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arXiv 2018年

作者： He, Jia-Jia Qian, Sheng-Bang Soonthornthum, B. Aungwerojwit, A. Liu, Niang-Ping Sarotsakulchai, T. P. O. Box 110 Kunming650216 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P. O. Box 110 Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China University of Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China National Astronomical Research Institute of Thailand 191 Siriphanich Bidg. 2nd Fl. Huay Kaew Rd. Suthep District Muang Chiang Mai50200 Thailand Department of Physics Faculty of Science Naresuan University Phitsanulok65000 Thailand

Four-color charge-coupled device (CCD) light curves in B, V, Rc and Ic bands of the total-eclipsing binary system, V1853 Ori, are presented. By comparing our light curves with those published by previous investigators, it is detected that the O’Connell effect on the light curves is 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 new determined times of light minima together with the others published in the literature, the period changes of the system is investigated. We found that the general trend of the observed-calculated (O − C) curve shows a downward parabolic variation that corresponds to a long-term decrease in the orbital period with a rate of dP/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 the Gaia DR 2 data, absolute parameters were derived as M1 = 1.20 M☉, M2 = 0.23 M☉, R1 = 1.36 R☉, and R2 = 0.66 R☉. The long-term period decrease and the intermediate-contact configuration suggest that V1853 Ori will evolve into a high fill-out overcontact binary. Copyright © 2018, The Authors. All rights reserved.

关键词： Photometry

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Contribution of primordial binary evolution to the two blue-straggler sequences in globular cluster M30

arXiv

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arXiv 2017年

作者： Jiang, Dengkai Chen, Xuefei Li, Lifang Han, Zhanwen Yunnan Observatories 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 Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China

Two blue-straggler sequences discovered in globular cluster M30 provide a strong constraint on the formation mechanisms of blue stragglers. We study the formation of the blue-straggler binaries through binary evolution, and find that binary evolution can contribute to the blue stragglers in both of the sequences. Whether a blue straggler is located in the blue sequence or red sequence depends on the contribution of the mass donor to the total luminosity of the binary, which is generally observed as a single star in globular clusters. The blue stragglers in the blue sequence have a cool white-dwarf companion, while the majority (∼ 60%) of the objects in the red sequence are the binaries that are still experiencing mass transfer, but there are also some objects that the donors have just finished the mass transfer (the stripped-core stars, ∼ 10%) or the blue stragglers (the accretors) have evolved away from the blue sequence (∼ 30%). Meanwhile, W UMa contact binaries found in both sequences may be explained by various mass ratios, that is, W UMa contact binaries in the red sequence have two components with comparable masses (e.g. mass ratio q ∼ 0.3-1.0), while those in the blue sequence have low mass ratio (e.g. q Copyright © 2017, The Authors. All rights reserved.

关键词： Mass transfer

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Mass retention efficiencies of He accretion onto carbon-oxygen white dwarfs and type Ia supernovae

arXiv

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arXiv 2017年

作者： Wu, C. Wang, B. Liu, D. Han, Z. 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 Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China

Context. Type Ia supernovae (SNe Ia) play a crucial role in studying cosmology and galactic chemical evolution. They are thought to be thermonuclear explosions of carbon-oxygen white dwarfs (CO WDs) when their masses reach the Chandrasekar mass limit in binaries. Previous studies have suggested that He novae may be progenitor candidates of SNe Ia. However, the mass retention efficiencies during He nova outbursts are still uncertain. Aims. In this article, we aim to study the mass retention efficiencies of He nova outbursts and to investigate whether SNe Ia can be produced through He nova outbursts. Methods. Using the stellar evolution code Modules for Experiments in Stellar Astrophysics, we simulated a series of multicycle He-layer flashes, in which the initial WD masses range from 0.7 to 1.35 M☉ with various accretion rates. Results. We obtained the mass retention efficiencies of He nova outbursts for various initial WD masses, which can be used in the binary population synthesis studies. In our simulations, He nova outbursts can increase the mass of the WD to the Chandrasekar mass limit and the explosive carbon burning can be triggered in the center of the WD;this suggests that He nova outbursts can produce SNe Ia. Meanwhile, the mass retention efficiencies in the present work are lower than those of previous studies, which leads to a lower birthrates of SNe Ia through the WD + He star channel. Furthermore, we obtained the elemental abundances distribution at the moment of explosive carbon burning, which can be used as the initial input parameters in studying explosion models of SNe Ia. Copyright © 2017, The Authors. All rights reserved.

