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arXiv 2017年

作者： Li, K.L. Kong, A.K.H. Tam, P.H.T. Hou, X. Takata, J. Hui, C.Y. Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Astrophysics Department of Physics University of Oxford Keble Road OxfordOX1 3RH United Kingdom Institute of Astronomy and Department of Physics National Tsing Hua University Hsinchu30013 Taiwan School of Physics and Astronomy Sun Yat-sen University Zhuhai519082 China 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 Institute of Particle Physics and Astronomy Huazhong University of Science and Technology China Department of Astronomy and Space Science Chungnam National University Daejeon Korea Republic of

We report our recent Swift, NuSTAR, and XMM-Newton X-ray and Lijiang optical observations on PSR J2032+4127/MT91 213, the γ-ray binary candidate with a period of 45–50 years. The coming periastron of the system was predicted to be in November 2017, around which high-energy flares from keV to TeV are expected. Recent studies with Chandra and Swift X-ray observations taken in 2015/16 showed that its X-ray emission has been brighter by a factors of ∼10 than that before 2013, probably revealing some on-going activities between the pulsar wind and the stellar wind. Our new Swift/XRT lightcurve shows no strong evidence of a single vigorous brightening trend, but rather several strong X-ray flares on weekly to monthly timescales with a slowly brightening baseline, namely the low state. The NuSTAR and XMM-Newton observations taken during the flaring and the low states, respectively, show a denser environment and a softer power-law index during the flaring state, implying that the pulsar wind interacted with stronger stellar winds of the companion to produce the flares. These precursors would be crucial in studying the predicted giant outburst from this extreme γ-ray binary during the periastron passage in late 2017. Copyright © 2017, The Authors. All rights reserved.

关键词： Pulsars

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Force-free magnetosphere on near-horizon geometry of near-extreme Kerr black holes

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Physical Review D 2015年第2期92卷 023009-023009页

作者： Huiquan Li Cong Yu Jiancheng Wang Zhaoyi Xu Yunnan Observatories Chinese Academy of Sciences 650011 Kunming China and Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 650011 Kunming China

We study force-free magnetospheres in the Blandford-Znajek process from rapidly rotating black holes by adopting the near horizon geometry of near-extreme Kerr black holes (near-NHEK). It is shown that the Znajek regularity condition on the horizon can be directly derived from the resulting stream equation. In terms of the condition, we split the full stream equation into two separate equations. Approximate solutions around the rotation axis are derived. They are found to be consistent with previous solutions obtained in the asymptotic region. The solutions indicate energy and angular-momentum extraction from the hole.

关键词： Magnetosphere Kerr black holes Electrodynamics

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A pair of CO + He white dwarfs as the progenitor of 2005E-like supernovae?

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Astronomy and Astrophysics 2015年第1期573卷

作者： Meng, Xiangcun Han, Zhanwen Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China

Context. Ca-rich transients (CRTs, 2005E-like supernovae) exhibit unusually strong Ca features during their nebular phase, and their distribution in their host galaxies indicates that they belong to a metal-poor old population. A pair of low-mass CO + He white dwarfs (WD) has been suggested to be the progenitor of CRTs. A helium shell is accumulated onto the CO WD by accretion, and then a helium-shell detonation is ignited when the helium shell reaches a critical mass, which could lead to the second detonation in the center of the CO ***. Taking the birth rate of CRTs into consideration, we examine whether and if yes, which type of low-mass CO + He WD pairs fulfill the constraints of being of an old population and of the birth rate derived from ***. We carried out a series of binary population syntheses and present four different channels in which CO + He WD pairs can be formed. We selected the systems that fulfill the constraints of being of an old population and of the birth rate from all the CO + He WD pairs by constraining the component mass of the WD ***. For the four channels, the stable Roche lobe overflow (RLOF) could significantly influence the formation of the WD pairs. Based on their position on the MCO-MHe plane, the mass-transfer between the components for most of the CO + He WD pairs is neither always unstable nor always stable. We found that it is necessary that the CO WDs are less massive than 0.6 M and the He WDs are less massive than 0.25 M if CO + He WD pairs are to fulfill the constraints of being of an old population and of the birth rate of CRTs. However, the He WD mass is lower than the ejecta mass of the CRTs derived from observations, while the total mass of the low-mass WD pairs is higher than ***. Our results imply that the CO WDs participate in CRT explosions and at the same time, a bound remnant could be left after the CRT explosion if the low-mass WD pairs are the progenitors of CRTs. Therefor

