检索结果-内蒙古大学图书馆

arXiv 2018年

作者： Yan, Dahai Zhou, Jianeng Zhang, Pengfei Zhu, Qianqian Wang, Jiancheng Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatory Chinese Academy of Sciences Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing210008 China Key Laboratory of Astroparticle Physics of Yunnan Province Yunnan University Kunming650091 China Department of General Studies Nanchang Institute of Science & Technology Nanchang330108 China

The mechanism for producing gamma-ray quasi-periodic oscillation (QPO) in blazar is unknown. One possibility is the geometric model, in which without the need for intrinsic quasi-periodic variation, the relativistic Doppler factor changes periodically, resulting in observed gamma-ray QPO. We propose a method to test this geometric model. We analyze the Fermi-LAT data of PG 1553+113 spanning from 2008 August until 2018 February. According to 29 four-month average spectral energy distributions (SEDs) in the energy range of 0.1-300 GeV, we split the Fermi-LAT energy range into three bands: 0.1-1 GeV, 1-10 GeV, and 10-300 GeV. The spectrum in each energy range can be successfully fitted by a power-law. The light curves and photon indices in the three energy ranges are obtained. Then, light curves in three narrow energy ranges, i.e., 0.2-0.5 GeV, 2-5 GeV and 20- 40 GeV, are constructed, and the relative variability amplitudes in the three narrow energy ranges are calculated. A discrete- correlation analysis is performed for the light curves. Our results indicate that (i) the light curves in the different energy ranges follow the same pattern showed in the light curve above 0.1 GeV;(ii) the three groups of photon indices in the energy ranges of 0.1-1 GeV, 1-10 GeV, and 10-300 GeV keep nearly constant;(iii) the ratio between relative variability amplitudes in different narrow energy ranges are equal (within their errors) to the prediction by the Doppler e ect. Our results support the scenario of the relativistic boost producing the gamma-ray QPO for PG 1553+113. Copyright © 2018, The Authors. All rights reserved.

关键词： Germanium alloys

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Expanded solutions of force-free electrodynamics on general Kerr black holes

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Physical Review D 2017年第2期96卷 023014-023014页

作者： Huiquan Li Jiancheng Wang Yunnan Observatories Chinese Academy of Sciences 650216 Kunming China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 650216 Kunming China and Center for Astronomical Mega-Science Chinese Academy of Sciences 100012 Beijing China

In this work, expanded solutions of force-free magnetospheres on general Kerr black holes are derived through a radial distance expansion method. From the regular conditions both at the horizon and at spatial infinity, two previously known asymptotical solutions (one of them is actually an exact solution) are identified as the only solutions that satisfy the same conditions at the two boundaries. Taking them as initial conditions at the boundaries, expanded solutions up to the first few orders are derived by solving the stream equation order by order. It is shown that our extension of the exact solution can (partially) cure the problems of the solution: it leads to magnetic domination and a mostly timelike current for restricted parameters.

关键词： Electromagnetic radiation astronomy

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Massive stars, successes and challenges

arXiv

引用

arXiv 2017年

作者： Meynet, Georges Maeder, André Georgy, Cyril Ekström, Sylvia Eggenberger, Patrick Barblan, Fabio Song, Han Feng Department of Astronomy University of Geneva Switzerland College of Science Guizhou University GuiyangGuizhou Province550025 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China

We give a brief overview of where we stand with respect to some old and new questions bearing on how massive stars evolve and end their lifetime. We focus on the following key points that are further discussed by other contributions during this conference: convection, mass losses, rotation, magnetic field and multiplicity. For purpose of clarity, each of these processes are discussed on its own but we have to keep in mind that they are all interacting between them offering a large variety of outputs, some of them still to be discovered. Copyright © 2017, The Authors. All rights reserved.

