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1SWASP J034439.97+030425.5:a short-period eclipsing binary system with a close-in stellar companion

Research in Astronomy and Astrophysics 2020年第4期20卷 31-38页

作者： Bin Zhang Sheng-Bang Qian Jing-Jing Wang Qi-Jun Zhi Ai-Jun Dong Wei Xie Li-Ying Zhu Lin-Qiao Jiang School of Physics and Electronic Science Guizhou Normal UniversityGuiyang 550001China Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guizhou Normal UniversityGuiyang 550001China Yunnan Observatories Chinese Academy of SciencesKunming 650216China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of SciencesKunming 650216China University of Chinese Academy of Sciences Beijing 100049China Center for Astronomical Mega-Science Chinese Academy of SciencesBeijing 100101China China University of Petroleum-Beijing at Karamay Karamay 834000China School of Physics and Electronic Engineering Sichuan University of Science and EngineeringZigong 643000China

First multi-wavelength photometric light curves(LCs)of the short-period eclipsing binary(EB)1 SWASP J034439.97+030425.5(hereafter J0344)are presented and analyzed by using the 2013 version of the Wilson-Devinney(W-D)*** explain the asymmetric LCs of J0344,a cool star-spot on the less massive component was *** photometric solutions suggest that J0344 is a W-subtype shallow contact EB with a contact degree of f=4.9%±3.0%and a mass ratio of q=2.456±***,an obvious third light was detected in our *** calculated the average luminosity contribution of the third light to the total light,and that value reaches up to 49.78%.Based on the O-C method,the variations of the orbital period were studied for the first *** O-C diagram reveals a secular decrease superimposed on a cyclic *** orbital period decreases at a rate of d P/dt=-6.07×10-7 d yr-1,which can be explained by the mass transfer from the more massive component to the less massive ***,its O-C diagram also shows a cyclic oscillation with an amplitude of 0.0030 d and a period about 7.08 yr,which can be explained by the presence of a third body with a minimum mass of M3 min=0.15±0.02 M⊙.The third component may play an important role in the formation and evolution of J0344 by drawing angular momentum from the central system.

关键词： stars:binaries:close stars:binaries:eclipsing stars:individual(1SWASP J034439.97+030425.5)

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Back to business: SLX 1746–331 after 13 years of silence

arXiv

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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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Interference location using an improved TDOA algorithm with antenna array and beamforming

Interference location using an improved TDOA algorithm with ...

引用

International Conference on Intelligent Computing, Communication and Devices, ICCD 2017

作者： Miao, Sheng Zhou, Hua Yang, Hongji Southwest Forestry University Kunming China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming China Centre for Creative Computing Bath Spa University Bath United Kingdom

ISBN: (纸本)9789811089435

Time Difference of Arrival (TDOA) is a popular interference location algorithm in the radio astronomy monitoring environment, where radio interference source may interfere with the performance of the receiver. However, with the geomagnetic white noise interference, interference detection is hard for a normal TDOA algorithm. In this paper, an improved interfere detection method is proposed. Single receiving antenna has been replaced by array antenna, and the adaptive beamforming algorithm is used in data preprocessing. A composite signal after beam-forming as an input of TDOA algorithm. The experiment shows that, comparing with the traditional TDOA algorithm and using beamforming, the location of the interference has been enhanced about 10 m for normal in the about 5 km. © Springer Nature Singapore Pte Ltd. 2019.

