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Studies on the Equatorial Spot of G-type Contact Binary UV Lyn

Research in Astronomy and Astrophysics 2022年第2期22卷 53-61页

作者： Jing-Jing Wang Bin Zhang lin-qiao jiang China University of Petroleum–Beijing at Karamay Anding Road 355834000 KaramayChina School of Physics and Electronic Science Guizhou Normal University550025 GuiyangChina School of Physics and Electronic Engineering Sichuan University of Science Engineering643000 ZigongChina

New CCD photometric observations of G-type contact binary UV Lyn were obtained in 2006 and 2020,when the light curves(LCs)showed positive O'Connell effect and negative O'Connell effect,*** the previous studies,the LCs by other ground-based telescope are variable from 1973 to 2020,particularly the magnitude difference between the two *** phenomena indicate that the component has been active in the past 47 *** addition,during monitoring by the space telescope Transiting Exoplanet Survey Satellite(TESS)from January to March 2020,we fortunately found continuous variations from the O'Connell effect in every cycle for the first *** analysis also shows that in a short time,the positive O'Connell effect has been transformed into the negative one,which demonstrates that there are stronger magnetic activities on the surface of the *** using the Wilson-Devinney code with a spot model,these photometric solutions confirm UV Lyn is a shallow W-subtype contact binary with a cool equatorial spot on the less massive *** successive variability of the O'Connell effect possibly results from one equatorial cool spot shifting gradually along with *** also investigated its O-C curve from these continuous LCs,and there is no apparent variation in such a short ***,regarding the O'Connell effect as the indicator of magnetic activity indicates the system is possibly undergoing a periodic trend with a period of nearly 38 *** with the trend of the O-C curve,we could not find any relation between the period variation and magnetic activity.

关键词： (stars:)binaries(including multiple):close stars:solar-type stars:magnetic field

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On properties of mass transfer in an Algol-type binary system:an example of VV Vir

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Research in Astronomy and Astrophysics 2014年第2期14卷 179-192页

作者： Jia Zhang Sheng-Bang Qian lin-qiao jiang Yunnan Observatories Chinese Academy of Sciences Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences University of Chinese Academy of Sciences

Some properties of mass transfer within a semi-detached binary system are discussed based on an example of VV Vir. The observations and analysis of VV Vir show that it is a semi-detached binary system with the less massive cooler component filling its Roche lobe, which is also called an Algol-type binary system. Based on the parameters of this semi-detached binary, a theoretical study on the mass flow is carded out, including the trajectory of the mass flow, the position, radius and temperature of the impact spot caused by the mass flow, the inconsistent form of the mass flow and the possibly huge rate of energy transfer carried by the mass flow. Humps and distortions in light curves of VV Vir are deemed to be weak evidence for the theoretical results.

关键词： binaries eclipsing -- stars individual (VV Vir) -- techniques photo-metric

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SDSS J012119.10 001949.9:a very short period M dwarf contact binary from SDSS stripe 82

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Research in Astronomy and Astrophysics 2015年第12期15卷 2237-2243页

作者： lin-qiao jiang Sheng-Bang Qian Jia Zhang Yunnan Observatories Chinese Academy of Sciences Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences University of Chinese Academy of Sciences

We present the first multicolor photometric observations of the short period low-mass eclipsing binary SDSS J012119.10-4301949.9. By using the 2013 version of the Wilson-Devinney code, the photometric solutions are derived. It is found that the system is in a contact configuration （f = 18.9± 6.0%） with a moderate mass ratio of 0.5 ± 0.01. A third light contributing about 6.1± 1.3% of the total luminosity in the V band was found, which may come from a cool tertiary component. The derived high orbital inclination （i - 83.9°± 0.5°） and the almost symmetric three light curves suggest that the determined parameters are reliable. Both the color class and spectral class of the system correspond to a spectral type of M0, which may indicate that SDSS J012119.10-001949.9 belongs to a very rare class of M dwarf contact binaries that are below the theoretical short period limit.

