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Solar Supergranular Fractal Dimension Dependence on the Solar Cycle Phase

Research in Astronomy and Astrophysics 2022年第4期22卷 55-61页

作者： G.Rajani G.M.Sowmya U.Paniveni R.Srikanth PES College of Engineering Mandya-571401KarnatakaIndia GSSS Institute of Engineering and Technology for Women KRS RoadMetagalli Mysuru-570016KarnatakaIndia Bangalore University JnanabharathiBengaluru-560056India Poornaprajna Institute of Scientific Research DevanahalliBangalore-562110KarnatakaIndia

We study the complexity of the supergranular network through fractal dimension by using the Ca II K digitized data archive obtained from the Kodaikanal Solar *** data consist of 326 visually selected supergranular cells spread across the 23rd solar *** cells that were well-defined were chosen for the analysis and we discuss the potential selection effect thereof,mainly that it favors cells of a smaller size(<20 Mm).Within this sample,we analyzed the fractal dimension of supergranules across the solar cycle and find that it is anticorrelated with the activity level.

关键词： sun:chromosphere sun:granulation sun:activity

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Two-telescope-based solar seeing profile measurement simulation

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Research in Astronomy and Astrophysics 2021年第12期21卷 305-314页

作者： Zi-Yue Wang De-Qing Ren Raffi Saadetian National Astronomical Observatories/Nanjing Institute of Astronomical Optics&Technology Chinese Academy of SciencesNanjing 210042China CAS Key Laboratory of Astronomical Optics&Technology Nanjing Institute of Astronomical Optics&TechnologyNanjing 210042China University of Chinese Academy of Sciences Beijing 100049China Physics&Astronomy Department California State University NorthridgeCalifornia 91330-8268USA

Measurements of the daytime seeing profile of the atmospheric turbulence are crucial for evaluating a solar astronomical site so that research on the profile of the atmospheric turbulence as a function of altitude C_(n)^(2)(h_(n))becomes more and more critical for performance estimation and optimization of future adaptive optics(AO)including the multi-conjugate adaptive optics(MCAO)***,the S-DIMM+method has been successfully used to measure daytime turbulence profiles above the New Solar Telescope(NST)on Big Bear ***,such techniques are limited by the requirement of using a large solar telescope which is not realistic for a new potential astronomical ***,the AMASP(advanced multiple-aperture seeing profiler)method is more portable and has been proved that can reliably retrieve the seeing profile up to 16 km with the Dunn Solar Telescope(DST)on the National Solar Observatory(Townson,Kellerer et al.).But the turbulence of the ground layer is calculated by combining A-MASP and S-DIMM+(Solar Differential Image Motion Monitor+)due to the limitation of the twoindividual-telescopes *** solve these problems,we introduce the two-telescope seeing profiler(TTSP)which consists of two portable individual *** simulations have been conducted to evaluate the performance of *** find our TTSP can effectively retrieve seeing profiles of four turbulence layers with a relative error of less than 4%and is dependable for actual seeing measurement.

关键词： turbulence atmospheric effects sun:granulation

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Length Scale of Photospheric Granules in Solar Active Regions

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Research in Astronomy and Astrophysics 2022年第8期22卷 103-110页

作者： Yan-Xiao Liu Chao-Wei Jiang Ding Yuan Ping-Bing Zuo Wen-Da Cao Institute of Space Science and Applied Technology Harbin Institute of TechnologyShenzhen 518055China New Jersey Institute of Technology Center for Solar ResearchNewarkNJUSA Big Bear Solar Observatory 40386 North Shore LaneBig Bear CityCAUSA

Investigating the length scales of granules could help understand the dynamics of granules in the *** this work,we detected and identified granules in an active region near disk center observed at wavelength of TiO(7057?)by the 1.6 m Goode Solar Telescope(GST).By a detailed analysis of the size distribution and flatness of granules,we found a critical size that divides the granules in motions into two regimes:convection and *** length scales of granules with sizes larger than 600 km follow Gauss function and demonstrate“flat”in flatness,which reveal that these granules are dominated by *** with sizes smaller than 600 km follow power-law function and behave power-law tendency in flatness,which indicate that the small granules are dominated by ***,for the granules in active regions,they are originally convective in large length scale,and directly become turbulent once their sizes turn to small,likely below the critical size of 600 *** with the granules in quiet regions,they evolve with the absence of the mixing motions of convection and *** a difference is probably caused by the interaction between fluid motions and strong magnetic fields in active *** strong magnetic fields make high magnetic pressure which creates pressure walls and slows down the evolution of convective *** walls cause convective granules extending to smaller sizes on one hand,and cause wide intergranular lanes on the other *** small granules isolated in such wide intergranular lanes are continually sheared,rotated by strong downflows in surroundings and hereby become turbulent.

关键词： sun:granulation sun:photosphere sun:faculae plages

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