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

Only authorized users are allowed to rename pages.

Only authorized users are allowed to delete pages.

Version Date Modified Size Author Changes ... Change note
83 02-Feb-2017 13:19 43 KB David R Williams to previous
82 19-Mar-2009 13:50 41 KB David R Williams to previous | to last
81 18-Mar-2009 21:12 40 KB David R Williams to previous | to last
Incoming links Outgoing links
TeamSciMeetingMar09
TeamSciMeetingMar09

Difference between version and

At line 1 added 2 lines
[{ALLOW edit EISMainUsers}]
[{ALLOW view Anonymous}]
At line 568 added 33 lines
Small-FOV, high-cadence spectral images are key for good physics.
*** Line profiles from FPs during impulsive phase
*** Measure Doppler and nonthermal velocities as functions of time and temperature
*** How are line profiles related to electron beam parameters
*** n_e measurements.
Wish list:
# < 4-min cadence rasters
# moderate FOV 100 x 100
# fast exposures < 5 seconds
## (originally advertised 1 second exposures)
# line selections:
Core lines, Fe species, at least one n_e sensitive pair
# long duration observations >16 hours per day
# Max millennium ToOs
# not using the flare trigger to increase chance of catching the very early conditions
## what latency is there using the trigger anyway?
## ''seems like it's a second or two from XRT's trigger to EIS
# for RHESSI-specific observations, running EIS only during RHESSI's day?
*** People often write that a spectral window is centred on a given line. Maybe junk the red side of the window, because most high-T lines have blue shifts, but not high redshifts.
*** Are coronal HXR sources the reconnection site? EIS could measure the differences in the pre- and post-flare densities. Perhaps detect reconnection inflows around the source.
*** Observe regions __after__ they've rotated beyond the limb.
*** Impulsive EUV emission
high-cadence (1-second) 266" slot observations
*** resonant absorption of MHD waves
At line 605 added 12 lines
PRY: if EIS puts a strong message that we want to do one kind of obserbvation
HPW: how do we prioritise our observations when the ARs come back?
PRY: would be good if we came up with an observation
Needs to be freedom -- want to run for long periods of time
Could there be working groups on how to build active region observations, for example? Does there need to be a meeting?
* Active regions
* Quiet Sun
This page (revision-83) was last changed on 02-Feb-2017 13:19 by David R WilliamsTop