Multi-wavelength observations of the 2014 June 11 M3.9 flare: temporal and spatial characteristics

查看全文 作　　者：Damian [1]J.Christian;David [2,3]Kuridze;David [3]B.Jess;Menoa [1]Yousefi;Mihalis [3]Mathioudakis 机构地区：[1]Department of Physics and Astronomy,California State University Northridge,Northridge,CA 91330,USA;[2]Institute of Mathematics,Physics and Computer Science,Aberystwyth University,Ceredigion,Cymru,SY23 3,UK;[3]Astrophysics Research Center,School of Mathematics and Physics,Queen's University Belfast,Belfast BT7 INN,UK 出　　处：《Research in Astronomy and Astrophysics》索引2019年第19卷第7期,共10页 基　　金：supported by S?r Cymru II Part-funded by the European Regional Development Fund through the Welsh Government. D.K;support from the Georgian Shota Rustaveli National Science Foundation project FR17 323 摘　　要：We present multi-wavelength observations of an M-class flare(M3.9) that occurred on 2014 June 11.Our observations were conducted with the Dunn Solar Telescope(DST),employing adaptive optics,the multi-camera system Rapid Oscillations in Solar Atmosphere(ROSA),the new Hydrogen-Alpha Rapid Dynamics camera(HARDcam) in various wavelengths,such as Ca II K,Mg I b2(at 5172.7 A),and Hα narrow band and G-band continuum filters.Images were re-constructed using the Kiepenheuer-Institut Speckle Interferometry Package(KISIP) code,to improve our image resolution.We observed intensity increases of ≈120%–150% in the Mg,Ca K and Hα narrow band filters during the flare.Intensity increases for the flare observed in the SDO EUV channels were several times larger,and the X-rays,as recorded by GOES,increased over a factor of 30 for the harder band.Only a modest delay was found between the onset of flare ribbons of a nearby sympathetic flare and the main flare ribbons observed in these narrow band filters.The peak flare emission occurred within a few seconds for the Ca K,Mg and Hα bands.Timedistance techniques indicate propagation velocities of ≈60 km s^-1 for the main flare ribbon and as high as300 km s^-1 for smaller regions,which we attribute to filament eruptions.This result and delays and velocities observed with SDO(≈100 km s^-1) for different coronal heights agree well with the simple model of energy propagation versus height,although a more detailed model for the flaring solar atmosphere is needed.Finally,we detected marginal quasi-periodic pulsations(QPPs) in the 40–60 s range for the Ca K,Mg and Hα bands,and such measurements are important for disentangling the detailed flare-physics. 关 键 词：magnetic reconnection-Sun flares-Sun ATMOSPHERE