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New CCD photometric investigation of the early-type overcontact binary BH Cen in the young star-forming Galactic cluster IC 2944

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Research in Astronomy and Astrophysics 2018年第5期18卷 119-130页

作者： Er-Gang Zhao Sheng-Bang Qian Miloslav Zejda Bin Zhang Jia Zhang Yunnan Observatories Chinese Academy of Sciences Kunming 650216 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing 100101 China University of Chinese Academy of Sciences Beijing 100049 China Department of Theoretical Physics and Astrophysics Masaryk University Brno Czech Republic

BH Cen is a short-period early-type binary with a period of 0.792^d in the extremely young star-forming cluster IC 2944. New multi-color CCD photometric light curves in U, B, V, R and I bands are presented and are analyzed by using the Wilson-Devinney code. It is detected that BH Cen is a high-mass-ratio overcontact binary with a fill-out factor of 46.4% and a mass ratio of 0.89. The derived orbital inclination i is 88.9 degrees, indicating that it is a totally eclipsing binary and the photometric parameters can be determined reliably. By adding new eclipse times, the orbital period changes in the binary are analyzed. It is confirmed that the period of BH Cen shows a long-term increase while it undergoes a cyclic oscillation with an amplitude of A3 = 0.024 d and a period of P3 = 50.3 yr. The high mass ratio, overcontact configuration and long-term continuous increase in the orbital period all suggest that BH Cen is in the evolutionary state after the shortest-period stage of Case A mass *** continuous increase in period can be explained by mass transfer from the secondary component to the primary one at a rate of˙M2 = 2.8×10^-6 M⊙per year. The cyclic change can be plausibly explained by the presence of a third body because both components in the BH Cen system are early-type stars. Its mass is determined to be no less than 2.2 M⊙ at an orbital separation of about 32.5 AU. Since no third light was found during the photometric solution, it is possible that the third body may be a candidate for a compact object.

关键词： binary （including multiple） close - stars binaries eclipsing - stars early-type - stars evolution - stars individual （BH Cen）

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The study of multi-peaked type-I X-ray bursts in the neutron-star low mass X-ray binary 4U 1636−536 with RXTE

arXiv

引用

arXiv 2020年

作者： Li, Chen Zhang, Guobao Méndez, Mariano Wang, Jiancheng Lyu, Ming 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 University of Chinese Academy of Science Beijing100049 China Kapteyn Astronomical Institute University of Groningen P.O. Box 800 GroningenNL-9700 AV Netherlands Department of Physics Xiangtan University Xiangtan Hunan411105 China Key Laboratory of Stars and Interstellar Medium Xiangtan University Xiangtan Hunan411105 China

We have found and analysed 16 multi-peaked type-I bursts from the neutron-star low mass X-ray binary 4U 1636−53 with the Rossi X-ray Timing Explorer (RXTE). One of the bursts is a rare quadruple-peaked burst which was not previously reported. All 16 bursts show a multi-peaked structure not only in the X-ray light curves but also in the bolometric light curves. Most of the multi-peaked bursts appear in observations during the transition from the hard to the soft state in the colour-colour diagram. We find an anti-correlation between the second peak flux and the separation time between two peaks. We also find that in the double-peaked bursts the peak-flux ratio and the temperature of the thermal component in the pre-burst spectra are correlated. This indicates that the double-peaked structure in the light curve of the bursts may be affected by enhanced accretion rate in the disc, or increased temperature of the neutron star. Copyright © 2020, The Authors. All rights reserved.

关键词： Stars

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A seven-Earth-radius helium-burning star inside a 20.5-min detached binary

arXiv

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arXiv 2023年

作者： Lin, Jie Wu, Chengyuan Xiong, Heran Wang, Xiaofeng Németh, Péter Han, Zhanwen Li, Jiangdan Elias-Rosa, Nancy Salmaso, Irene Filippenko, Alexei V. Brink, Thomas G. Yang, Yi Chen, Xuefei Yan, Shengyu Zhang, Jujia Guo, Sufen Cai, Yongzhi Mo, Jun Xi, Gaobo Liu, Jialian Guo, Jincheng Xia, Qiqi Xiang, Danfeng Li, Gaici Li, Zhenwei Zheng, WeiKang Zhang, Jicheng Liu, Qichun Guo, Fangzhou Chen, Liyang Li, Wenxiong Physics Department Tsinghua Center for Astrophysics 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 the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China Research School of Astronomy & Astrophysics Australian National University Canberra2611 Australia Beijing Planetarium Beijing Academy of Sciences and Technology Beijing100044 China Astronomical Institute of the Czech Academy of Sciences Fričova 298 Ondřejov25165 Czech Republic *** Fő tér 1 Malomsok8533 Hungary INAF-Osservatorio Astronomico di Padova Vicolo dell'Osservatorio 5 Padova35122 Italy Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Dipartimento di Fisica e Astronomia "G. Galilei" Università degli Studi di Padova Vicolo dell'Osservatorio 3 Padova35122 Italy Department of Astronomy University of California BerkeleyCA94720-3411 United States School of Physical Science and Technology Xinjiang University Urumqi830046 China Institute for Frontiers in Astronomy and Astrophysics Beijing Normal University 100875 China Department of Astronomy Beijing Normal University Beijing100875 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China The School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel

