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arXiv 2018年

作者： Li, Zhenwei Chen, Xuefei Chen, Hai-Liang Han, Zhanwen Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Science University of the Chinese Academy of Science Yuquan Road 19 Shijingshan Block Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Science 20A Datun Road Chaoyang District Beijing100012 China

Extremely low-mass white dwarfs (ELM WDs) are helium WDs with a mass less than ∼0.3 Mo. Most ELM WDs are found in double degenerates (DDs) in the ELM Survey led by Brown and Kilic. These systems are supposed to be significant gravitational-wave sources in the mHz frequency. In this paper, we firstly analyzed the observational characteristics of ELM WDs and found that there are two distinct groups in the ELM WD mass and orbital period plane, indicating two different formation scenarios of such objects, i.e. a stable Roche lobe overflow channel (RL channel) and common envelope ejection channel (CE channel). We then systematically investigated the formation of ELM WDs in DDs by a combination of detailed binary evolution calculation and binary population synthesis. Our study shows that the majority of ELM WDs with mass less than 0.22 Mo are formed from the RL channel. The most common progenitor mass in this way is in the range of 1.15 − 1.45 Mo and the resulting ELM WDs have a peak around 0.18 Mo when selection effects are taken into account, consistent with observations. The ELM WDs with a mass larger than 0.22 Mo are more likely to be from the CE channel and have a peak of ELM WD mass around 0.25 Mo which needs to be confirmed by future observations. By assuming a constant star formation rate of 2 Moyr−1 for a Milky Way-like galaxy, the birth rate and local density are 5 × 10−4 yr−1 and 1500 kpc−3, respectively, for DDs with an ELM WD mass less than 0.25 Mo. Copyright © 2018, The Authors. All rights reserved.

关键词： White dwarfs

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The metamorphosis of the Type Ib SN 2019yvr: late-time interaction

arXiv

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arXiv 2024年

作者： Ferrari, Lucía Folatelli, Gastón Kuncarayakti, Hanindyo Stritzinger, Maximilian Maeda, Keiichi Bersten, Melina Román Aguilar, Lili M. Sáez, M. Manuela Dessart, Luc Lundqvist, Peter Mazzali, Paolo Nagao, Takashi Ashall, Chris Bose, Subhash Brennan, S.J. Cai, Y.-Z. Handberg, Rasmus Holmbo, Simon Karamehmetoglu, Emir Pastorello, Andrea Reguitti, Andrea Anderson, Joseph Chen, Ting-Wan Galbany, Lluís Gromadzki, Mariusz Gutiérrez, Claudia P. Inserra, Cosimo Kankare, Erkki Müller Bravo, Tomás E. Mattila, Seppo Nicholl, Matt Pignata, Giuliano Sollerman, Jesper Srivastav, Shubham Young, David R. Instituto de Astrofísica de La Plata CONICET Argentina Facultad de Ciencias Astronómicas y Geofísicas Universidad Nacional de La Plata Paseo del Bosque S La PlataN B1900FWA Argentina The University of Tokyo Chiba Kashiwa277-8583 Japan Department of Physics and Astronomy University of Turku TurkuFI-20014 Finland University of Turku FI-20014 Finland Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Department of Astronomy Kyoto University Kitashirakawa-Oiwake-cho Sakyo-ku Kyoto606-8502 Japan RIKEN Saitama Wako351-0198 Japan Department of Physics University of California BerkeleyCA94720 United States Institut d’Astrophysique de Paris CNRS-Sorbonne Université 98 bis boulevard Arago Paris75014 France The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-10691 Sweden Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Str. 1 GarchingD-85748 Germany Astrophysics Research Institute Liverpool John Moores University 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Aalto University Metsähovi Radio Observatory Metsähovintie 114 Kylmälä02540 Finland Aalto University Department of Electronics and Nanoengineering P.O. BOX 15500 AaltoFI-00076 Finland Department of Physics Virginia Tech BlacksburgVA24061 United States Department of Astronomy The Ohio State University 140 W. 18th Avenue ColumbusOH43210 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 International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China INAF - Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 Padova35122 Italy Merate23807 Italy European Southern Observatory Alonso de Córdova 3107 Casilla 19 Santiago Chile Graduate Institute of Astronomy National Central University 300 Jhongda Road Jhongli32001

