in Information Systems Tennessee State University NashvilleTN37209 United States DTU Space National Space Institute Technical University of Denmark Elektrovej 328 Kgs. LyngbyDK-2800 Denmark Instituto de Astrofísica de Canarias E-38205 La Laguna Tenerife Spain Universidad de La Laguna Departamento de Astrofísica La Laguna TenerifeE-38206 Spain

Aims. We aim to study the spot evolution and differential rotation in the magnetically active cool K-type giant star σ Gem from broadband photometry and continuous spectroscopic observations that span 150 nights. Methods. We use high-resolution, high signal-to-noise ratio spectra obtained with the Hertzsprung SONG telescope to reconstruct surface (photospheric) temperature maps with Doppler imaging techniques. The 303 observations span 150 nights and allow for a detailed analysis of the spot evolution and surface differential rotation. The Doppler imaging results are compared to simultaneous broadband photometry from the Tennessee State University T3 0.4 m Automated Photometric Telescope. The activity from the stellar chromosphere, which is higher in the stellar atmosphere, is also studied using SONG observations of Balmer Hα line profiles and correlated with the photospheric activity. Results. The temperature maps obtained during eight consecutive stellar rotations show mainly high-latitude or polar spots, with the main spot concentrations above latitude 45◦. The spots concentrate around phase 0.25 near the beginning of our observations and around phase 0.75 towards the end. The photometric observations confirm a small jump in spot phases that occurred in February 2016. The cross-correlation of the temperature maps reveals rather strong solar-like differential rotation, giving a relative surface differential rotation coefficient of α = 0.10 ± 0.02. There is a weak correlation between the locations of starspots and enhanced emission in the chromosphere at some epochs. Copyright © 2020, The Authors. All rights reserved.

关键词： Photometry

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YZ Phe: a very short period K-type contact binary with variation of the O’Connell effect and orbital period change

arXiv

引用

arXiv 2019年

作者： Sarotsakulchai, T. Qian, S.-B. Soonthornthum, B. Zhou, X. Zhang, J. Li, L.-J. Reichart, D.E. Haislip, J.B. Kouprianov, V.V. Poshyachinda, S. Yunnan Observatories Chinese Academy of Sciences Kunming650216 China University of Chinese Academy of Sciences 19 A Yuquan Rd. Shijingshan Beijing100049 China National Astronomical Research Institute of Thailand Donkaew MaerimChiang Mai50180 Thailand Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Rd. Chaoyang District Beijing100012 China Department of Physics and Astronomy University of North Carolina CB #3255 Chapel HillNC27599 United States

YZ Phe is a very short-period contact binary (Sp.= K2 V) with an orbital period of 0.2347 days near the short period limit (0.22 d). We present the complete light curves in V RI bands, which photometric data were obtained with the 0.61-m reflector of PROMPT-8 at CTIO in Chile during June to October 2016 and August 2017. The photometric solutions were determined by using the W-D method and the results reveal that YZ Phe is a W-subtype shallow contact binary (f ∼ 10%, q = 2.635 or 1/q = 0.379 for W subtype) with rotational motion of a large hot spot on the more massive component, showing a strong O’Connell effect with variation of maxima in photometric time series at period of 4.20 yr and stellar cycle at period of 1.28 yr. By compiling all available eclipse times, the result shows a long-term period decrease at a rate of dP/dt = −2.64(±0.02) × 10−8 d yr−1, superimposed on a cyclic variation (A3 = 0.0081 days and P3 = 40.76 years). This variation cannot be explained by Applegate mechanism. Thus, the cyclic change may be interpreted as light-travel time effect via the presence of a cool third body. Based on photometric solutions, the third light was detected with 2% of total light in V and I bands. Those support the existence of a third body. For the long-term period decrease, it can be explained by mass transfer from the more massive component (M2 ∼ 0.74M☉) to the less massive one (M1 ∼ 0.28M☉) or plus AML via magnetic braking. With 1/q Copyright © 2019, The Authors. All rights reserved.

关键词： Photometry

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SN 2017hpa: A nearby carbon-rich type ia supernova with a large velocity gradient

arXiv

引用

arXiv 2021年

作者： Zeng, Xiangyun Wang, Xiaofeng Esamdin, Ali Pellegrino, Craig Zheng, Weikang Zhang, Jujia Mo, Jun Li, Wenxiong Howell, D. Andrew Filippenko, Alexei V. Lin, Han Brink, Thomas G. Baron, Edward A. Burke, Jamison Derkacy, James M. McCully, Curtis Hiramatsu, Daichi Hosseinzadeh, Griffin Jeffers, Benjamin T. Ross, Timothy W. Stahl, Benjamin E. Stegman, Samantha Valenti, Stefano Wang, Lifan Xiang, Danfeng Zhang, Jicheng Zhang, Tianmeng Xinjiang Astronomical Observatory Chinese Academy of Sciences Xinjiang Urumqi830011 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing100049 China Tsinghua University Beijing100084 China Beijing Planetarium Beijing Academy of Science of Technology Beijing100044 China Department of Physics University of California Santa BarbaraCA93106-9530 United States Las Cumbres Observatory 6740 Cortona Drive Suite 102 GoletaCA93117-5575 United States Department of Astronomy University of California BerkeleyCA94720-3411 United States 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 School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Homer L. Dodge Department of Physics and Astronomy University of Oklahoma United States Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138-1516 United States Las Cumbres Observatory 6740 Cortona Drive Suite 102 GoletaCA9311-5575 United States Department of Physics University of California BerkeleyCA94720-7300 United States Department of Chemistry University of Wisconsin MadisonWI53706 United States Department of Physics University of California DavisCA95616 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy Texas A&M University Department of Physics and Astronomy 4242 TAMU College StationTX77843 United States Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China