关键词： White dwarfs

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The orbital period variations of AH Virginis

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Research in Astronomy and Astrophysics 2015年第2期15卷 275-280页

作者： Ming Chen Fu-Yuan Xiang Yun-Xia Yu Ting-Yu Xiao Department of Physics Xiangtan University Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences

Abstract We present a study of orbital period changes in AH Virginis. We perform a careful literature search for all available minima times, from which we derived a new linear ephemeris and constructed an O - C curve. We found that the orbital period of AH Virginis shows a long-term increase, dP/dt = （2.1869 ± 0.0161） × 10^-7 d yr^-1, and a small periodic variation with a period of 37.19 yr. Since AH Virginis is an over- contact system and the primary component shows strong Ha and Mg II emission lines, we discuss the possible connection between mass transfer, magnetic activity and or- bital period changes.

关键词： binaries: close binaries: eclipsing stars: individual (AH Virginis)

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Analytic properties of force-free jets in the kerr spacetime - III: Uniform field solution

arXiv

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arXiv 2017年

作者： Pan, Zhen Yu, Cong Huang, Lei Department of Physics University of California One Shields Avenue DavisCA95616 United States Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China

The structure of steady axisymmetric force-free magnetosphere of a Kerr black hole (BH) is governed by a second-order partial differential equation of Aφ depending on two "free" functions Ω(Aφ) and I(Aφ), where Aφ is the φ component of the vector potential of the electromagnetic field, Ω is the angular velocity of the magnetic field lines and I is the poloidal electric current. In this paper, we investigate the solution uniqueness. Taking asymptotically uniform field as an example, analytic studies imply that there are infinitely many solutions approaching uniform field at infinity, while only a unique one is found in general relativistic magnetohydrodynamic simulations. To settle down the disagreement, we reinvestigate the structure of the governing equation and numerically solve it with given constraint condition and boundary condition. We find that the constraint condition (field lines smoothly crossing the light surface (LS)) and boundary conditions at horizon and at infinity are connected via radiation conditions at horizon and at infinity, rather than being independent. With appropriate constraint condition and boundary condition, we numerically solve the governing equation and find a unique solution. Contrary to naive expectation, our numerical solution yields a discontinuity in the angular velocity of the field lines and a current sheet along the last field line crossing the event horizon. We also briefly discuss the applicability of the perturbation approach to solving the governing equation. Copyright © 2017, The Authors. All rights reserved.

关键词： Magnetohydrodynamics

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Constraining the redshifts of TeV BL Lac objects

arXiv

引用

arXiv 2017年

作者： Qin, Longhua Jiancheng, Wang Dahai, Yan Yang, Chuyuan Zunli, Yuan Zhou, Ming Yunnan Observatory Chinese Academy of Sciences Kunming Yunnan Province650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming China University of Chinese Academy of Sciences Beijing China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China

We present a model-dependent method to estimate the redshifts of three TeV BL Lac objects (BL Lacs) through fitting their (quasi-) simultaneous multi-waveband spectral energy distributions (SEDs) by one-zone leptonic synchrotron self-Compton (SSC) model. Considering the impact of electron energy distributions (EEDs) on the results, we use three types of EEDs, such as the power-law EED with exponential cut-off (PLC), the log-parabola (PLLP) and the broken power-law (BPL) EEDs, to fit the SEDs. We also use a parameter α to describe the uncertainties of the extragalactic background light (EBL) models, as in (Abdo et al. 2010b). We then use Markov Chain Monte Carlo (MCMC) method to explore multi-dimensional parameter space and obtain the uncertainties of the model parameters based on the observational data. We apply our method to obtain the redshifts of three TeV BL Lac objects in the marginalized 68% confidence, and find that the PLC EED does not fit the SEDs. For 3C66A, the redshift is 0.14 - 0.31 and 0.16 - 0.32 in the BPL and PLLP EEDs;for PKS1424+240, the redshift is 0.55 - 0.68 and 0.55 - 0.67 in the BPL and PLLP EEDs;for PG1553+113, the redshift is 0.22 - 0.48 and 0.22 - 0.39 in the BPL and PLLP EEDs. We also estimate the redshift of PKS1424+240 in the high stage to be 0.46 - 0.67 in the PLLP EED, roughly consistent with that in the low stage. Copyright © 2017, The Authors. All rights reserved.