关键词： binaries: eclipsing -- stars: individual (SDSS J012119.10-001949.9) --techniques: photometric

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New Photometric Investigations of G-type Contact Binary TU Boo

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Research in Astronomy and Astrophysics 2023年第4期23卷 103-109页

作者： Jing-jing Wang Meng Guo lin-qiao jiang Bin Zhang China University of Petroleum–Beijing at Karamay Karamay 834000China College of Mathematics and Physics Leshan Normal UniversityLeshan 614000China School of Physics and Electronic Science Guizhou Normal UniversityGuiyang 550025China

Two sets of CCD photometric observations for contact binary TU Boo were obtained in 2020 and *** from its asymmetric light curves published from the literature,our BVRcIc-band curves show that the heights of maximum are almost *** distortions of light curves possibly indicate that the components were active in past 25 yr,but they were stable in the last two *** total-eclipse binary TU Boo,due to some star-spots on the surface of the components,the physical structure obtained by many investigators are ***,the symmetric multi-color light curves in 2020,2021 are important for understanding configuration and evolution of this *** using the Wilson–Devinney program,it is confirmed that TU Boo is an A-type shallow-contact binary with the temperature difference ofΔT=152 K and fill-out of f=14.67%.In the O−C diagram of orbital period analysis,a cyclic oscillation superimposed on a continuous decrease was *** long-term decreasing is often explained by the mass transfer from the more massive star to less massive one,this system will evolve into a deeper contact binary with *** cyclic oscillations computed from much more CCD times of light minimum maybe result from the light-travel time effect via the presence of a third *** characters of structure,evolution and ternary belong to typical A-type W UMa binaries with spectral G.

关键词： (stars:)binaries eclipsing-stars solar-type-stars individual(TU Boo)

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Multi-color light curves and orbital period research of eclipsing binary V1073 Cyg

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Research in Astronomy and Astrophysics 2018年第2期18卷 83-92页

作者： Xiao-Man Tian Li-Ying Zhu Sheng-Bang Qian lin-Jia Li lin-qiao jiang 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 University of Chinese Academy of Sciences Beijing 100049 China School of Physics and Electronic Engineering Sichuan University of Science & Engineering Zigong 643000 China

New multi-color BVRcIc photometric observations are presented for the W UMa type eclips- ing binary V1073 Cyg. The multi-color light curve analysis with the Wilson-Devinney procedure yielded the absolute parameters of this system, showing that V 1073 Cyg is a shallow contact binary system with a fill-out factor f = 0.124（±0.011）. We collected all available times of light minima spanning 119yr, including CCD data to construct the O - C curve, and performed detailed O - C analysis. The O - C diagram shows that the period change is complex. A long-term continuous decrease and a cyclic vari- ation exist. The period is decreasing at a rate ofP = -1.04（±0.18） × 10-10 d cycle-land, with the period decrease, V1073 Cyg will evolve to the deep contact stage. The cyclic variation with a period of P3 = 82.7（±3.6） yr and an amplitude of A = 0.028（±0.002） d may be explained by magnetic activ- ity of one or both components or the light travel time effect caused by a distant third companion with M3（i1 = 90°） = 0.511 M⊙.

关键词： stars: binaries: close -- stars: binaries: eclipse -- stars: binaries: individual (V1073 Cyg)

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A photometric-spectroscopic study of the infrared-excess eclipsing binary V2364 Cyg

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Research in Astronomy and Astrophysics 2020年第12期20卷 307-316页

作者： Hui-Yu Yuan lin-qiao jiang Hai-Feng Dai Shuang Wang Yuan-Gui Yang Information College&School of Physics and Electronic Information Huaibei Normal UniversityHuaibei 235000China Artificial Intelligence Key Laboratory of Sichuan Province Sichuan University of Science&EngineeringZigong 643000China

The eclipsing binary V2364 Cyg is an A7 V-type contact binary with a period of 0.5921 *** present six spectra from LAMOST and BVRc light curves(LCs),which are simultaneously analyzed to obtain the absolute physical *** first light maxima are brighter than the second ones by up to 0.m038,0.m036 and 0.m024 for BVRc bands,*** distorted LCs are modeled by a cool spot on the less massive *** mass ratio and over-contact degree are q=0.319(±0.004) and f=28.4%(±1.0) % *** the mass-luminosity diagram,the primary component is a normal main-sequence star,while the secondary one is a subgiant *** the(O-C) curve,the orbital period secularly decreases at a rate dP/dt=-1.62(±0.03) × 10^-7 dyr^-1,which is mainly attributed to mass loss via stellar wind from the binary *** may result in the observed infrared excess in the W4 band.

