Chromospheric flare
WebNov 5, 2015 · It is widely accepted that the vast majority of the solar flare radiative energy originates in the photosphere and chromosphere. The chromospheric radiation is dominated by hydrogen, calcium, and magnesium lines, plus hydrogen continua, providing vital diagnostics on energy deposition rates in the lower atmosphere. WebWith observations of the Interface Region Imaging Spectrograph (IRIS), we study chromospheric heating and evaporation during an M1.6 flare SOL2015-03-12T11:50. At the flare ribbons, the Mg ii 2791.59 Å line shows quasi-periodic short-duration red-wing enhancement, which is likely related to repetitive chromospheric condensation as a …
Chromospheric flare
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WebApr 6, 2007 · The formation of chromospheric radiations during a flare presents several difficult and interesting physical problems. Comments: Coimbra Solar Physics Meeting … WebThe flare plasma dynamics and associated thermal evolution during a flare consists of a number of sequential processes: plasma heating in coronal reconnection sites, chromospheric flare plasma heating (either by precipitating nonthermal particles or by downward propagating heat conduction fronts), chromospheric evaporation in the form …
WebThis low energy X-ray emission seems to indicate that the heating source was around the null point and along the outer spine, while it did not show any spatial correlation with the chromospheric emission, contrarily to what observed by Yang, Guo & Ding (2015) in a X-class circular ribbon flare occurred on 2013 October 23. WebAug 22, 2024 · The chromosphere is a highly dynamic outer plasma layer of the Sun. Its physical processes accounting for the variability are poorly understood. We …
WebWe present observations of optical spectra of a flare in which blue line asymmetry was seen for more than 4 min close to the flare onset. The maximum blue asymmetry coincided with the maximum of a hard X-ray and microwave burst. We discuss possible interpretations of the blue asymmetry and conclude that the most plausible one is electron-beam heating … WebApr 11, 2024 · One is based on the evaporation process during the flare, which can transport the chromospheric fractionated plasma very quickly to the corona in the decay phase of the flares. The other scenario is based on the evaporation process as well as the flare-driven Alfvén waves. In the decay phase, the reflection of the high amplitude flare …
WebSep 26, 2024 · Flares are classified into confined and eruptive types according to their association with CMEs (Wang & Zhang 2007; Sun et al. 2015; Thalmann et al. 2015 ), although the visibility of CMEs depends greatly on flare intensity (Yashiro et al. 2005 ).
WebThe chromosphere and transition region The physical processes occurring as a result of the transfer of energy and momentum from the primary solar flare energy release site in the corona to the underlying chromosphere and transition region during the course of the flare are investigated through a comparison of theoretical models and observational … high sithWebFeb 28, 2011 · the chromosphere. We studied the Hα emission of a flare which occurred on 3 July 2002 using some spectroscopical observations from the Ondrejov Observatory. Analyzing the available data in other... high site fidelityWebSep 1, 2013 · The SCFS will record are spectra in two channels in the wavelength range of 350-890 nm, which has several chromospheric spectral lines. The SCFS will have a multi-fiber based slit capable of... how many days for common coldWeb2 days ago · We present light curves and flares from a seven day, multi-wavelength observational campaign of AU Mic, a young and active dM1e star with exoplanets and a debris disk. We report on 73 unique flares between the X-ray to optical data. We use high-time resolution NUV photometry and soft X-ray (SXR) data from XMM-Newton to study … high sitting beach chairsWebStepwise and permanent changes of magnetic fields can often be observed in active regions during flares 1,2. These changes are important because they may allow us to probe the reconfiguration of coronal fields during flares and it has been speculated that they may be related to sunquakes. how many days for cilantro to germinateWebThe chromospheric and coronal evolution of the AR around the procedure of Falconer et al. (2002) and Jiang et al. (2014), the time of the major flare as seen in the AIA 304 Å and we estimated the shear by using the following horizontal shear 193 Å passbands is shown in the two bottom rows of Figure 3. high sith-curityWebOct 9, 2024 · Heated chromospheric material will expand upward into the (smaller density) corona, filling loops that appear as hot, dense, thermal flare structures visible at EUV and soft X-ray wavelengths. This process, first described by Neupert ( 1968 ), has become known as "chromospheric evaporation" (see reviews by Bornmann 1999 and Fletcher … how many days for corn to germinate