关键词： Magnetic fields

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JWST NIRSpec+MIRI Observations of the nearby Type IIP supernova 2022acko

arXiv

引用

arXiv 2024年

作者： Shahbandeh, M. Ashall, C. Hoeflich, P. Baron, E. Fox, O. Mera, T. DerKacy, J. Stritzinger, M.D. Shappee, B. Law, D. Morrison, J. Pauly, T. Pierel, J. Medler, K. Andrews, J. Baade, D. Bostroem, A. Brown, P. Burns, C. Burrow, A. Cikota, A. Cross, D. Davis, S. de Jaeger, T. Do, A. Dong, Y. Dominguez, I. Galbany, L. Janzen, D. Jencson, J. Hoang, E. Hsiao, E. Karamehmetoglu, E. Khaghani, B. Krisciunas, K. Kumar, S. Lu, J. Lundquist, M. Maund, J. Mazzali, P. Morrell, N. Patat, F. Pearson, J. Pfeffer, C. Phillips, M. Rest, A. Retamal, N. Stangl, S. Shrestha, M. Stevens, C. Suntzeff, N. Telesco, C. Tucker, M. Wang, L. Yang, Y. Cai, Y.-Z. Camacho-Neves, Y. Elias-Rosa, N. Foley, R. Jha, S. Kwok, L. Larison, C. LeBaron, N. Moran, S. Rho, J. Salmaso, I. Schmidt, J. Tinyanont, S. Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218-2410 United States Department of Physics Virginia Tech BlacksburgVA24061 United States Department of Physics Florida State University 77 Chieftan Way TallahasseeFL32306 United States Planetary Science Institute 1700 East Fort Lowell Road Suite 106 TucsonAZ85719-2395 United States Hamburger Sternwarte Gojenbergsweg 112 HamburgD-21029 Germany Dept of Physics & Astronomy University of Oklahoma 440 W. Brooks Rm 100 NormanOK United States Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Institute for Astronomy University of Hawai’i at Manoa 2680 Woodlawn Dr. Hawai’i HI96822 United States Astrophysics Research Institute Liverpool John Moores University United Kingdom Gemini Observatory NSF’s NOIRLab 670 North A‘ohoku Place HiloHI96720-2700 United States Karl-Schwarzschild-Str. 2 Garching b. München85748 Germany Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721-0065 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Texas A&M University Department of Physics and Astronomy College StationTX77843 United States Observatories of the Carnegie Institution for Science 813 Santa Barbara Street PasadenaCA91101 United States Homer L. Dodge Department of Physics and Astronomy University of Oklahoma 440 W. Brooks Rm 100 NormanOK73019-2061 United States Gemini Observatory NSF’s NOIRLab Casilla 603 La Serena Chile Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain Private Astronomer Laboratoire de Physique Nucléaire et de Hautes Énergies Paris75005 France Department of Physics University of California 1 Shields Avenue DavisCA95616-5270 United States Universidad de Granada Granada18071 Spain BarcelonaE-08034 Spain Department of Physics and Engineering Physics University of Saskatchewan 116 Science Place SaskatoonSKS7N 5E

We present JWST spectral and photometric observations of the Type IIP supernova (SN) 2022acko at ∼50 days past explosions. These data are the first JWST spectral observations of a core-collapse SN. We identify ∼ 30 different H i features, other features associated with products produced from the CNO cycle, and s-process elements such as Sc ii, Ba ii. By combining the JWST spectra with ground-based optical and NIR spectra, we construct a full Spectral Energy Distribution from 0.4 to 25 μm and find that the JWST spectra are fully consistent with the simultaneous JWST photometry. The data lack signatures ofCO formation and we estimate a limit on the CO mass of −8M☉. We demonstrate how the CO fundamental band limits can be used to probe underlying physics during the stellar evolution, explosion, and the environment. The observations indicate little mixing between the H envelope and C/O core in the ejecta and show no evidence for dust. The data presented here set a critical baseline for future JWST observations, where possible molecular and dust formation may be seen. © 2024, CC BY.

关键词： Supernovae

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TESS Asteroseismic Analysis of HD76920: The Giant Star Hosting An Extremely Eccentric Exoplanet

