1/3/2023 0 Comments Markx phase dimming![]() ![]() The plasma composition is the same in the current sheet, in the loop arcade, and in the ambient plasma, so all these plasmas are likely of coronal origin. Both the electron density and thermal structure do not show significant evolution with time, while we found that the size of the loop arcade in the Hinode plane of the sky decreased with time. ![]() Post-CME plasma is hotter than the surrounding corona, but its temperature never exceeds 3 MK. We find that the loop arcade observed by EIS and XRT may not be related to the post-eruption arcade. ![]() The main physical properties of the plasma along the line of sight-electron density, thermal structure, plasma composition, size, and, when possible, mass-are measured and monitored with time for the first three hours following the CME event of 2008 April 9. The goal of this paper is to provide a comprehensive set of measurements for all these aspects of the CME phenomenon made on the same CME event. The field of view includes a post-eruption arcade, a current sheet, and a coronal dimming. In the present work we study the evolution of an active region after the eruption of a coronal mass ejection (CME) using observations from the EIS and XRT instruments on board Hinode. Outflow, originating from the 'open' field twin dimming regions. Two hours after the eruption Hinode/EIS observations show no substantial plasma The mass loss occurs mainly during the period of strongest CME acceleration. That: (1) the global-scale dimmings, expanding from the source region of theĮruption, propagate with a speed similar to that of the leaving CME front (2) Rope, but also the ensuing stretching of the overlying arcade. Motion pattern of the twin dimmings reflects not only the eruption of the flux 'sheared-to-potential' evolution as the postflare loops. Additionally, they rotate around the 'center' of theįlare site, i.e., the configuration of the dimmings exhibits the same Pre-flare sigmoid structure, show an apparent migration away from the site of Two confined, bipolar dimming regions, appearing near the footpoints of a Weįind that these dimmings are synchronized and appear during the impulsiveĪcceleration phase of the CME, with the highest EUV intensity drop occurring aįew minutes after the maximum CME acceleration. Observations with the twin STEREO spacecraft in quadrature allow us toĬompare for the first time in one and the same event the temporal evolution ofĬoronal EUV dimmings, observed simultaneously on-disk and above the limb. 378348 stanza faceplate engraving sheet.We investigate the early phase of the 13 February 2009 coronal mass ejection.378346 stanza faceplate engraving sheet.ai. Markx phase dimming software license#
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