关键词： White dwarfs

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CO (7−6), [C i] 370 µm and [N ii] 205 µm line emission of the QSO BRI 1335-0417 at redshift 4.407

arXiv

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arXiv 2018年

作者： Lu, Nanyao Cao, Tianwen Díaz-Santos, Tanio Zhao, Yinghe Privon, George C. Cheng, Cheng Gao, Yu Xu, C. Kevin Charmandaris, Vassilis Rigopoulou, Dimitra van der Werf, Paul P. Huang, Jiasheng Wang, Zhong Evans, Aaron S. Sanders, David B. Beijing100012 China China-Chile Joint Center for Astronomy Camino El Observatorio 1515 Las Condes Santiago Chile School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing China Nucleo de Astronomia de la Facultad de Ingenieria Universidad Diego Portales Av. Ejercito Libertador 441 Santiago Chile Yunnan Observatories Chinese Academy of Sciences Kunming650011 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 Department of Astronomy University of Florida 211 Bryant Space Sciences Center GainesvilleFL32611 United States Departamento de Astronomía Universidad de Concepción Casilla 160-C Concepción Chile Pontificia Universidad Católica de Chile Instituto de Astrofisica Casilla 306 Santiago 22 Chile Instituto de Física y Astronomía Universidad de Valparaíso Avda. Gran Bretanã 1111 Valparaíso Chile Purple Mountain Observatory CAS Nanjing210008 China Department of Physics University of Crete HeraklionGR-71003 Greece IAASARS National Observatory of Athens PenteliGR-15236 Greece Department of Physics University of Oxford Keble Road OxfordOX1 3RH United Kingdom Leiden Observatory Leiden University PO Box 9513 Leiden2300 RA Netherlands Department of Astronomy University of Virginia 530 McCormick Road CharlottesvilleVA22904 United States National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903 United States University of Hawaii Institute for Astronomy 2680 Wood-lawn Drive HonoluluHI96822 United States

We present the results from our Atacama Large Millimeter/submillimeter Array (ALMA) imaging observations of the CO (7−6), [C i] 370 µm (hereafter [C i]) and [N ii] 205 µm (hereafter [N ii]) lines and their underlying continuum emission of BRI 1335-0417, an infrared bright quasar at z = 4.407. At the achieved resolutions of -1.1′′ to 1.2′′ (or 7.5 to 8.2 kpc), the continuum at 205 and 372 µm (rest-frame), the CO (7−6), and the [C i] emissions are at best barely resolved whereas the [N ii] emission is well resolved with a beam de-convolved major axis of 1.3′′ (±0.3′′) or 9 (±2) kpc. As a warm dense gas tracer, the CO (7−6) emission shows a more compact spatial distribution and a significantly higher peak velocity dispersion than the other two lines that probe lower density gas, a picture favoring a merger-triggered star formation (SF) scenario over an orderly rotating SF disk. The CO (7−6) data also indicate a possible QSO-driven gas outflow that reaches a maximum line-of-sight velocity of 500 to 600 km s−1. The far-infrared (FIR) dust temperature (Tdust) of 41.5 K from a graybody fit to the continuum agrees well with the average Tdust inferred from various line luminosity ratios. The resulting LCO(7−6)/LFIR luminosity ratio is consistent with that of local luminous infrared galaxies powered predominantly by SF. The LCO(7−6)-inferred SF rate is 5.1 (±1.5) × 103 M☉ yr−1. The system has an effective star-forming region of 1.7+1−0..78 kpc in diameter and a molecular gas reservoir of -5 × 1011 M☉. Copyright © 2018, The Authors. All rights reserved.

关键词： Density of gases

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Binary stars on the galaxy SFH

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Proceedings of the International Astronomical Union 2016年第S315期11卷 E86-E86页

作者： F. Zhang L. Li Z. Han Yunnan Observatories Chinese Academy of Sciences Kunming 650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 China email: zhangfh@***

Using the Yunnan-II evolutionary population synthesis models comprising binary stars, we find that the inclusion of binary stars can raise the derived stellar metallicity Z* and/or age t (degeneracy problem), raise the stellar mass M*, lower the gaseous metallicity Zgas and star formation rate (SFR) of galaxies. This means that a few stars form recently in galaxies, while more stars form during the entire evolution process when considering binary stars. If the degeneracy between t and Z* can be broken, its effect on the feedback process and star formation history can be determined.