关键词： Markov processes

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The broad-lined Type-Ic supernova SN 2022xxf with extraordinary two-humped light curves

arXiv

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arXiv 2023年

作者： Kuncarayakti, H. Sollerman, J. Izzo, L. Maeda, K. Yang, S. Schulze, S. Angus, C.R. Aubert, M. Auchettl, K. Della Valle, M. Dessart, L. Hinds, K. Kankare, E. Kawabata, M. Lundqvist, P. Nakaoka, T. Perley, D. Raimundo, S.I. Strotjohann, N.L. Taguchi, K. Cai, Y.-Z. Charalampopoulos, P. Fang, Q. Fraser, M. Gutiérrez, C.P. Imazawa, R. Kangas, T. Kawabata, K.S. Kotak, R. Kravtsov, T. Matilainen, K. Mattila, S. Moran, S. Murata, I. Salmaso, I. Anderson, J.P. Ashall, C. Bellm, E.C. Benetti, S. Chambers, K.C. Chen, T.-W. Coughlin, M. De Colle, F. Fremling, C. Galbany, L. Gal-Yam, A. Gromadzki, M. Groom, S.L. Hajela, A. Inserra, C. Kasliwal, M.M. Mahabal, A.A. Martin-Carrillo, A. Moore, T. Müller-Bravo, T.E. Nicholl, M. Ragosta, F. Riddle, R.L. Sharma, Y. Srivastav, S. Stritzinger, M.D. Wold, A. Young, D.R. Tuorla Observatory Department of Physics and Astronomy University of Turku FI-20014 Finland University of Turku FI-20014 Finland Department of Astronomy Oskar Klein Centre AlbaNova Stockholm10691 Sweden DARK Niels Bohr Institute University of Copenhagen Copenhagen Denmark Department of Astronomy Kyoto University Kitashirakawa-Oiwake-cho Sakyo-ku Kyoto606-8502 Japan Henan Academy of Sciences Henan Zhengzhou450046 China The Oskar Klein Centre Department of Physics Stockholm University AlbaNova University Center StockholmSE 106 91 Sweden Université Clermont Auvergne CNRS IN2P3 LPC Clermont-Ferrand France School of Physics The University of Melbourne ParkvilleVIC3010 Australia Sydney2006 Australia Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Capodimonte Astronomical Observatory INAF-Napoli Salita Moiariello 16 NapoliI-80131 Italy Institut d’Astrophysique de Paris CNRS-Sorbonne Université 98 bis boulevard Arago ParisF-75014 France Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Turku Collegium for Science Medicine and Technology University of Turku TurkuFI-20014 Finland Hiroshima Astrophysical Science Center Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan Department of Physics and Astronomy University of California Los AngelesCA United States Department of Physics & Astronomy University of Southampton Southampton United Kingdom Benoziyo Center for Astrophysics The Weizmann Institute of Science Rehovot76100 Israel Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China School of Physics O’Brien Centre for Science North University College Dublin Belfield Dublin 4 Dublin Ireland Department of Physics Graduate School

We report on our study of supernova (SN) 2022xxf based on observations obtained during the first four months of its evolution. The light curves (LCs) display two humps of similar maximum brightness separated by 75 days, unprecedented for a broad-lined (BL) Type Ic supernova (SN IcBL). SN 2022xxf is the most nearby SN IcBL to date (in NGC 3705, z = 0.0037, at a distance of about 20 Mpc). Optical and near-infrared photometry and spectroscopy are used to identify the energy source powering the LC. Nearly 50 epochs of high signal-to-noise-ratio spectroscopy were obtained within 130 days, comprising an unparalleled dataset for a SN IcBL, and one of the best-sampled SN datasets to date. The global spectral appearance and evolution of SN 2022xxf points to typical SN Ic/IcBL, with broad features (up to ∼ 14000 km s−1) and a gradual transition from the photospheric to the nebular phase. However, narrow emission lines (corresponding to ∼ 1000−2500 km s−1) are present in the spectra from the time of the second rise, suggesting slower-moving circumstellar material (CSM). These lines are subtle, in comparison to the typical strong narrow lines of CSM-interacting SNe, for example, Type IIn, Ibn, and Icn, but some are readily noticeable at late times such as in Mg I λ5170 and [O I] λ5577. Unusually, the near-infrared spectra show narrow line peaks in a number of features formed by ions of O and Mg. We infer the presence of CSM that is free of H and He. We propose that the radiative energy from the ejecta-CSM interaction is a plausible explanation for the second LC hump. This interaction scenario is supported by the color evolution, which progresses to the blue as the light curve evolves along the second hump, and the slow second rise and subsequent rapid LC drop. SN 2022xxf may be related to an emerging number of CSM-interacting SNe Ic, which show slow, peculiar LCs, blue colors, and subtle CSM interaction lines. The progenitor stars of these SNe likely experienced an episode of m