Binary evolution theory predicts that the second common envelope (CE) ejection can produce low-mass (0.32 − 0.36 M☉) subdwarf B (sdB) stars inside ultrashort-orbital-period binary systems, as their helium cores are ignited under nondegenerate conditions. With the orbital decay driven by gravitational-wave (GW) radiation, the minimum orbital periods of detached sdB binaries could be as short as ∼ 20 minutes. However, only four sdB binaries with orbital periods below an hour have been reported so far, while none of them has an orbital period approaching the above theoretical limit. Here we report the discovery of a 20.5-minute-orbital-period ellipsoidal binary, TMTS J052610.43+593445.1, in which the visible star is being tidally deformed by an invisible carbon-oxygen white dwarf (WD) companion. The visible component is inferred to be an sdB star with a mass of ∼ 0.33 M☉, approaching that of helium-ignition limit, although a He-core WD cannot be completely ruled out. In particular, the radius of this low-mass sdB star is only 0.066 R☉, about seven Earth radii, possibly representing the most compact nondegenerate star ever known. Such a system provides a key clue to map the binary evolution scheme from the second CE ejection to the formation of AM CVn stars having a helium-star donor, and it will also serve as a crucial verification binary of space-borne GW detectors in the future. Copyright © 2023, The Authors. All rights reserved.

关键词： White dwarfs

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The bright long-lived Type II SN 2021irp powered by aspherical circumstellar material interaction (I): Revealing the energy source with photometry and spectroscopy

arXiv

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arXiv 2025年

作者： Reynolds, T.M. Nagao, T. Gottumukkala, R. Gutiérrez, C.P. Kangas, T. Kravtsov, T. Kuncarayakti, H. Maeda, K. Elias-Rosa, N. Fraser, M. Kotak, R. Mattila, S. Pastorello, A. Pessi, P.J. Cai, Y.-Z. Fynbo, J.P.U. Kawabata, M. Lundqvist, P. Matilainen, K. Moran, S. Reguitti, A. Taguchi, K. Yamanaka, M. Tuorla Observatory Department of Physics and Astronomy University of Turku TurkuFI-20014 Finland Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 København N2200 Denmark Aalto University Metsähovi Radio Observatory Metsähovintie 114 Kylmälä02540 Finland Aalto University Department of Electronics and Nanoengineering P.O. BOX 15500 AaltoFI-00076 Finland Edifici RDIT Campus UPC Castelldefels Barcelona08860 Spain Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain University of Turku FI-20014 Finland Department of Astronomy Kyoto University Kitashirakawa-Oiwake-cho Sakyo-ku Kyoto606-8502 Japan INAF – Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaI-35122 Italy UCD School of Physics L.M.I. Main Building Beech Hill Road Dublin 4 D04 P7W1 Ireland School of Sciences European University Cyprus Diogenes Street Engomi Nicosia1516 Cyprus The Oskar Klein Centre Department of Astronomy Stockholm University Albanova University Center StockholmSE 106 91 Sweden Yunnan Observatories Chinese Academy of Sciences Kunming650216 China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Okayama Observatory Kyoto University 3037-5 Honjo Kamogatacho Asakuchi Okayama719-0232 Japan INAF – Osservatorio Astronomico di Brera Via E. Bianchi 46 LC MerateI-23807 Italy Graduate School of Science and Engineering Kagoshima University 1-21-35 Korimoto Kagoshima Kagoshima890-0065 Japan