We present observational evidence of late-time interaction between the ejecta of the hydrogen-poor Type Ib supernova (SN) 2019yvr and hydrogen-rich circumstellar material (CSM), similar to the Type Ib SN 2014C. A narrow Hα emission line appears simultaneously with a break in the light-curve decline rate at around 80 − 100 d after explosion. From the interaction delay and the ejecta velocity, under the assumption that the CSM is detached from the progenitor, we estimate the CSM inner radius to be located at ∼ 6.5 − 9.1 × 1015 cm. The Hαemission line persists throughout the nebular phase at least up to +420 d post-explosion, with a full width at half maximum (FWHM) of ∼ 2000 km s−1. Assuming a steady mass loss, the estimated mass-loss rate from the luminosity of the Hα line is ∼ 3 − 7 × 10−5 M☉ yr−1. From hydrodynamical modeling and analysis of the nebular spectra, we find a progenitor He-core mass of 3 − 4 M, which would imply an initial mass of 13 − 15 M☉Our result supports the case of a relatively low mass progenitor possibly in a binary system as opposed to a higher mass single star undergoing an LBV phase. Copyright © 2024, The Authors. All rights reserved.

关键词： Supernovae

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

arXiv

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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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ROTATING BLACK HOLE SHADOW IN PERFECT FLUID DARK MATTER

arXiv

引用

arXiv 2018年

作者： Hou, Xian Xu, Zhaoyi Wang, Jiancheng 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

We study analytically the shadow cast by the rotating black hole in the perfect fluid dark matter. The apparent shape of the shadow depends upon the black hole spin a and the perfect fluid dark matter intensity parameter k (k > 0). In general, the shadow is a perfect circle in the non-rotating case (a = 0) and a deformed one in the rotating case (a 6= 0). The deformation gets more and more significant with the increasing a, similar to the Schwarzschild and Kerr black holes. In addition, there exists a reflection point k0. When k 0, the size of the shadow decreases with the increasing k and the distortion increases with the increasing k. When k > k0, the size of the shadow increases with the increasing k and the distortion decreases with the increasing k. Furthermore, the energy emission rate of the black hole in the perfect fluid dark matter increases with the increasing k and the peak of the emission shifts to higher frequencies. Finally, we propose that to observe the effect of the black hole spin a and the perfect fluid dark matter intensity k on the shadow of the black hole Sgr A∗ at the center of the Milky Way, highly improved techniques would be necessary for the development of future astronomical instruments. Copyright © 2018, The Authors. All rights reserved.

关键词： Galaxies

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

arXiv

引用

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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Star-formation rates of two GRB host galaxies at z ∼ 2 and a [C ii] deficit observed with ALMA

arXiv

引用

arXiv 2019年

作者： Hashimoto, Tetsuya Hatsukade, Bunyo Goto, Tomotsugu Kim, Seong Jin Ohta, Kouji Nagao, Tohru Kong, Albert K.H. Nakanishi, Kouichiro Mao, Jirong Institute of Astronomy National Tsing Hua University 101 Section 2. Kuang-Fu Road Hsinchu30013 Taiwan Institute of Astronomy Graduate School of Science University of Tokyo 2-21-1 Osawa Mitaka Tokyo181-0015 Japan Department of Astronomy Kyoto University Kitashirakawa-Oiwake-cho Sakyo-ku Kyoto Kyoto606-8502 Japan Research Center for Space and Cosmic Evolution Ehime University MatsuyamaEhime790-8577 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Yunnan Observatories Chinese Academy of Sciences Kunming Yunnan Province650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China