关键词： stars:circumstellar matter stars:binaries:close stars:individual(V2364 Cyg) mass loss infrared excess

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The first photometric investigation of the contact binary OQ Cam

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Research in Astronomy and Astrophysics 2020年第11期20卷 252-258页

作者： Ya-Ni Guo Kai Li Qi-Qi Xia Xing Gao lin-qiao jiang Yuan Liu Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment School of Space Science and PhysicsInstitute of Space SciencesShandong UniversityWeihai 264209China Xinjiang Astronomical Observatory Urumqi 830011China Artificial Intelligence Key Laboratory of Sichuan Province Sichuan University of Science&EngineeringZigong 643000China Qilu Institute of Technology Jinan 250200China

The first charge-coupled device photometric light curves in B,V,Rc,and Ic bands of the short-period contact binary star OQ Cam are *** analyzing the light curves with the WilsonDevinney code,it is found that OQ Cam is a W-type shallow contact binary star with a contact degree of f=20.2%.Based on the O-C analyzing,the orbit period displays a long term increasing with a rate of d P/dt=4.40×10^-7 d *** increasing in orbit period can be interpreted by mass transfer from the less massive component to the more massive *** the orbit period increases,OQ Cam would evolve from the present shallow contact configuration to a non-contact *** it may be a potential candidate to confirm the thermal relaxation oscillation theory.

关键词： stars binaries close stars binaries eclipsing stars evolution stars individual(OQ Cam)

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V0405 Dra:A New Deep and Low Mass Ratio Contact Binary with Extremely Fast Decrease in the Orbital Period

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Research in Astronomy and Astrophysics 2024年第6期24卷 287-293页

作者： Chao-Yue Li lin-qiao jiang Jie Zheng Yi-Man Liu Xiao-Yu Long Min Sun Han-Lu Zhang Xiao-Man Tian School of Science Leshan Normal UniversityLeshan 614000China Center for Applied Optics Research Leshan Normal UniversityLeshan 614000China Key Laboratory of Detection and Application of Space Effect in Southwest Sichuan Leshan 614000China CAS Key Laboratory of Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China School of Aeronautics Shandong Jiaotong UniversityJinan 250000China

V0405 Dra is a W UMa-type binary *** on the TESS data,we have conducted an orbital period study and performed a light curve analysis for the *** orbital period study reveals that the O-C curve for V0405 Dra exhibits secular decrease at an extremely high rate of d P/dt=-2.71×10^(-6)day year^(-1),along with periodic variations characterized by an amplitude of A_(3)=0.0032 day and a period of P_(3)=1.413 *** orbital periodic change is possibly due to the light-travel time effect resulting from an additional third body in the system,for which we estimate a minimum mass of M_(3)=0.77M_(⊙).By employing the 2013 version of the Wilson-Devinney(W-D)method to synthesize a light curve,we derived photometric solutions indicating that V0405 Dra is a new deep(f=68.7%)and low-mass ratio(q=0.175)contact *** fast decrease in its orbital period is likely caused by mass transfer from the more massive primary star to the less massive secondary star,or due to angular momentum *** further mass transfer and loss of angular momentum,the binary will gradually evolve into a tighter contact configuration,eventually leading to a merger into a single star,following the evolutionary paths suggested for such deep and low mass ratio contact binaries.

关键词： (stars:)binaries(including multiple):close (stars:)binaries:eclipsing stars:individual(V0405 Dra)

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

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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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Offload Strategy for Edge Computing in Satellite Networks Based on Software Defined Network

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Computers, Materials & Continua 2025年第1期82卷 863-879页

作者： Zhiguo Liu Yuqing Gui lin Wang Yingru jiang Communication and Network Laboratory Dalian UniversityDalian116622China College of Environment and Chemical Engineering Dalian UniversityDalian116622China

Satellite edge computing has garnered significant attention from researchers;however,processing a large volume of tasks within multi-node satellite networks still poses considerable *** sharp increase in user demand for latency-sensitive tasks has inevitably led to offloading bottlenecks and insufficient computational capacity on individual satellite edge servers,making it necessary to implement effective task offloading scheduling to enhance user *** this paper,we propose a priority-based task scheduling strategy based on a Software-Defined Network(SDN)framework for satellite-terrestrial integrated networks,which clarifies the execution order of tasks based on their ***,we apply a Dueling-Double Deep Q-Network(DDQN)algorithm enhanced with prioritized experience replay to derive a computation offloading strategy,improving the experience replay mechanism within the Dueling-DDQN ***,we utilize the Deep Deterministic Policy Gradient(DDPG)algorithm to determine the optimal resource allocation strategy to reduce the processing latency of *** results demonstrate that the proposed d3-DDPG algorithm outperforms other approaches,effectively reducing task processing latency and thus improving user experience and system efficiency.

关键词： Satellite network edge computing task scheduling computing offloading

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