arXiv

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arXiv 2023年

作者： Jiang, Chen Wu, Tao Feinstein, Adina D. Stassun, Keivan G. Bedding, Timothy R. Veras, Dimitri Corsaro, Enrico Buzasi, Derek L. Stello, Dennis Li, Yaguang Mathur, Savita García, Rafael A. Breton, Sylvain N. Lundkvist, Mia S. Mikolajczyk, Przemyslaw J. Gehan, Charlotte Campante, Tiago L. Bossini, Diego Kane, Stephen R. Ong, Jia Mian Joel Yildiz, Mutlu Kayhan, Cenk Orhan, Zeynep Çelik Örtel, Sibel Zhang, Xinyi Cunha, Margarida S. De Moura, Bruno Lustosa Yu, Jie Huber, Daniel Ou, Jian-Wen Wittenmyer, Robert A. Gizon, Laurent Chaplin, William J. Max-Planck-Institut für Sonnensystemforschung Justus-von-Liebig-Weg 3 Göttingen37077 Germany Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China University of Chinese Academy of Sciences Beijing100049 China Institute of Theoretical Physics Shanxi University Taiyuan030006 China Department of Astronomy and Astrophysics University of Chicago 5640 S. Ellis Ave ChicagoIL60637 United States Department of Physics and Astronomy Vanderbilt University NashvilleTN37235 United States School of Physics University of Sydney NSW2006 Australia Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus C8000 Denmark Centre for Exoplanets and Habitability University of Warwick CoventryCV4 7AL United Kingdom Centre for Space Domain Awareness University of Warwick CoventryCV4 7AL United Kingdom Department of Physics University of Warwick CoventryCV4 7AL United Kingdom Inaf - Osservatorio Astrofisico di Catania via S. Sofia 78 Catania95123 Italy Department of Chemistry & Physics Florida Gulf Coast University 10501 FGCU Boulevard S. Fort MyersFL33965 United States School of Physics University of New South Wales NSW2052 Australia Tenerife La LagunaE-38205 Spain Departamento de Astrofísica Tenerife La LagunaE-38206 Spain Université Paris-Saclay Université Paris Cité Cea Cnrs Aim Gif-sur-Yvette91191 France Département d'Astrophysique/aim CEA/IRFU CNRS/INSU Univ. Paris-Saclay Univ. de Paris Gif-sur-Yvette91191 France Astronomical Observatory University of Warsaw Al. Ujazdowskie 4 Warsaw00-478 Poland Astronomical Institute University of Wroclaw Mikolaja Kopernika 11 Wroclaw51-622 Poland Instituto d

The Transiting Exoplanet Survey Satellite (TESS) mission searches for new exoplanets. The observing strategy of TESS results in high-precision photometry of millions of stars across the sky, allowing for detailed asteroseismic studies of individual systems. In this work, we present a detailed asteroseismic analysis of the giant star HD 76920 hosting a highly eccentric giant planet (e = 0.878) with an orbital period of 415 days, using 5 sectors of TESS light curve that cover around 140 days of data. Solar-like oscillations in HD 76920 are detected around 52 μHz by TESS for the first time. By utilizing asteroseismic modeling that takes classical observational parameters and stellar oscillation frequencies as constraints, we determine improved measurements of the stellar mass (1.22 ± 0.11Mo), radius (8.68 ± 0.34 Ro), and age (5.2 ± 1.4 Gyr). With the updated parameters of the host star, we update the semi-major axis and mass of the planet as a = 1.165 ± 0.035 au and Mpsin i = 3.57 ± 0.22 MJup. With an orbital pericenter of 0.142±0.005 au, we confirm that the planet is currently far away enough from the star to experience negligible tidal decay until being engulfed in the stellar envelope. We also confirm that this event will occur within about 100 Myr, depending on the stellar model used. © 2023, CC BY.

关键词： Satellites

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Chromospheric activity on the late-type star V1355 Ori using Lijiang 1.8-m and 2.4-m telescopes

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Research in Astronomy and Astrophysics 2016年第10期16卷 27-34页

作者： Qing-Feng Pi Li-Yun Zhang Liang Chang Xian-Ming Han Hong-Peng Lu Xi-Liang Zhang Dai-Mei Wang College of Physics/Department of Physics and Astronomy Guizhou University Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Mingde College Guizhou University Yunnan Observatories Chinese Academy of Sciences Dept.of Physics and Astronomy Butler University

We obtained new high-resolution spectra using the Lijiang 1.8-m and 2.4-m telescopes to inves- tigate the chromospheric activities of V1355 Ori as indicated in the behaviors of Ca n H＆K, Hγ HT, H/3, Na1 D1, D2, Ha and Ca II infrared triplet （IRT） lines. The observed spectra show obvious emissions above the continuum in Ca II H＆K lines, absorptions in the Hδ, Hγ, H/3 and NaI D1, D2 lines, variable behavior （filled-in absorption, partial emission with a core absorption component or emission above the continuum） in the Ha line, and weak self-reversal emissions in the strong filled-in absorptions of the Ca II IRT lines. We used a spectral subtraction technique to analyze our data. The results show no excess emission in the H6 and H7 lines, very weak excess emissions in the Na I D1, D2 lines, excess emission in the H/3 line, clear excess emission in the Ha line, and excess emissions in the Ca II IRT lines. The value of the ratio of EWs542/EWsa9s is in the range 0.9 to 1.7, which implies that chromospheric activity might have been caused by plage events. The value of the ratio EHδ/EHβ is above 3, indicating that the Balmer lines would arise from prominence-like material. We also found time variations in light curves associated with equiva- lent widths of chromospheric activity lines in the Na I D1, phenomena can be explained by plage events, which are activity indicators. D2, Ca II IRT and Ha lines in particular. These consistent with the behavior of chromospheric