关键词： Supernovae

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The YNEV stellar evolution and oscillation code

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Research in Astronomy and Astrophysics 2015年第4期15卷 549-568页

作者： Qian-Sheng Zhang Yunnan Observatories Chinese Academy of Sciences Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences

We have developed a new stellar evolution and oscillation code YNEV, which calculates the structures and evolutions of stars, taking into account hydrogen and helium burning. A nonlocal turbulent convection theory and an updated over- shoot mixing model are optional in this code. The YNEV code can evolve low- and intermediate-mass stars from the pre-main sequence to a thermally pulsing asymptotic branch giant or white dwarf. The YNEV oscillation code calculates the eigenfrequen- cies and eigenfunctions of the adiabatic oscillations for a given stellar structure. The input physics and numerical scheme adopted in the code are introduced. Examples of solar models, stellar evolutionary tracks of low- and intermediate-mass stars with different convection theories （i.e. mixing-length theory and nonlocal turbulent con- vection theory）, and stellar oscillations are shown.

关键词： stars -- stellar structure -- stellar evolution -- stellar oscillations

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Forbidden hugs in pandemic times: IV. Panchromatic evolution of three luminous red novae

引用

Astronomy and Astrophysics 2023年 671卷

作者： Pastorello, A. Valerin, G. Fraser, M. Reguitti, A. Elias-Rosa, N. Filippenko, A.V. Rojas-Bravo, C. Tartaglia, L. Reynolds, T.M. Valenti, S. Andrews, J.E. Ashall, C. Bostroem, K.A. Brink, T.G. Burke, J. Cai, Y.-Z. Cappellaro, E. Coulter, D.A. Dastidar, R. Davis, K.W. Dimitriadis, G. Fiore, A. Foley, R.J. Fugazza, D. Galbany, L. Gangopadhyay, A. Geier, S. Gutiérrez, C.P. Haislip, J. Hiramatsu, D. Holmbo, S. Howell, D.A. Hsiao, E.Y. Hung, T. Jha, S.W. Kankare, E. Karamehmetoglu, E. Kilpatrick, C.D. Kotak, R. Kouprianov, V. Kravtsov, T. Kumar, S. Li, Z.-T. Lundquist, M.J. Lundqvist, P. Matilainen, K. Mazzali, P.A. McCully, C. Misra, K. Morales-Garoffolo, A. Moran, S. Morrell, N. Newsome, M. Padilla Gonzalez, E. Pan, Y.-C. Pellegrino, C. Phillips, M.M. Pignata, G. Piro, A.L. Reichart, D.E. Rest, A. Salmaso, I. Sand, D.J. Siebert, M.R. Smartt, S.J. Smith, K.W. Srivastav, S. Stritzinger, M.D. Taggart, K. Tinyanont, S. Yan, S.-Y. Wang, L. Wang, X.-F. Williams, S.C. Wyatt, S. Zhang, T.-M. De Boer, T. Chambers, K. Gao, H. Magnier, E. INAF Osservatorio Astronomico di Padova Vicolo dell Osservatorio 5 Padova35122 Italy Universitá Degli Studi di Padova Dipartimento di Fisica e Astronomia Vicolo dell Osservatorio 2 Padova35122 Italy School of Physics O Brien Centre for Science North University College Dublin Dublin 4 Belfield Ireland Instituto de Astrofísica Facultad de Ciencias Exactas Universidad Andres Bello Fernández Concha 700 Las Condes Santiago Chile Nuncio Monsenor Sótero Sanz 100 Santiago Providencia8320000 Chile CSIC Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Department of Astronomy University of California BerkeleyCA94720-3411 United States Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Tuorla Observatory Department of Physics and Astronomy University of Turku Turku20014 Finland Niels Bohr Institute University of Copenhagen Jagtvej 128 København N2200 Denmark Department of Physics and Astronomy University of California Davis 1 Shields Avenue DavisCA95616-5270 United States Gemini Observatory 670 North A ohoku Place HiloHI96720-2700 United States Department of Physics Virginia Tech 850 West Campus Drive BlacksburgVA24061 United States DIRAC Institute Department of Astronomy University of Washington 3910 15th Avenue NE SeattleWA98195-0002 United States Las Cumbres Observatory 6740 Cortona Dr. Suite 102 GoletaCA93117 United States Department of Physics University of California Santa BarbaraCA93106 United States Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Tsinghua University Beijing100084 China School of Physics Trinity College Dublin University of Dublin Dublin Ireland Fondazione Bruno Kessler Trento38123 Italy INFN-TI