关键词： Beamforming

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One Reliable Method for Stellar Parameter Determination Based on Space Photometry and the Phoenix Spectral Library

SSRN

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SSRN 2022年

作者： Liu, Yisi Gu, Shenghong Perdelwitz, Volker Liu, Jing Yunnan Observatories Chinese Academy of Sciences Yunnan Kunming650216 China National Astronomical Observatories Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Yunnan Kunming650216 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China Hamburger Sternwarte Gojenbergsweg 112 Hamburg21029 Germany Department of Physics Ariel University Ariel40700 Israel

For a survey project, to get precise determination on parameters of stars is quite important. Although the second data release of Gaia provided stellar parameters for an unprecedented number of stars, due to the proximity of the Gaia passbands, the reliability of these parameters is still not unshakeable, especially for specific targets. In order to establish a reliable estimation of stellar parameters such as the effective temperature and so on, we are currently developing an algorithm which compares the absolute fluxes of all Gaia passbands, combined with those from the WISE mission, to PHOENIX spectra. Results have shown that a broader wavelength range enables a reliable determination of these parameters. Furthermore, the effective temperature we derived has a better precision than Gaia’s one, which shows the good performance of PHOENIX model. © 2022, The Authors. All rights reserved.

关键词： Surveys

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Unprecedented Central Engine "Breathing" Phenomenon in an Active Supermassive Black Hole

arXiv

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arXiv 2024年

作者： Zhou, Shuying Sun, Mouyuan Feng, Hai-Cheng Li, Sha-Sha Xue, Yongquan Wang, Jun-Xian Cai, Zhen-Yi Bai, Jin-Ming Li, Danyang Guo, Hengxiao Liu, H.T. Lu, Kai-Xing Mao, Jirong Marculewicz, Marcin Wang, Jian-Guo Department of Astronomy Xiamen University Fujian Xiamen361005 China SHAO-XMU Joint Center for Astrophysics Fujian Xiamen361005 China 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 Beijing100012 China Department of Astronomy University of Science and Technology of China Anhui Hefei230026 China School of Astronomy and Space Science University of Science and Technology of China Anhui Hefei230026 China High School Affiliated to Yunnan Normal College Yunnan Kunming650506 China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China

Resolving the inner structures of active galactic nuclei (AGNs) provides the "standard ruler" to measure the parallax distances of the Universe and a powerful way to weigh supermassive black holes (SMBHs). Thanks to time-domain observations, it is possible to use the reverberation mapping (RM) technique to measure time delays between different light curves that probe the structures of the SMBH accretion disks and broad line regions (BLRs), which are otherwise often too compact to be spatially resolved with current facilities for most AGNs. Despite decades of RM studies, the critical physical process that controls the structures of SMBH accretion disk and BLR and their temporal evolution remains unclear. Here we report the variation of the SMBH accretion disk structure of NGC 4151, a highly variable AGN, in response to changes in luminosity within ∼ 6 years. In the high-flux state, the time delays measured from our continuum RM with high-cadence (∼ 2 days) spectroscopy are 3.8+1.8−1.0 times larger than that in the low-flux state and 14.9 ± 2.0 times longer than the classical standard thin disk (SSD) prediction. This result provides the first piece of direct evidence that the SMBH disk structure "breathes" in highly-variable AGN manifestations. The significant time-delay change severely challenges the popular X-ray reprocessing of the classical SSD model, with or without contributions from BLRs. More importantly, the continuum time delays can be comparable with the time delay between the light curves of the broad Hβ emission line and the nearby optical continuum, and the latter is commonly used to calculate the BLR sizes. Hence, the BLR sizes are significantly underestimated if the continuum time delays are not properly considered. This underestimation introduces up to 0.3 dex systematic uncertainties on RM SMBH masses and BLR parallax distances. Our findings underscore that simultaneous continuum and BLR RM studies are vital for better deciphering the SMBH mass growt

关键词： Reverberation

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Monte-Carlo simulations on possible collimation effects of outflows to fan-beamed emission of ultraluminous accreting X-ray pulsars

arXiv

引用

arXiv 2022年

作者： Hou, X. You, Y. Ji, L. Soria, R. Zhang, S.N. Ge, M.Y. Tao, L. Zhang, S. Feng, H. Zhou, M. Tuo, Y.L. Song, L.M. Wang, J.C. Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Key Laboratory for 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 School of Physics and Astronomy Sun Yat-Sen University Zhuhai519082 China Sydney Institute for Astronomy School of Physics A28 The University of Sydney SydneyNSW2006 Australia Department of Astronomy Tsinghua University Beijing100084 China

