This page (revision-83) was last changed on 02-Feb-2017 13:19 by David R Williams

This page was created on 27-Jan-2009 03:17 by David R Williams

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At line 192 changed one line
Seems like we have issues more with the Wiki than with Data Access per se. HEM suggested Nuggets à la Hudson for RHESSI. KPD felt that we weren't advertising or communicating enough. DRW felt that it was easy and good to put information on the EISWiki.
Ultimately, though, it might be good to set up ways to make event catalogues; it could be possible for people to construct and contribute custom cataloguing/data-mining routines.
At line 194 added 5 lines
Seems like we have issues more with the Wiki than with Data Access per se, though.
*HEM suggested Nuggets à la Hudson for RHESSI.
*KPD felt that we weren't advertising or communicating enough.
*DRW felt that it was easy and good to put information on the EISWiki.
At line 208 added 10 lines
Correlation of Doppler speed and non-thermal width implies unresolved flows in acrive regions.
Magnetic reconnection, if it at all takes place for coronal heating, is far below the height of the reconnection point that causes major flares.
Recent results from DHB: even if we look at 1 arcsec pixel of Quiet Sun, we usually have the same shape of EM distributions. Unresolved very common nature of a plasma temperature distribution that causes this universal shape of DEM even in a size less than 1".
Triggered by Sakao et al.'s observations, we observe high-velocity outflows, although they're slow in the solar wind sense. We've actually found plasma upflows taking place close to coronal holes and quiet Sun beside active regions. The same sort of mechanism took place the data analysed by Imada after the largest 20061213 flare. In quiet regions, the kinetic energy is roughly enough to heat the QS corona.
20061217 LDE was analysed by Hara: Reconnection inflows seen in LOS velocity by HH;
20060519 flare: EIS counterpart of a ''Masuda'' source? The EIS slit was very lucily at the flaring loop top when its initial phase started. ''TRACE'' shows a clear two-ribbon pattern; RHESSI image contours for 12 - 25 keV which show a high-temperature RHESSI structure. Fe XXIII emission corresponding to it shows a slight red-shift.
This page (revision-83) was last changed on 02-Feb-2017 13:19 by David R WilliamsTop