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arXiv 2025年

作者： Peng, Jing-Qiang Zhang, Shu Wang, Peng-Ju Zhang, Shuang-Nan Kong, Ling-Da Chen, Yu-Peng Shui, Qing-Cang Ji, Long Qu, Jin-Lu Tao, Lian Ge, Ming-Yu Ma, Rui-Can Chang, Zhi Li, Jian Li, Zhao-Sheng Yu, Zhuo-Li Yan, Zhe Zhang, Peng Xiao, Yun-Xiang Zhao, Shu-Jie Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China University of Chinese Academy of Sciences Chinese Academy of Sciences Beijing100049 China Institute für Astronomie und Astrophysik Kepler Center for Astro and Particle Physics Eberhard Karls Universität Sand 1 TübingenD-72076 Germany School of Physics and Astronomy Sun Yat-Sen University Zhuhai519082 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 Key Laboratory of Stars and Interstellar Medium Xiangtan University Hunan Xiangtan411105 China Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China College of Science China Three Gorges University Yichang443002 China Center for Astronomy and Space Sciences China Three Gorges University Yichang443002 China

The black hole candidate system SLX 1746–331 was back to business in 2023, after a long silence of roughly 13 years. An outburst was observed thoroughly by Insight-HXMT and NICER. The outburst is characterized by spectral dominance of the soft state, where the joint Insight-HXMT and NICER spectral analysis shows the temperature dependence of the disk flux follows Tin3.98, and thus suggests that the inner disk reaches to ISCO during almost the entire outburst. By assuming 0.3 LEdd for the peak flux and an inclination angle of zero degrees, the lower limit of the compact object hosted in this system is estimated as 3.28±2.14M☉. We also look into the relation of the disk temperature and disk flux for a sample of black hole systems, and by taking the disk temperature derived in the outburst of SLX 1746–331, such a relation results in a mass estimation of 5.2 ± 4.5M☉. Finally, the spin of the compact object is constrained to larger than 0.8 with a spectral model of kerrbb. Copyright © 2025, The Authors. All rights reserved.

关键词： Black holes

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Velocity-Resolved Ionization Mapping of Broad Line Region. I. Insights into Diverse Geometry and Kinematics

arXiv

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arXiv 2024年

作者： Li, Sha-Sha Feng, Hai-Cheng Liu, H.T. Bai, J.M. Ji, Xiang Pang, Yu-Xuan Cheng, Cheng Lu, Kai-Xing Wang, Jian-Guo Li, Rui Yunnan Observatories Chinese Academy of Sciences Yunnan Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Yunnan Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory of Radio Astronomy and Technology Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100101 China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Department of Astronomy School of Physic Peking University Beijing100871 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China CAS Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China School of Physics and Microelectronics Zhengzhou University Zhengzhou450001 China

Broad emission lines of active galactic nuclei (AGNs) originate from the broad-line region (BLR), consisting of dense gas clouds in orbit around an accreting supermassive black hole. Understanding the geometry and kinematics of the region is crucial for gaining insights into the physics and evolution of AGNs. Conventional velocity-resolved reverberation mapping may face challenges in disentangling the degeneracy between intricate motion and geometry of this region. To address this challenge, new key constraints are required. Here, we report the discovery of an asymmetric BLR using a novel technique: velocity-resolved ionization mapping, which can map the distance of emitting gas clouds by measuring Hydrogen line ratios at different velocities. By analyzing spectroscopic monitoring data, we find that the Balmer decrement is anticorrelated with the continuum and correlated with the lags across broad emission line velocities. Some line ratio profiles deviate from the expectations for a symmetrically virialized BLR, suggesting that the red-shifted and blue-shifted gas clouds may not be equidistant from the supermassive black hole (SMBH). This asymmetric geometry might represent a formation imprint, provide new perspectives on the evolution of AGNs, and influence SMBH mass measurements. © 2024, CC BY.