We present photometric and spectroscopic data on three extragalactic luminous red novae (LRNe): AT 2018bwo, AT 2021afy, and AT 2021blu. AT 2018bwo was discovered in NGC 45 (at about 6.8 Mpc) a few weeks after the outburst onset. During the monitoring period, the transient reached a peak luminosity of 1040 erg s1. AT 2021afy, hosted by UGC 10043 (49.2 Mpc), showed a double-peaked light curve, with the two peaks reaching a similar luminosity of 2.1(±0.6) - 1041 erg s1. Finally, for AT 2021blu in UGC 5829 (∼8.6 Mpc), the pre-outburst phase was well-monitored by several photometric surveys, and the object showed a slow luminosity rise before the outburst. The light curve of AT 2021blu was sampled with an unprecedented cadence until the object disappeared behind the Sun, and it was then recovered at late phases. The light curve of LRN AT 2021blu shows a double peak, with a prominent early maximum reaching a luminosity of 6.5 - 1040 erg s1, which is half of that of AT 2021afy. The spectra of AT 2021afy and AT 2021blu display the expected evolution for LRNe: a blue continuum dominated by prominent Balmer lines in emission during the first peak, and a redder continuum consistent with that of a K-type star with narrow absorption metal lines during the second, broad maximum. The spectra of AT 2018bwo are markedly different, with a very red continuum dominated by broad molecular features in absorption. As these spectra closely resemble those of LRNe after the second peak, AT 2018bwo was probably discovered at the very late evolutionary stages. This would explain its fast evolution and the spectral properties compatible with that of an M-type star. From the analysis of deep frames of the LRN sites years before the outburst, and considerations of the light curves, the quiescent progenitor systems of the three LRNe were likely massive, with primaries ranging from about 13 M for AT 2018bwo, to 141+4 Mo for AT 2021blu, and over 40 M for AT 2021afy. © 2023 The Authors.

关键词： Luminance

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The rate of period change in DAV stars

arXiv

引用

arXiv 2017年

作者： Chen, Y.H. Ding, C.Y. Na, W.W. Shu, H. Institute of Astrophysics Chuxiong Normal University Chuxiong675000 China School of Physics and Electronical Science Chuxiong Normal University Chuxiong675000 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P.O. Box 110 Kunming650011 China School of Physics and Electronic Engineering Yuxi Normal University Yuxi653100 China

Grids of DAV star models are evolved by WDEC, taking the element diffusion effect into account. The grid parameters are hydrogen mass log(MH/M*), helium mass log(MH/M*), stellar mass M., and effective temperature Teff for DAV stars. The core compositions are from white dwarf models evolved by MESA. Therefore, those DAV star models evolved by WDEC have historically viable core compositions. Based on those DAV star models, we studied the rate of period change (P(k)) for different values of H, He, M., and Teff. The results are consistent with previous work. Two DAV stars G117-B15A and R548 have been observed around forty years. The rates of period change of two largeamplitude modes were obtained through O-C method. We did asteroseismological study on the two DAV stars and then obtained a best-fittingmodel for each star. Based on the two best-fitting models, the mode identifications (l, k) of the observed modes for G117-B15A and R548 are consistent with previous work. Both the observed modes and the observed Ps can be fitted by calculated ones. The results indicate that our method of evolving DAV star models is feasible. Copyright © 2017, The Authors. All rights reserved.

关键词： White dwarfs

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