关键词： (stars:) binaries: general galaxies: evolution

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The physical constraints on a new lobal QSO at Z = 4.82

arXiv

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arXiv 2017年

作者： Yi, Weimin Green, Richard Bai, Jin-Ming Wang, Tinggui Grier, Catherine J. Trump, Jonathan R. Brandt, William N. Zuo, Wenwen Yang, Jinyi Wang, Feige Yang, Chenwei Wu, Xue-Bing Zhou, Hongyan Fan, Xiaohui Jiang, Linhua Yang, Qian Varricatt, Watson Kerr, Tom Milne, Peter Benigni, Sam Wang, Jian-Guo Zhang, Jujia Wang, Fang Wang, Chuan-Jun Xin, Yu-Xin Fan, Yu-Feng Chang, Liang Zhang, Xiliang Lun, Bao-Li Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Steward Observatory University of Arizona TucsonAZ85721-0065 United States CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China China Department of Astronomy & Astrophysics Institute for Gravitation & the Cosmos Pennsylvania State University 525 Davey Laboratory University ParkPA16802 United States Hubble Department of Physics University of Connecticut Unit 3046 2152 Hillside Rd StorrsCT06269 United States Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Department of Astronomy School of Physics Peking University Beijing100871 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Polar Research Institute of China 451 Jinqiao Road Shanghai200136 China Center for Astronomical Mega-science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China UKIRT Observatory HiloHI96720 United States University of the Chinese Academy of Sciences Beijing100049 China Department of Physics Pennsylvania State University University ParkPA16802 United States Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China

Very few low-ionization broad absorption line (LoBAL) QSOs have been found at high redshifts to date. One high-redshift LoBAL QSO, J0122+1216, was recently discovered at the Lijiang 2.4-m Telescope with an initial redshift determination of 4.76. Aiming to investigate its physical properties, we carried out follow-up observations in the optical and near-IR spectroscopy. Near-IR spectra from UKIRT and P200 confirms that it is a LoBAL, with a new redshift determination of 4.82 ± 0.01 based on the Mg ii emission-line. The new Mg ii redshift determination reveals strong blueshifts and asymmetry of the high-ionization emission lines. We estimated a black hole mass of ∼ 2.3×109M☉ and Eddington ratio of ∼ 1.0 according to the empirical Mg ii-based single-epoch relation and bolometric correction factor. It is possible that strong outflows are the result of an extreme quasar environment driven by the high Eddington ratio. A lower limit on the outflowing kinetic power (> 0.9%LEdd) was derived from both emission and absorption lines, indicating these outflows play a significant role in the feedback process to regulate the growth of its black hole as well as host galaxy evolution. Copyright © 2017, The Authors. All rights reserved.

关键词： Ionization

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Photometric study of three ultrashort-period contact binaries

arXiv

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arXiv 2017年

作者： Liu, L. Qian, S.-B. Fernández Lajús, E. Essam, A. El-Sadek, M.A. Xiong, X. 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 Facultad de Ciencias Astronómicas y Geofísicas Universidad Nacional de La Plata Buenos Aires La Plata1900 Argentina Instituto de Astrofísica de La Plata CCT La Plata-CONICET UNLP Argentina Complejo Astronómico El Leoncito Consejo Nacional de Investigaciones Científicas y Técnicas Argentina National Universities of La Plata Córdoba National Research Institute of Astronomy and Geophysics Department of Astronomy Helwan Cairo Egypt

We carried out high-precision photometric observations of three eclipsing ultrashort-period contact binaries (USPCBs). Theoretical models were fitted to the light-curves by means of the Wilson-Devinney code. The solutions suggest that the three targets have evolved to a contact phase. The photometric results are as follows: a) 1SWASP J030749.87−365201.7, q = 0.439 ± 0.003, f = 0.0±3.6 %;b) 1SWASP J213252.93−441822.6, q = 0.560±0.003, f = 14.2±1.9 %;c) 1SWASP J200059.78+054408.9, q = 0.436 ± 0.008, f = 58.4 ± 1.8 %. The light curves show O’Connell effects, which can be modeled by assumed cool spots. The cool spots models are strongly supported by the night-to-night variations in the I-band light curves of 1SWASP J030749.87−365201.7. For a comparative study, we collected the whole set of 28 well-studied USPCBs with P 50 %). Generally, contact binaries with deep fill-out factors are going to merge, but it is believed that USPCBs have just evolved to a contact phase. Hence, the deep USPCB 1SWASPJ200059.78+054408.9 seems to be a contradiction, making it very interesting. Particularly, 1SWASPJ030749.87−365201.7 is a zero contact binary within thermal equilibrium, implying that it should be a turn-off sample as predicted by the thermal relaxation oscillation (TRO) theory. Copyright © 2017, The Authors. All rights reserved.