Context. Some core-collapse supernovae (CCSNe) are too luminous and radiate too much total energy to be powered by the release of thermal energy from the ejecta and radioactive-decay energy from the synthesised 56Ni/56Co. A source of additional power is the interaction between the supernova (SN) ejecta and a massive circumstellar material (CSM). This is an important power source in Type IIn SNe, which show narrow spectral lines arising from the unshocked CSM, but not all interacting SNe show such narrow lines. Aims. We present photometric and spectroscopic observations of the hydrogen-rich SN 2021irp, which is both luminous, with Mo o = -18 mag for ∼ 250 d. We show that an additional energy source is required to power such a SN, and determine the nature of the source. We also investigate the properties of the pre-existing and newly formed dust associated with the SN. Methods. Photometric observations show that the luminosity of the SN is an order of magnitude higher than typical Type II SNe and persists for much longer. We detect a infrared excess attributed to dust emission. Spectra show multi-component line profiles, an Fe ii pseudo-continuum and a lack of absorption lines, all typical features of Type IIn SNe. We detect a narrow (-1) P-Cygni profile associated with the unshocked CSM. An asymmetry in emission line profiles indicates dust formation occurring from 250-300 d. Analysis of the SN blackbody radius evolution indicates asymmetry in the shape of the emitting region. Results. We identify the main power source of SN 2021irp as extensive interaction with a massive CSM, and that this CSM is distributed asymmetrically around the progenitor star. The infrared excess is explained with emission from newly formed dust although there is also some evidence of an IR echo from pre-existing dust at early times. © 2025, CC BY.

关键词： Supernovae

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Detection of Gamma-Rays from the Protostellar Jet in the HH 80-81 System

arXiv

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arXiv 2019年

作者： Yan, Dahai Zhou, Jianeng Zhang, Pengfei Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Department of Astronomy Key Laboratory of Astroparticle Physics of Yunnan Province Yunnan University Kunming650091 China

Considering that the existence of relativistic particles in the protostellar jet has been confirmed by the detection of linearly polarized radio emission from the HH 80-81 jet, we search for gamma-rays from the HH 80-81 system using ten-year Fermi-LAT observations. A significant point-like γ-ray excess is found in the direction of the HH 80-81 system with Test-Statistic (TS) value >100, which is likely produced in the HH 80-81 jet. The γ-ray spectrum extends only to 1 GeV with a photon index of 3.5. No significant variability is found in the gamma-ray emission. It is discussed that the properties of HH 80-81 jet suffice for producing the observed γ-rays. Copyright © 2019, The Authors. All rights reserved.

关键词： Gamma rays

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

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Astronomy and Astrophysics 2025年 698卷

作者： Liu, Qichun Wang, Xiaofeng Lin, Jie Wu, Chengyuan Li, Chunqian Filippenko, Alexei V. Brink, Thomas G. Yang, Yi Zheng, Weikang 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 (PCEBs) 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 we applied a cross-correlation function 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 using 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 Mo, and an M4 dwarf with mass MB = 0:37 ±0:02 Mo and radius RB = 0:403+0:014 -0:015 Ro. The extra prominent Balmer emission lines seen in the spectra can trace the motion of the WD;these lines 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 Mo zero-agemain- 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 evol

关键词： White dwarfs

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Gamma-ray luminosity function of BL Lac objects and contribution to the extragalactic gamma-ray background

arXiv

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arXiv 2019年

作者： Qu, Yankun Zeng, Houdun Yan, Dahai Key laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing210008 China University of Chinese Academy of Sciences Yuquan Road 19 Beijing100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatory Chinese Academy of Sciences Kunming650011 China

Using a significantly enlarged Fermi-LAT BL Lac objects (BL Lacs) sample, we construct the gamma-ray luminosity function (GLF) of BL Lacs, by the joint use of the space density distribution and source counts distribution. We use three well-studied forms of the GLF, i.e., the forms of pure density evolution (PDE), pure luminosity evolution (PLE) and luminosity-dependent density evolution (LDDE). The Markov Chain Monte Carlo (MCMC) technique is used to constrain model parameters. Our results suggest that LDDE model can give the best description for the BL Lac GLF. And the model shows that the BL Lacs with a harder GeV spectrum and a less luminosity evolve as strongly as FSRQs, and the evolution decreases as increasing luminosity. We also model the average photon spectra of BL Lacs with a double power laws model. Using this modeled spectra, BL Lacs contribute ∼ 20% of the total extragalactic gamma-ray background (EGB) at E > 100 MeV, ∼ 100% of the EGB at E > 50 GeV, and the unresolved BL Lacs contribute ∼ 20% of the isotropic diffuse gamma-ray background (IGRB) at E > 100 MeV. A prediction of the TeV EGB spectra are given, which may be tested by the future detectors. Copyright © 2019, The Authors. All rights reserved.