关键词： stars： chromosphere- stars： activity -- stars： individual （V1355 Ori）

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The double-degenerate model for the progenitors of type Ia supernovae

arXiv

引用

arXiv 2017年

作者： Liu, D. Wang, B. Han, Z. Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories CAS Kunming650216 China University of Chinese Academy of Sciences Beijing100049 China Center for Astronomical Mega-Science CAS Beijing100012 China

The double-degenerate (DD) model, involving the merging of massive double carbon-oxygen white dwarfs (CO WDs) driven by gravitational wave radia- tion, is one of the classical pathways for the formation of type Ia supernovae (SNe Ia). Recently, it has been proposed that the WD+He subgiant channel has a significant contribution to the production of massive double WDs, in which the primary WD accumulates mass by accreting He-rich matter from a He subgiant. We evolved about 1800 CO WD+He star systems and ob- tained a large and dense grid for producing SNe Ia through the DD model. We then performed a series of binary population synthesis simulations for the DD model, in which the WD+He subgiant channel is calculated by interpo- lations in this grid. According to our standard model, the Galactic birthrate of SNe Ia is about 2.4 × 10-3yr-1for the WD+He subgiant channel of the DD model;the total birthrate is about 3.7×10-3 yr-1for all channels, repro- ducing that of observations. Previous theoretical models still have deficit with the observed SNe Ia with delay times 8Gyr. After considering the WD+He subgiant channel, we found that the delay time distributions is comparable with the observed results. Additionally, some recent studies pro- posed that the violent WD mergers are more likely to produce SNe Ia based on the DD model. We estimated that the violent mergers through the DD model may only contribute to about 16% of all SNe Ia. Copyright © 2017, The Authors. All rights reserved.

关键词： White dwarfs

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Comprehensive models of novae at metallicity Z = 0.02 and Z = 10−4

arXiv

引用

arXiv 2019年

作者： Chen, Hai-Liang Woods, T.E. Yungelson, L.R. Piersanti, Luciano Gilfanov, M. Han, Zhanwen Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Max Planck Institute for Astrophysics Karl-Schwarzschild-Str. 1 Garching b. München85741 Germany Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Science Beijing100012 China Institute of Gravitational Wave Astronomy School of Physics and Astronomy University of Birmingham Edgbaston BirminghamB15 2TT United Kingdom Institute of Astronomy RAS 48 Pyatnitskaya Str. Moscow119017 Russia Space Research Institute of Russian Academy of Sciences Profsoyuznaya 84/32 Moscow117997 Russia INAF – Osservatorio Astronomico d’Abruzzo via Mentore Maggini snc TeramoI-64100 Italy INFN – Sezione di Perugia via Pascoli Perugia Italy Kazan Federal University Kremlevskaya str. 18 Kazan420008 Russia

Novae are the observational manifestations of thermonuclear runaways on the surface of accreting white dwarfs (WDs). Although novae are an ubiquitous phenomenon, their properties at low metallicity are not well understood. Using the publicly-available stellar evolution code Modules for Experiments in Stellar Astrophysics (MESA), we model the evolution of accreting carbon-oxygen WDs and consider models which accrete matter with metallicity Z=0.02 or 10−4. We consider both models without mixing and with matter enriched by CO-elements assuming that mixing occurs in the process of accretion (with mixing fraction 0.25). We present and contrast ignition mass, ejected mass, recurrence period and maximum luminosity of novae for different WD masses and accretion rates for these metallicities and mixing cases. We find that models with Z = 0.02 have ignition masses and recurrence periods smaller than models with low Z, while the ejected mass and maximum luminosity are larger. Retention efficiency during novae outbursts decreases with increasing metallicity. In our implementation, inclusion of mixing at the H/He interface reduces accreted mass, ejected mass and recurrence period as compared to the no-mixing case, while the maximum luminosity becomes larger. Retention efficiency is significantly reduced, becoming negative in most of our models. For ease of use, we provide a tabular summary of our results. Copyright © 2019, The Authors. All rights reserved.