Event rate of long Gamma-Ray Bursts (GRBs) is expected to be an useful tracer of the cosmic star-formation history. For this purpose, it is necessary to understand what kind of star formations/galaxies are traced by GRBs. Here we report rest-frame far-infrared (FIR) continuum detections of GRB 070521 and 080207 host galaxies at z ∼ 2 with ALMA band 8 and 9. The FIR photometries provide the reliable star-formation rates (SFRs), because FIR emission is free from dust extinction and possible radio contamination from long-lived afterglows of GRBs. The spectral energy distribution fittings indicate 49.85+−722.86.33 and 123.4+−2521..1978 M yr−1 for the 070521 and 080207 hosts, respectively. The derived SFRs place them on the "main sequence" of normal star-forming galaxies at z ∼ 2. The derived SFRs are significantly lower than that of radio observations. It is inferred that the observed radio fluxes in a previous study are contaminated by the afterglows. ALMA marginally detected [C ii] 158 µm emission line from the GRB 080207 host galaxy with S/N ∼ 4. This is the first detection of [C ii] 158 µm of a GRB host at z > 2, and the second detection among known GRBs. The luminosity ratio of [C ii] 158µm to FIR is 7.5×10−4, which is one of the smallest values among galaxies at z ∼ 1 − 2 with the same FIR luminosity. The "[C ii] deficit" could be a new physical property to characterise GRB hosts at z ∼ 1 − 2. Possible parameters controlling the deficit include the metallicity, initial mass function, and gas density. Copyright © 2019, The Authors. All rights reserved.

关键词： Stars

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A Close-in Substellar Object Orbiting the sdOB-type Eclipsing-Binary System NSVS14256825

arXiv

引用

arXiv 2019年

作者： Zhu, L.-Y. Qian, S.-B. Lajús, Fernández E. Wang, Z.-H. Li, L.-J. 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 District Beijing100012 China University of Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China Facultad de Ciencias AstronómicasyGeofísicas Universidad Nacional de La Plata La PlataBuenos Aires1900 Argentina La Plata BA Paseo del Bosque s/n B1900FWA Argentina

NSVS 14256825 is the second sdOB + dM eclipsing binary systems with an orbital period of 2.65 hours. The special binary was reported to contain circumbinary planets or brown dwarfs by using the timing method. However, different results were derived by different authors because of the insufficient coverage of eclipse timings. Since 2008, we have monitored this binary for about 10 years by using several telescopes and 84 new times of light minimum in high precision were obtained. It is found that the O-C curve is increasing recently and it shows a cyclic variation with a period of 8.83 years and amplitude of 46.31 seconds. The cyclic change cannot be explained by magnetic activity cycles of the red-dwarf component because the required energy is much larger than that radiated by this component in one whole period. This cyclic change detected in NSVS1425 could be explained by the light-travel time effect via the presence of a third body. The lowest mass of the third body is determined as 14.15 Mjup that is in the transition between planets and brown dwarfs. The substellar object is orbiting around this evolved binary at an orbital separation around 3 AU with an eccentricity of 0.12. These results indicate that NSVS 14256825 is the first sdOB-type eclipsing binary consisting of a hierarchical substellar object. The detection of a close-in substellar companion to NSVS 14256825 will provide some insights on the formation and evolution of sdOB-type binaries and their companions. Copyright © 2019, The Authors. All rights reserved.

关键词： Systems (metallurgical)

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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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Possibility of identifying matter around rotating black hole with black hole shadow

arXiv

引用

arXiv 2018年

作者： Xu, Zhaoyi Hou, Xian Wang, Jiancheng 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

Shadows cast by the rotating black hole in perfect fluid matter are studied using analytical method. We consider three kinds of matter with standard equation of state in Cosmology: -1/3 (dark matter), 0 (dust) and 1/3 (radiation). The apparent shape of the shadow depends on the black hole spin a and the perfect fluid matter intensity k. We find that the shadow is a perfect circle in the non-rotating case (a = 0) and a distorted one in the rotating case (a ≠ 0), similar to what is found for other black holes. Interestingly, different kinds of matter have different influence on the black hole shadow. Dark matter has the strongest effect, dust is the next and radiation is the weakest. By applying our result to the black hole Sgr A∗ at the center of the Milky Way, we find that the angular resolution required to distinguish among different kinds of matter around the black hole is not much higher than the resolution of current astronomical instruments would be able to achieve in the near future. We propose that observing the black hole shadow provides a possibility of identifying the dominant matter near the black hole. Copyright © 2018, The Authors. All rights reserved.

关键词： Dust

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