Pulsating ultraluminous X-ray sources (PULXs) are accreting pulsars with apparent X-ray luminosity exceeding 1039 erg s−1. We perform Monte-Carlo simulations to investigate whether high collimation effect (or strong beaming effect) is dominant in the presence of accretion outflows, for the fan beam emission of the accretion column of the neutron stars in PULXs. We show that the three nearby PULXs (RX J0209.6−7427, Swift J0243.6+6124 and SMC X-3), namely the three musketeers here, have their main pulsed emission not strongly collimated even if strong outflows exist. This conclusion can be extended to the current sample of extragalactic PULXs, if accretion outflows are commonly produced from them. This means that the observed high luminosity of PULXs is indeed intrinsic, which can be used to infer the existence of very strong surface magnetic fields of ∼ 1013−14 G, possibly multipole fields. However, if strong outflows are launched from the accretion disks in PULXs as a consequence of disk spherization by radiation pressure, regular dipole magnetic fields of ∼ 1012 G may be required, comparable to that of the three musketeers, which have experienced large luminosity changes from well below their Eddington limit (2 × 1038 erg s−1 for a NS) to super-Eddington and their maximum luminosity fills the luminosity gap between Galactic pulsars and extragalactic PULXs. Copyright © 2022, The Authors. All rights reserved.

关键词： Luminance

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Close binary black hole in a radio-quiet quasar: a candidate of Nano-Hertz gravitational wave emitter

Research Square

引用

Research Square 2021年

作者： Feng, Hai-Cheng Liu, Hong-Tao Bai, Jin-Ming Yunnan Observatories Chinese Academy of Sciences Kunming Yunnan650011 China University of Chinese Academy of Sciences Beijing100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming Yunnan650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China

Close supermassive binary black holes (SMBBHs) with separations less than ∼ 0.1 parsec are expected to be Nano-Hertz gravitational wave sources1. SMBBH systems should exhibit periodic variability2. However, periodic variability in radio-loud quasars may be interpreted with the jet model3. Here we report the detection of a robust periodic signal in the optical variability of the radio-quiet quasar PG 0923+201 with an observed period of 726.8 ± 4.7 days, obtained from the sinusoid-like light curve of a temporal baseline of about 9 years. This periodicity is probably from a close SMBBH with a total mass of 109.3 solar masses and a separation of ∼ 0.01 parsec, implying relativistic orbital speeds. Such a system has passed through the well-known "final parsec problem" of SMBBH systems4, and the Nano-Hertz gravitational wave radiation becomes significant. The ratio of the separation between these two black holes to the broad-line region size is ∼ 0.1. A close SMBBH is also suggested by this small ratio and the spectral properties of Balmer broad lines in this quasar. This radio-quiet quasar is a candidate emitter of Nano-Hertz gravitational waves at a frequency of about 30 Nano-Hertz. © 2021, CC BY.

关键词： Gravity waves

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A post-common-envelope binary with double-peaked Balmer emission lines from TMTS

arXiv

引用

arXiv 2025年

作者： Liu, Qichun Wang, Xiaofeng Lin, Jie Wu, Chengyuan Li, Chunqian Filippenko, Alexei V. Brink, Thomas G. Yang, Yi Liu, Cheng Song, Cuiying Kovalev, Mikhail Ge, Hongwei Zhang, Fenghui Zhang, Xiaobin Xia, Qiqi Peng, Haowei Xi, Gaobo Mo, Jun Yan, Shengyu Shi, Jianrong Li, Jiangdan Yi, Tuan Physics Department Tsinghua University Beijing100084 China CAS Key laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei230026 China School of Astronomy and Space Sciences University of Science and Technology of China Hefei230026 China Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China School of Physics and Astronomy Beijing Normal University Beijing100875 China Institute for Frontiers in Astronomy and Astrophysics Beijing Normal University Beijing102206 China Department of Astronomy University of California BerkeleyCA94720-3411 United States Beijing Planetarium Beijing Academy of Science and Technology Beijing100044 China CAS 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 Beijing100049 China Department of Astronomy School of Physics Peking University Beijing100871 China Kavli Institute of Astronomy and Astrophysics Peking University Beijing100871 China