关键词： Photometry

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Hadronic Scenarios for Gamma-Ray Emission from Three Supernova Remnants Interacting with Molecular Clouds

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Chinese Physics Letters 2014年第4期31卷 206-209页

作者： YU Huan FANG Jun ZHANG Li Department of Physics Yunnan University Kunming 650091 Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011

GeV γ-rays detected with the large area telescope on board the Fermi Gamma-ray space telescope in the direc- tion of HB21, MSH 17-39 and G337.0-0.1 have been recently reported. The three supernova remnants （SNRs） show interactions with molecular clouds, and they are effective gamma-ray emitters as the relativistic protons accelerated by the SNR shocks inelastically colliding with the dense gas in the clouds. The origin of the observed γ-rays for the three remnants is investigated in the scenario of the diffusive shock acceleration. In the model, a part of the SNR shock transmits into the nearby molecular clouds, and the shock velocity is greatly reduced. As a result, a shock with a relatively low Alfven Mach number is generated, and the spectra of the accelerated protons and thee＇γ-ray photons produced via proton-proton interaction can be obtained. The results show that the observed γ-ray spectra for the three SNRs interacting with the molecular clouds can be reproduced. It can be concluded that the hadronic origin of the γ-rays for the three SNRs is approved, and the ability of SNR shocks to accelerate protons is also supported.

关键词： HADRONIC atoms GAMMA-ray absorption SUPERNOVA remnants PROTON-proton interactions PLASMA Alfven waves

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Determination of Disk Thickness of Face-on Spiral Galaxies and Image Processing Method^1,2

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Chinese Astronomy and Astrophysics 2015年第2期39卷 166-176页

作者： Hu, Tao Peng, Q.-H. Department of Automation Shanghai University Shanghai 200072 China Key Laboratory for the Structure and Evolution of Celestial Bodies Chinese Academy of Sciences Kunming 650011 China School of Astronomy and Space Science Nanjing University Nanjing 210093 China

It is unable to obtain the disk thickness of a face-on spiral galaxy by measuring its surface brightness distribution. Here, in order to obtain the disk thickness of faced-on spiral galaxies, we determine the scale heights of their disks using an analytical method, based on the asymptotic solution of Poison's equation of gravitational potential in a 3-D galactic disk under the equiangular logarithmic spiral type of density perturbation. For measuring the key parameter, namely the innermost position of spiral arms (forbidden radius r0), and free from the effect of light contamination of galactic bulge, an improved image processing method is used in this study by subtracting a two-component (disk+bulge) brightness model from the observed galaxy image. On the basis of some fitted and measured fundamental parameters of spiral structures, we obtain the disk thickness and other parameters for the two face-on spiral galaxies: one normal spiral galaxy (S) and one spiral bar galaxy (SB), and their ratio parameters (the scale ratio of bulge and disk rb/rd, and the ratio of disk scale and thickness rd/H) are also derived. By using this improved method of two-component subtraction, it is easy to obtain the forbidden radius r0, which is smaller than that obtained by measuring directly the original galaxy image, thus the obtained effective thickness of galactic disks becomes thinner. © 2015.

关键词： Galaxies: disk Galaxies: fundamental parameters Galaxies: spiral Galaxies: structure

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Gravitational Test beyond the First Post-Newtonian Order with the Shadow of the M87 Black Hole

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Physical Review Letters 2020年第14期125卷 141104-141104页

