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.
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.
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
