HOP 0020

HINODE Operation Plan (HOP)

accepted on

20-jun-07

HOP No.

HOP title

HOP 0020

EIS+ SOT+XRT Physical mechanisms driving solar microflares and supergranular network dynamics - relevance for coronal heating

abstract of observational proposal

This proposal merges together attempts to observe two kinds of solarstructures – solar micro flares and super granular network – which are planned tobe investigated toaddress common openquestions on the irrelevance for the heating and dynamics of the solar corona.

request to SOT

SOT: We plan (if possible) to run in time a sequence of 3exposures:2using the BFI imager and 1 using the NBIimager.The reason is to cover evolution of the photosphere with its magnetic concentration signatures (G-band), evolution of the longitudinal component of the magnetic field vector inthe photosphere, and evolution of chromosphere (CaIIH)witha reasonable temporal resolution (～10s per image,　～30s　per　sequence　of 3 selected channels).　
　•BFI: G-band and CaIIH channels,
　 FOV:109”x109”(1k x1kmode, binning 2 x 2 pxs),
3bit JPEG compression, cadence:～10s per filtergram,
telemetry needed: 300kbps, nocompensation of the solar rotation
•NFI: FeI630.25nm longitudinal magnetograms,other parameters as in
case of BFI
•SP:none

request to XRT

XRT: high cadence of the images is required using just one selected filter using no binning and loss-less compression of data.

•Microflare mode: 256x256px,thin Be filter, exposure max. 1s with AEC cadence 10s

•Network mode: 384x384px, thin-Al/Mesh, exposure max. 15s with AEC, cadence 15s For the each particular day target will selected well in advance leading to the corresponding XRT observing mode.

request to EIS

EIS: measurements are proposed using 2 prepared rasters acronymedas’ Context－calib－jr’and’Obs－sit－stare－jr’.They have been specified using the EIS study template and the corresponding.DEF file which we real ready sent to the EISSSCL. Culhane. The EIS measurements should start and ends with 3 repetitions of the scanning’Context－calib－jr’raster (28minutes). In between the sit-and-stare’Obs－sit－stare－jr’raster (5.6hours) is scheduled. Intention is to place the EIS slit for the sit-and-stare raster to the middle of the X-range of the previous scanning raster. For both rasters the same set of 11 selected lines is used.