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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TeamSciMeetingMar09
TeamSciMeetingMar09

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** Studies of small ARs and Flares
*** Moss (Tripathi et al., 2008)
*** AR Jets (Chifor et al., 2008)
*** AR microflares and precursors to filament eruptions (Chifor et al., 2008, 2009)
*** Small flares (Del Zanna, 2008)
*** AR flows (Del Zanna, 2008)
*** AR loops: n_e, T_e and flows (Tripathi et al. 2009)
*** Small flare activity (Mitra et al., 2009)
** This presentation
Small active region close to the limb
Can take the n_e ratio as we go from the disc to off-limb.
We can also attempt to get the temperature in a simple way. Never subscribed to this before, but I'm showing a plot! We want to see how hot the temperature is. But if you take Fe XVI / Fe XV, you can see that the core is very hot around log(T) 6.7. We've done the same for Fe XIV / Fe XIII, we get a lot more, interesting structure, which we need to follow up and invesigate.
We want to look for these higher temperature lines, but must be really careful about removing blends. The Fe XVII line is a good line to use.
When looking at Ca XVII, you can't use the CHIANTI Fe XI ratio, as it's wrong. But you can do it empirically by finding the ratio on the quiet Sun and then using that to remove the blend with Ca XVII.
This page (revision-83) was last changed on 02-Feb-2017 13:19 by David R WilliamsTop