作者： Dimitrios Psaltis Lia Medeiros Pierre Christian Feryal Özel Kazunori Akiyama Antxon Alberdi Walter Alef Keiichi Asada Rebecca Azulay David Ball Mislav Baloković John Barrett Dan Bintley Lindy Blackburn Wilfred Boland Geoffrey C. Bower Michael Bremer Christiaan D. Brinkerink Roger Brissenden Silke Britzen Dominique Broguiere Thomas Bronzwaer Do-Young Byun John E. Carlstrom Andrew Chael Chi-kwan Chan Shami Chatterjee Koushik Chatterjee Ming-Tang Chen Yongjun Chen Ilje Cho John E. Conway James M. Cordes Geoffrey B. Crew Yuzhu Cui Jordy Davelaar Mariafelicia De Laurentis Roger Deane Jessica Dempsey Gregory Desvignes Jason Dexter Ralph P. Eatough Heino Falcke Vincent L. Fish Ed Fomalont Raquel Fraga-Encinas Per Friberg Christian M. Fromm Charles F. Gammie Roberto García Olivier Gentaz Ciriaco Goddi José L. Gómez Minfeng Gu Mark Gurwell Kazuhiro Hada Ronald Hesper Luis C. Ho Paul Ho Mareki Honma Chih-Wei L. Huang Lei Huang David H. Hughes Makoto Inoue Sara Issaoun David J. James Buell T. Jannuzi Michael Janssen Wu Jiang Alejandra Jimenez-Rosales Michael D. Johnson Svetlana Jorstad Taehyun Jung Mansour Karami Ramesh Karuppusamy Tomohisa Kawashima Garrett K. Keating Mark Kettenis Jae-Young Kim Junhan Kim Jongsoo Kim Motoki Kino Jun Yi Koay Patrick M. Koch Shoko Koyama Michael Kramer Carsten Kramer Thomas P. Krichbaum Cheng-Yu Kuo Tod R. Lauer Sang-Sung Lee Yan-Rong Li Zhiyuan Li Michael Lindqvist Rocco Lico Jun Liu Kuo Liu Elisabetta Liuzzo Wen-Ping Lo Andrei P. Lobanov Colin Lonsdale Ru-Sen Lu Jirong Mao Sera Markoff Daniel P. Marrone Alan P. Marscher Iván Martí-Vidal Satoki Matsushita Yosuke Mizuno Izumi Mizuno James M. Moran Kotaro Moriyama Monika Moscibrodzka Cornelia Müller Gibwa Musoke Alejandro Mus Mejías Hiroshi Nagai Neil M. Nagar Ramesh Narayan Gopal Narayanan Iniyan Natarajan Roberto Neri Aristeidis Noutsos Hiroki Okino Héctor Olivares Tomoaki Oyama Daniel C. M. Palumbo Jongho Park Nimesh Patel Ue-Li Pen Vincent Piétu Richard Plambeck Aleksandar PopStefanija Ben Prather Jorge A. Preciado-López Venkatessh Ramak Steward Observatory and Department of Astronomy University of Arizona 933 North Cherry Avenue Tucson Arizona 85721 USA School of Natural Sciences Institute for Advanced Study 1 Einstein Drive Princeton New Jersey 08540 USA National Radio Astronomy Observatory 520 Edgemont Road Charlottesville Virginia 22903 USA Massachusetts Institute of Technology Haystack Observatory 99 Millstone Road Westford Massachusetts 01886 USA National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan Black Hole Initiative at Harvard University 20 Garden Street Cambridge Massachusetts 02138 USA Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n E-18008 Granada Spain Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 D-53121 Bonn Germany Institute of Astronomy and Astrophysics Academia Sinica 11F of Astronomy-Mathematics Building AS/NTU No. 1 Sec. IV Roosevelt Road Taipei 10617 Taiwan Republic of China Departament d’Astronomia i Astrofísica Universitat de València C. Dr. Moliner 50 E-46100 Burjassot València Spain Observatori Astronmic Universitat de València C. Catedrático José Beltrán 2 E-46980 Paterna València Spain Center for Astrophysics–Harvard & Smithsonian 60 Garden Street Cambridge Massachusetts 02138 USA East Asian Observatory 660 North A’ohoku Place Hilo Hawaii 96720 USA Nederlandse Onderzoekschool voor Astronomie (NOVA) P.O. Box 9513 2300 RA Leiden Netherlands Institute of Astronomy and Astrophysics Academia Sinica 645 North A’ohoku Place Hilo Hawaii 96720 USA Institut de Radioastronomie Millimétrique 300 rue de la Piscine F-38406 Saint Martin d’Hères France Department of Astrophysics Institute for Mathematics Astrophysics and Particle Physics (IMAPP) Radboud University P.O. Box 9010 6500 GL Nijmegen Netherlands Korea Astronomy and Space Science Institute Daedeok-daero 776 Yuseong-gu Daejeon 34055 Republic of Korea University of Science and Technology Gajeong-ro 217 Yuseong-gu Daejeon 34113 Re

The 2017 Event Horizon Telescope (EHT) observations of the central source in M87 have led to the first measurement of the size of a black-hole shadow. This observation offers a new and clean gravitational test of the black-hole metric in the strong-field regime. We show analytically that spacetimes that deviate from the Kerr metric but satisfy weak-field tests can lead to large deviations in the predicted black-hole shadows that are inconsistent with even the current EHT measurements. We use numerical calculations of regular, parametric, non-Kerr metrics to identify the common characteristic among these different parametrizations that control the predicted shadow size. We show that the shadow-size measurements place significant constraints on deviation parameters that control the second post-Newtonian and higher orders of each metric and are, therefore, inaccessible to weak-field tests. The new constraints are complementary to those imposed by observations of gravitational waves from stellar-mass sources.

关键词： Astrophysical studies of gravity Classical black holes Experimental studies of gravity Astronomical black holes

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