关键词： Kinematics

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Comparing the Super-Eddington accretion of SMC X-3 and RX J0209.6-7427 with Swift J0243.6+6124

arXiv

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arXiv 2022年

作者： Liu, Jiren Vasilopoulos, Georgios Ge, MingYu Ji, Long Weng, Shan-Shan Zhang, Shuang-Nan Hou, Xian Beijing Planetarium 138 Sizhimenwai Road Beijing100044 China Observatoire astronomique de Strasbourg UMR 7550 StrasbourgF-67000 France Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China School of Physics and Astronomy Sun Yat-sen University 2 Daxue Road Guangdong Zhuhai519082 China Department of Physics Institute of Theoretical Physics Nanjing Normal University Nanjing210023 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

We study the giant outbursts of SMC X-3 and RX J0209.6-7427 to compare their super-Eddington accretion regime with that of Swift J0243.6+6124. The high double-peak profile of SMC X-3 is found to be 0.25 phase offset from that below 2.3 × 1038erg s−1, which is similar to Swift J0243 (happened around 0.9 × 1038erg s−1). The profile of RX J0209 shows a similar 0.25 phase offset between high double-peak and low double-peak around 1.25 × 1038erg s−1. The 0.25 phase offset corresponds to a 90 degree angle change of the emission beam and strongly supports for a transition from a fan beam to a pencil beam. Their critical luminosities imply a surface magnetic field ∼ 4 × 1013 G and 2 × 1013 G for SMC X-3 and RX J0209, respectively, based on the recently measured cyclotron line of Swift J0243. The spin-up rate and luminosity of SMC X-3 follows a relation of ν ∝ L0.94±0.03, while that of RX J0209 follows ν ∝ L1.00±0.03, which are similar to Swift J0243 and consistent with the prediction of a radiation-pressure-dominated (RPD) disk. These results indicate that accretion columns are indeed formed above Eddington luminosity, and the population of ULXPs likely corresponds to X-ray pulsars of highest magnetic field. Copyright © 2022, The Authors. All rights reserved.

关键词： Luminance

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K2 photometry on oscillation mode variability: the new pulsating hot B subdwarf star EPIC 220422705

arXiv

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arXiv 2022年

作者： Ma, Xiao-Yu Zong, Weikai Fu, Jian-Ning Reed, M.D. Wang, Jiaxin Charpinet, Stéphane Su, Jie Department of Astronomy Beijing Normal University Beijing100875 China Department of Physics Astronomy and Materials Science Missouri State University 901 S. National SpringfieldMO65897 United States College of Science Chongqing University of Posts and Telecommunications Chongqing 400065 China Institut de Recherche en Astrophysique et Planétologie CNRS Université de Toulouse CNES 14 Avenue Edouard Belin Toulouse31400 France Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China

We present analysis of oscillation mode variability in the hot B subdwarf star EPIC 220422705, a new pulsator discovered from ∼ 78 days of K2 photometry. The high-quality light curves provide a detection of 66 significant independent frequencies, from which we identified 9 incomplete potential triplets and 3 quintuplets. Those g- and p-multiplets give rotation periods of ∼ 36 and 29 days in the core and at the surface, respectively, potentially suggesting a slightly differential rotation. We derived a period spacing of 268.5 s and 159.4 s for the sequence of dipole and quadruple modes, respectively. We characterized the precise patterns of amplitude and frequency modulations (AM and FM) of 22 frequencies with high enough amplitude for our science. Many of them exhibit intrinsic and periodic patterns of AM and FM, with periods on a timescale of months as derived by the best fitting and MCMC test. The nonlinear resonant mode interactions could be a natural interpretation for such AMs and FMs after other mechanisms are ruled out. Our results are the first step to build a bridge between mode variability from K2 photometry and nonlinear perturbation theory of stellar oscillation. © 2022, CC BY.

关键词： Photometry

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Rotating spacetime: Black-bounces and quantum deformed black hole

arXiv

引用

arXiv 2021年

作者： Xu, Zhaoyi Tang, Meirong College of Physics Guizhou University Guiyang550025 China Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China University of Chinese Academy of Sciences Beijing100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China

Recently, two kinds of deformed schwarzschild spacetime have been proposed, which are the black-bounces metric ([1, 2]) and quantum deformed black hole (BH) ([3]). In present work, we investigate the rotating spacetime of these deformed Schwarzschild metric. They are exact solutions to the Einstein′s field equation. We analyzed the properties of these rotating spacetimes, such as event horizon (EH), stationary limit surface (SIS), structure of singularity ring, energy condition (EC), etc., and found that these rotating spacetime have some novel properties. Copyright © 2021, The Authors. All rights reserved.