Context. The dynamical method provides an efficient way to discover post-common-envelope binaries (PCEB) with faint white dwarfs (WDs), thanks to the development of time-domain survey projects. As close binary systems undergo a common-envelope phase, they offer unique opportunities to study the astrophysical processes associated with binary evolution. Aims. We perform a comprehensive analysis of the PCEB system TMTS J15530469+4457458 (J1553), discovered by the Tsinghua University-Ma Huateng Telescopes for Survey, to explore its physical origin and evolutionary fate. Methods. This system is characterized by double-peaked Balmer emission lines, and a cross-correlation function is applied to derive its radial velocity (RV) from a series of phase-resolved Keck spectra. The physical parameters of this binary were obtained by fitting the light curves and RV simultaneously. The locations of the Balmer lines were inferred from Doppler tomography, and a MESA simulation was performed to explore the evolution of this system. Results. Analyses with the cross-correlation function suggest that this system is a single-lined spectroscopic binary and only one star is optically visible. Further analysis through Doppler tomography indicates that J1553 is a detached binary without an accretion disk. Under such a configuration, the simultaneous light-curve and RV fitting reveal that this system contains an unseen WD with mass MA = 0.56 ± 0.09 M☉, and an M4 dwarf with mass MB = 0.37 ± 0.02 M☉ and radius RB = 0.403+−00.014015 R☉. The extra prominent Balmer emission lines seen in the spectra can trace the motion of the WD, which are likely formed near the WD surface as a result of wind accretion. According to the MESA simulation, J1553 could have evolved from a binary consisting of a 2.0–4.0 M☉ zero-age-main-sequence star and an M dwarf with an initial orbital period Pi ≈ 201 − 476 d, and the system has undergone a common-envelope (CE) phase. After about 3.3 × 106 yr, J1553 should evolve i

关键词： White dwarfs

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Three new late-type hypervelocity star candidates from Gaia DR2 with refined selection criteria

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Research in Astronomy and Astrophysics 2020年第3期20卷 170-184页

作者： Jiao Li Shi Jia Yan Gao Deng-Kai Jiang Thomas Kupfer Ulrich Heber Chao Liu Xue-Fei Chen Zhan-Wen Han Yunnan observatories Chinese Academy of SciencesKunming 650011China Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan observatoriesChinese Academy of SciencesKunming 650011China University of Chinese Academy of Sciences Beijing 100049China Center for Astronomical Mega-Science Chinese Academy of SciencesBeijing 100101China State Key Laboratory of Lunar and Planetary Sciences Macao University of Science and TechnologyMacaoChina Kavli Institute for Theoretical Physics University of CaliforniaSanta BarbaraCA 93106USA Department of Physics University of CaliforniaSanta BarbaraCA 93106USA Dr.Remeis-Sternwarte&ECAP University of Erlangen-NurnbergErlangenGermany Key Lab of Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China

Several dozen hypervelocity star(HVS)candidates have been reported based on the second data release of Gaia(Gaia DR2).However,it has been proven that the radial velocities of some Gaia HVS candidates are not *** this paper,we employ refined astrometric criteria to re-examine Gaia DR2,arriving at a more reliable sample of HVS and high velocity star candidates than those found by previous *** develop a method called Binary Escape Probability Analysis to identify some HVS *** method allows us to work with stars having only two epochs of measured radial *** stars were usually discarded in previous similar studies.A scrutiny of our final results sheds light on selection effects present in our studies,which we propose to be the focus of future *** total,we find three late-type(2 G-type and 1 K-type)HVS and 21 high velocity star candidates,3 and 11 of which are new,*** by their historical trajectories,which we calculate,all three HVS candidates could not have had Galactic center *** monitoring is required to confirm their status.

关键词： stars kinematics and dynamics-evolution-statistics

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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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