关键词： Gamma rays

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Finding Quasars behind the Galactic Plane. II. Spectroscopic Identifications of 204 Quasars at |b|<20°

arXiv

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arXiv 2022年

作者： Fu, Yuming Wu, Xue-Bing Jiang, Linhua Zhang, Yanxia Huo, Zhi-Ying Ai, Y.L. Yang, Qian Ma, Qinchun Feng, Xiaotong Joshi, Ravi Hon, Wei Jeat Wolf, Christian Li, Jiang-Tao Yao, Su Pang, Yuxuan Wang, Jian-Guo Jin, Jun-Jie Lu, Kai-Xing Wang, Chuan-Jun Zheng, Jie Xu, Liang Yu, Xiao-Guang Lun, Bao-Li Zuo, Pei Department of Astronomy School of Physics Peking University Beijing100871 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China CAS Key Laboratory of Optical Astronomy National Astronomical Observatories Beijing100101 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China College of Engineering Physics Shenzhen Technology University Shenzhen518118 China Shenzhen Key Laboratory of Ultraintense Laser and Advanced Material Technology Shenzhen518118 China Department of Astronomy University of Illinois at Urbana-Champaign UrbanaIL61801 United States School of Physics University of Melbourne ParkvilleVIC3010 Australia Research School of Astronomy and Astrophysics Australian National University CanberraACT2611 Australia Centre for Gravitational Astrophysics Australian National University CanberraACT2600 Australia Department of Astronomy University of Michigan 311 West Hall 1085 S. University Avenue Ann ArborMI48109-1107 United States Purple Mountain Observatory Chinese Academy of Sciences 10 Yuanhua Road Nanjing210023 China Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 BonnD-53121 Germany Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China University of Chinese Academy of Sciences Beijing100049 China University of Western Australia 35 Stirling Highway CrawleyWA6009 Australia

Quasars behind the Galactic plane (GPQs) are important astrometric references and valuable probes of Galactic gas, yet the search for GPQs is difficult due to severe extinction and source crowding in the Galactic plan... 详细信息

关键词： Stars

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Spot model for identifications of periods in asynchronous polars

arXiv

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arXiv 2020年

作者： Wang, Qishan Qian, Shengbang Han, Zhongtao Fang, Xiaohui Zang, Lei Liu, Wei 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 University of Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Science 20A Datun Road Chaoyang Distric Beijing100012 China Guizhou Provincial Key Laboratory of Radio Data Processing School of Physics and Electronic Sciences Guizhou Normal University Guiyang550001 China

We improved the discless accretion models of Wynn & King, considering the effects of the changing aspect due to the white dwarf spin and the variable feeding intensity caused by the asynchronism, and set up a more general spot model which is not sensitive to the different forms of these effects and can be applied for the period analysis of the optical and X-ray light curve. The spot model can produce the power spectra compatible with the observations, and its simulations limit the ratio Pspin/Porb Copyright © 2020, The Authors. All rights reserved.

关键词： White dwarfs

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Reverberation mapping of changing-look active galactic nucleus NGC 3516

arXiv

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arXiv 2020年

作者： Feng, Hai-Cheng Hu, Chen Li, Sha-Sha Liu, H.T. Bai, J.M. Xing, Li-Feng Wang, Wei-Yang Yang, Zi-Xu Xiao, Ming Lu, Kai-Xing Yunnan Observatories Chinese Academy of Sciences KunmingYunnan650011 China University of Chinese Academy of Sciences Beijing100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences KunmingYunnan650011 China Key Laboratory for Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences 19B Yuquan Road Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory for Computational Astrophysics National Astronomical Observatories Chinese Academy of Sciences 20A Datun Road Beijing100101 China

The changes of broad emission lines should be a crucial issue to understanding the physical properties of changing-look active galactic nucleus (CL-AGN). Here, we present the results of an intensive and homogeneous 6-month long reverberation mapping (RM) monitoring campaign during a low-activity state of the CL-AGN Seyfert galaxy NGC 3516. Photometric and spectroscopic monitoring was carried out during 2018–2019 with the Lijiang 2.4 m telescope. The sampling is 2 days in most nights, and the average sampling is ∼3 days. The rest frame time lags of Hα and Hβ are τHα = 7.56+4.42−2.10 days and τHβ = 7.50+2.05−0.77 days, respectively. From a RMS Hβ line dispersion of σline = 1713.3 ± 46.7 km s−1 and a virial factor of fσ = 5.5, the central black hole mass of NGC 3516 is estimated to be MBH = 2.4+0.7−0.3 × 107M☉, which is in agreement with previous estimates. The velocity-resolved delays show that the time lags increase towards negative velocity for both Hα and Hβ. The velocity-resolved RM of Hα is done for the first time. These RM results are consistent with other observations before the spectral type change, indicating a basically constant BLR structure during the changing-look process. The CL model of changes of accretion rate seems to be favored by long-term Hβ variability and RM observations of NGC 3516. Copyright © 2020, The Authors. All rights reserved.

关键词： Galaxies

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