关键词： Gravitation

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New photometric investigation of the low-mass-ratio contact binary star V1853 Orionis

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Research in Astronomy and Astrophysics 2019年第4期19卷 77-88页

作者： Jia-Jia He Sheng-Bang Qian Boonrucksar Soonthornthum Amornrat Aungwerojwit Niang-Ping Liu Thawicharat Sarotsakulchai Yunnan Observatories Chinese Academy of Sciences Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Center for Astronomical Mega-Science Chinese Academy of Sciences University of Chinese Academy of Sciences National Astronomical Research Institute of Thailand 191 Siriphanich Bldg.2nd Fl.Huay Kaew Rd.Suthep DistrictMuang Department of Physics Faculty of Science Naresuan University

Four-color charge-coupled device(CCD) light curves in the B, V, Rc and I c bands of the totaleclipsing binary system V1853 Orionis(V1853 Ori) are presented. By comparing our light curves with those published by previous investigators, it is determined that the O'Connell effect on the light curves has disappeared. By analyzing those multi-color light curves with the Wilson-Devinney code(W-D code),it is discovered that V1853 Ori is an A-type intermediate-contact binary with a degree of contact factor of f = 33.3%(3.7%) and a mass ratio of q = 0.1896(0.0013). Combining our 10 newly determined times of light minima together with others published in the literature, the period changes of the system are investigated. We found that the general trend of the observed minus calculated(O-C) curve shows a downward parabolic variation that corresponds to a long-term decrease in the orbital period with a rate of d P/dt =-1.96(0.46)×10^(-7) d yr^(-1). The long-term period decrease could be explained by mass transfer from the more-massive component to the less-massive one. By combining our photometric solutions with data from Gaia DR_2, absolute parameters were derived as M_1 = 1.20 M⊙, M_2 = 0.23 M⊙, R_1 = 1.36 R⊙and R_2 = 0.66 R⊙. The long-term period decrease and intermediate-contact configuration suggest that V1853 Ori will evolve into a high fill-out overcontact binary.

关键词： stars: binaries:close stars:binaries:eclipsing stars:individual(V1853 Ori)

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Constraining evolution of magnetic field strength in dissipation region of two BL Lac objects

arXiv

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arXiv 2021年

作者： Fan, Xu-Liang Yan, Da-Hai Wu, Qingwen Chen, Xu School of Mathematics Physics and Statistics Shanghai University of Engineering Science Shanghai201620 China Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China School of Physics Huazhong University of Science and Technology Wuhan430074 China Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment Institute of Space Sciences Shandong University Weihai264209 China

With the assumption that the optical variability timescale is dominated by the cooling time of the synchrotron process for BL Lac objects, we estimate time dependent magnetic field strength of the emission region for two BL Lac objects. The average magnetic field strengths are consistent with those estimated from core shift measurement and spectral energy distribution modelling. Variation of magnetic field strength in dissipation region is discovered. Variability of flux and magnetic field strength show no clear correlation, which indicates the variation of magnetic field is not the dominant reason of variability origin. The evolution of magnetic field strength can provide another approach to constrain the energy dissipation mechanism in jet. © 2021, CC BY.

关键词： Magnetic fields

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Discovery of the Closest Ultrastripped Supernova: SN 2021agco in UGC 3855

arXiv

引用

arXiv 2023年

作者： Yan, Shengyu Wang, Xiaofeng Gao, Xing Zhang, Jujia Filippenko, Alexei V. Brink, Thomas G. Mo, Jun Lin, Weili Xiang, Danfeng Ma, Xiaoran Guo, Fangzhou Tomasella, Lina Benetti, Stefano Cai, Yongzhi Cappellaro, Enrico Chen, Zhihao Li, Zhitong Pastorello, Andrea Zhang, Tianmeng Tsinghua University Haidian District Beijing100084 China Beijing Planetarium Beijing Academy of Sciences and Technology Beijing100044 China Xinjiang Astronomical Observatory Urumqi830011 China Yunnan Observatories Chinese Academy of Sciences Kunming260216 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 Department of Astronomy University of California BerkeleyCA94720-3411 United States INAF – Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 Padova35122 Italy Key Laboratory of Space Astronomy and Technology National Astronomical Observatories Chinese Academy of Sciences 20A Datun Road Beijing100101 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China