We present extensive, well-sampled optical and ultraviolet photometry and optical spectra of the Type Ia supernova (SN Ia) 2017hpa. The light curves indicate that SN 2017hpa is a normal SN Ia with an absolute peak magnitude of MmaxB ≈ −19.12 ± 0.11 mag and a post-peak decline rate ∆m15(B) = 1.02 ± 0.07 mag. According to the quasibolometric light curve, we derive a peak luminosity of 1.25 × 1043 erg s−1and a 56Ni mass of 0.63 ± 0.02 M☉. The spectral evolution of SN 2017hpa is similar to that of normal SNe Ia, while it exhibits unusually rapid velocity evolution resembling that of SN 1991bg-like SNe Ia or the high-velocity subclass of SNe Ia, with a post-peak velocity gradient of ∼ 130 ± 7 km s−1 d−1. Moreover, its early spectra (t © 2021, CC BY.

关键词： White dwarfs

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Formation of the electronic spectrum in relativistic jets of gamma-ray blazars

arXiv

引用

arXiv 2018年

作者： Zheng, Y.G. Long, G.B. Yang, C.Y. Bai, J.M. Department of Physics Yunnan Normal University Kunming650092 China Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment Shandong University Weihai264209 Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for Structure and Evolution of Celestial Objects Chinese Academy of Sciences Department of Physics and Astronomy Sun Yat-Sen University Zhuhai519082 China

We describe the theory of Fermi-type acceleration, including first-order Fermi acceleration at a parallel shock front and second-order Fermi acceleration in a test particle limit. Including the theory of the turbulent acceleration and the derivation of the general Fokker-Planck equation, we take into account the basic particle-transport equation and the Fokker-Planck equation with spatially homogeneous isotropic distribution. In the cases of some special physical processes, we construct the particle-transport equations, and compile the analytical or semianalytical solutions in 11 different cases. Even though, traditionally, one of the electron energy distributions for these different cases can be used to reproduce the multi-wavelength emission of a blazar, due to very long integration times of high-energy observations, a time-integrated electron energy distribution should be introduced in approaches to modeling the multi-wavelength spectral energy distribution of blazars, especially in modeling the flaring state. Copyright © 2018, The Authors. All rights reserved.

关键词： Gamma rays

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Discovery of an accretion-rate independent absolute RMS amplitude of millihertz quasi-periodic oscillations in 4U 1636−53

arXiv

引用

arXiv 2019年

作者： Lyu, Ming Méndez, Mariano Altamirano, D. Zhang, Guobao Mancuso, G.C. Department of Physics Xiangtan University Xiangtan Hunan411105 China Kapteyn Astronomical Institute University of Groningen PO BOX 800 GroningenNL-9700 AV Netherlands Physics & Astronomy University of Southampton SouthamptonHampshireSO17 1BJ United Kingdom Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650216 China C.C. No. 5 Villa Elisa1894 Argentina Facultad de Ciencias Astronómicas y Geofísicas Universidad Nacional de La Plata Paseo del Bosque s/n La Plata1900 Argentina

We investigate the frequency and amplitude of the millihertz quasi-periodic oscillations (mHz QPOs) in the neutron-star low-mass X-ray binary (NS LMXB) 4U 1636–53 using Rossi X-ray Timing Explorer observations. We find that no mHz QPOs appear when the source is in the hard spectral state. We also find that there is no significant correlation between the frequency and the fractional rms amplitude of the mHz QPOs. Notwithstanding, for the first time, we find that the absolute RMS amplitude of the mHz QPOs is insensitive to the parameter Sa, which measures the position of the source in the colour-colour diagram and is usually assumed to be an increasing function of mass accretion rate. This finding indicates that the transition from marginally stable burning to stable burning or unstable burning could happen very rapidly since, before the transition, the mHz QPOs do not gradually decay as the rate further changes. Copyright © 2019, The Authors. All rights reserved.

关键词： Stars

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Synchrotron polarization of relativistic thermal electrons

arXiv

引用

arXiv 2018年

作者： Mao, Jirong Wang, Jiancheng Yunnan Observatories Chinese Academy of Sciences Kunming Yunnan Province650011 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 Kunming650011 China

Relativistic electrons accelerated by both the first-order and the second-order Fermi accelerations in some synchrotron sources have a hybrid shape of thermal and nonthermal energy distribution. This particle acceleration result is supported by some recent numerical simulations. We calculate the synchrotron polarization by applying this electron energy distribution. The polarization degrees in the cases of active galactic nucleus (AGN) jets and gamma-ray bursts (GRBs) are given as examples. The possible application for the polarization study of Sgr A* is also mentioned. We finally suggest high-energy polarization measurements for these synchrotron sources to test our results. Copyright © 2018, The Authors. All rights reserved.

关键词： Polarization

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