关键词： Astrophysics

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Interstellar Scintillation observations for PSR B0355+54

arXiv

引用

arXiv 2018年

作者： Xu, Y.H. Lee, K.J. Hao, L.F. Wang, H.G. Liu, Z.Y. Yue, Y.L. Yuan, J.P. Li, Z.X. Wang, M. Dong, J. Tan, J.J. Chen, W. Bai, J.M. Yunnan Astronomical Observatory Chinese Academy of Sciences Kunming650011 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China University of Chinese Academy of Sciences Beijing100049 China Center for Astrophysics Guangzhou University Guangzhou510006 China Key Laboratory for Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Xinjiang Astronomical Observatory Chinese Academy of Sciences 150 Science 1-street Urumqi Xinjiang830011 China National Astronomical Observatories Chinese Academy of Sciences Beijing China

In this paper, we report our investigation of pulsar scintillation phenomena by monitor- ing PSR B0355+54 at 2.25 GHz for three successive months using Kunming 40-m radio telescope. We have measured the dynamic spectrum, the two-dimensional correlation function, and the secondary spectrum. In those observations with high signal-to-noise ratio (S/N ≥ 100), we have detected the scintillation arcs, which are rarely observable using such a small telescope. The sub-microsecond scale width of the scintillation arc indicates that the transverse scale of structures on scattering screen is as compact as AU size. Our monitoring has also shown that both the scintillation bandwidth, timescale, and arc curvature of PSR B0355+54 were varying temporally. The plausi- ble explanation would need to invoke multiple-scattering-screen or multiple-scattering- structure scenario that different screens or ray paths dominate the scintillation process at different epochs. Copyright © 2018, The Authors. All rights reserved.

关键词： Scintillation

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Observations of a fast-expanding and uv-bright type ia supernova SN 2013gs

arXiv

引用

arXiv 2019年

作者： Zhang, Tianmeng Wang, Xiaofeng Zhao, Xulin Xu, Dong Reguitti, Andrea Zhang, Jujia Pastorello, Andrea Tomasella, Lina Ochner, Paolo Tartaglia, Leonardo Benetti, Stefano Turatto, Massimo Harutyunyan, Avet Elias-Rosa, Nancy Huang, Fang Zhang, Kaicheng Chen, Juncheng Jiang, Zhaoji Ma, Jun Nie, Jundan Peng, Xiyan Zhou, Xu Zhou, Zhimin Zou, Hu Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China School of Astronomy and Space Science University of Chinese Academy of Sciences Tsinghua University Beijing100084 China School of Science Tianjin University of Technology Tianjin300384 China National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China Dipartimento di Fisica e Astronomia G. Galilei Universita’ di Padova Vicolo dell’Osservaotio 3 Padova35122 Italy 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 INAF-Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 Padova35122 Italy Department of Astronomy Stockholm University StockholmSE 10691 Sweden INAF-Fundacion Galileo Galilei Rambla Jose Ana Fernandez Perez 7 Brena BajaE-38712 Spain Department of Astronomy School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China

In this paper, we present extensive optical and ultraviolet (UV) observations of the type Ia supernova (SN Ia) 2013gs discovered during the Tsinghua-NAOC Transient Survey. The photometric observations in the optical show that the light curves of SN 2013gs is similar to that of normal SNe Ia, with an absolute peak magnitude of MB = −19.25 ± 0.15 mag and a post-maximum decline rate ∆m15(B) = 1.00 ± 0.05 mag. Gehrels Swift UVOT observations indicate that SN 2013gs shows unusually strong UV emission (especially in the uvw1 band) at around the maximum light (Muvw1 ∼ −18.9 mag). The SN is characterized by relatively weak Fe ii iii absorptions at ∼ 5000Å in the early spectra and a larger expansion velocity (vSi ∼ 13,000 km s−1 around the maximum light) than the normal-velocity SNe Ia. We discuss the relation between the uvw1−v color and some observables, including Si ii velocity, line strength of Si ii λ6355, Fe ii/iii lines and ∆m15(B). Compared to other fast-expanding SNe Ia, SN 2013gs exhibits Si and Fe absorption lines with similar strength and bluer uvw1 − v color. We briefly discussed the origin of the observed UV dispersion of SNe Ia. Copyright © 2019, The Authors. All rights reserved.

关键词： Supernovae

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