We present the discovery and studies of the helium-rich, fast-evolving supernova (SN) 2021agco at a distance of ∼ 40 Mpc. Its early-time flux is found to rise from half peak to the peak of −16.06 ± 0.42 mag in the r band within (formula presented) days, and the post-peak light curves also decline at a much faster pace relative to normal stripped-envelope SNe of Type Ib/Ic. The early-time spectrum of SN 2021agco (t ≈ 1.0 days after the peak) is characterized by a featureless blue continuum superimposed with a weak emission line of ionized C III, and the subsequent spectra show prominent He I lines. Both the photometric and spectroscopic evolution shows close resemblances to SN 2019dge, which is believed to have an extremely stripped progenitor. We reproduce the multicolor light curves of SN 2021agco with a model combining shock-cooling emission with 56Ni decay. The best-fit results give an ejecta mass of ≈ 0.3 M☉ and a synthesized nickel mass of ≈ 2.2 × 10−2 M☉. The progenitor is estimated to have an envelope radius Renv ≈ 80 R☉ and a mass Menv ≈ 0.10 M☉. All these suggest that SN 2021agco can be categorized as an ultrastripped SN Ib, representing the closest object of this rare subtype. This SN is found to explode in the disk of an Sab-type galaxy with an age of ∼ 10.0 Gyr and low star-forming activity. Compared to normal SNe Ib/c, the host galaxies of SN 2021agco and other ultrastripped SNe tend to have relatively lower metallicity, which complicates the properties of their progenitor populations. © 2023, CC BY.

关键词： Supernovae

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Deformed black hole immersed in dark matter spike

arXiv

引用

arXiv 2021年

作者： Xu, Zhaoyi Wang, Jiancheng Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China College of Physics Guizhou University Guiyang550025 China Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China University of Chinese Academy of Sciences Beijing100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China

If a lot of dark matter particles accumulate near the black hole, then the chances of detecting dark matter signals near a black hole are greatly increased. These effects may be observed by the Event Horizon Telescope (EHT), Tianqin project, Taiji project, Laser Interferometer Space Antenna (LISA) and Laser Interferometer Gravitational-Wave Observatory (LIGO). In this work, we explore the effects of dark matter spikes on black hole space-time. For the Schwarzschild-like black hole case, we consider Newton′s approximation and perturbation approximation. This makes it possible to use Xu′s method to solve the Einstein field equation, and extend Schwarzschild-like black hole to Kerr-like black hole (BH) via Newman-Janis (NJ) algorithm. By analyzing the dark matter spike on the black hole event horizon (EH), stationary limit surfaces (SLS), ergosphere and energy-momentum tensors (EMT), we found that compared with the dark matter halo, the dark matter spike would have a higher effect on the black hole by several orders of magnitude. Therefore, if there is a dark matter spike near the black hole, it is very possible to test the dark matter model through gravitational wave (GW) observation and EHT observation. Copyright © 2021, The Authors. All rights reserved.

关键词： Antennas

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LHAASO J2226+6057 as a pulsar wind nebula

arXiv

引用

arXiv 2022年

作者： De Sarkar, Agnibha Zhang, Wei Martín, Jonatan Torres, Diego F. Li, Jian Hou, Xian Raman Research Institute Karnataka Bengaluru560080 India Campus UAB Carrer de Magrans s/n BarcelonaE-08193 Spain INAF - Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 FirenzeI-50125 Italy BarcelonaE-08034 Spain Barcelona Spain CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei China School of Astronomy and Space Science University of Science and Technology of China Hefei 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

Context. The Large High Altitude Air Shower Observatory has reported the detection of cosmic-ray sources in Milky Way that can accelerate particles up to PeV (= 1015 eV) energies. These sources, so called "PeVatrons", are mostly unidentified. Several classes of sources, such as supernova remnants, pulsar wind nebula, or young stellar clusters can potentially be the counterparts of these PeVatrons. Aims. The aim of this work is to study a pulsar wind nebula interpretation of one of these PeVatrons, LHAASO J2226+6057, which has a relatively well covered multi-frequency spectrum. Methods. We have performed a leptonic, time-dependent modeling of the pulsar wind nebula (PWN) associated with PSR J2229+6114 considering a time-energy-dependent diffusion-loss equation. Injection, energy losses, as well as escape of particles were considered to balance the time-dependent lepton population. We have also included the dynamics of the PWN and the associated supernova remnant (SNR) and their interaction via the reverse shock to study the reverberation phase of the system. Results. We have considered different values of braking index (n) and true age (tage) for the fitting of the multi-wavelength (MWL) spectral energy distribution (SED) of LHAASO J2226+6057. The best-fit PWN model parameters and their 1σ confidence intervals were evaluated. We have also demonstrated the impact of reverberation on the MWL SED with increasing time. Additionally, we have discussed the resultant large radius and low magnetic field associated with the PWN in question, as caveats for the possible physical connection of the pulsar as the origin of this high energy source. © 2022, CC BY.

关键词： Reverberation

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