July 23, 2002 flare

QUESTIONS/COMMENTS/ETC. to Säm Krucker, krucker@ssl.berkeley.edu, 510 643 3101

first version of Apj letter, january 16 (ps file)

AGU poster, dec 6 (pdf file)

NEW: Nobeyama 17 GHz movie with 12keV and 35 keV RHESSI contours

NEW: first order pile up correction

This is the result using David's programs.

white curve: the uncorrected spectrum

red curve: corrected spectrum

for a 20 second time interval around the main peak. the difference of these two spectra is also plotted. total spectrum is plotted including background.

old version before November 29 changes

NEW version after November 29 changes (better pile up correction)

Eduard's imaging spectroscopy page

Halpha movie: 1 minute cadence before 00:27UT, 30 second cadence later

  • Halpha (images) & RHESSI 30-50 keV contours (alignment good within 10 arcsec or so)

    MDI movies: 1 minute cadence, so the movies have only 11 frames

  • MDI magnetogram (images) & RHESSI 30-50 keV contours
  • MDI magnetogram (pre-event subtracted) & RHESSI 30-50 keV contours
  • absolute value of MDI magnetogram (pre-event subtracted) & RHESSI 30-50 keV contours
  • MDI magnetogram (images), contours are changes relative to preflare, white = pos. changes, black= neg. changes
  • MDI magnetogram (images) with preevent emission subtracted

    POST FLARE MOVIE: TRACE & RHESSI

  • POST FLARE LOOPS: 01:00-02:40 UT (6-18 keV), slowly rising HXR source (~3km/s)

    HXR source position as a function of energy during main peak of the flare

    CORONAL, SOFTER SOURCE (eastern source): clear shift of 5 arcsec

  • CORONAL, SOFTER SOURCE TO THE EAST shows clearly different positions: at higher energies the source seems to originate from higher altitude. 10keV and 20keV centroids are about 5 arcsec apart. Since the shutters are in, the images below 8 keV might be dominated by higher energy photons. This is compatible with the sources position below 8 keV showing source position at higher altitude.
  • CORONAL, SOFTER SOURCE: 10 keV image and 25 keV contours, the sources are separated by about 5 arcsec = 4000 km

    harder sources (footpoints): no clear difference within 1 arcsec

  • northern, hard source
  • source between
  • southern source seems is composed of at least 2 sources

    RHESSI-TRACE movies (detectors 3-9 are used giving 7 arcsec resolution, images are CLEANed)

    TRACE: images are scaled to the maximum in the time series.

    RHESSI: levels are 30,50,70,90%, images are scaled separately to the maximum in the image. a cutoff at lower flux is applied

  • 00:20-00:40 UT (RED: 12-20 keV, BLUE: 100-150 keV), plus time profiles
  • same as MPEG movie
  • 00:20-00:40 UT (white contours=before shutter comes in, black afterwards) 30-50 keV
  • 00:20-00:40 UT (white contours=before shutter comes in, black afterwards) 20-30 keV
  • 00:20-00:40 UT (white contours=before shutter comes in, black afterwards) 6-12 keV
  • MAIN PHASE (thick shutter in) 50-100 keV (grid 2-9), 7 arcsec resolution
  • MAIN PHASE (thick shutter in) 100-150 keV (grid 3-9), 7 arcsec resolution
  • MAIN PHASE (thick shutter in) 100-150 keV (grid 2-9), 4 arcsec resolution

    Overview plot: GOES lightcurves, RHESSI lightcurves and spectrogram

    NOTE: the thin shutter is in all the time, the thick shutter is moving in and out several time changing the flux significantly.

    this is a zoom in around the main HXR emission

    NOTE: thick shutter in all the time

    here are some images:

    images (grid 2-9, 64"*64") at 16 energy ranges during the first main peak

    30-second averaged images at different energies can be found here (ps files):

    detectors 3 -9 are used, images are CLEANed, images shown are scaled separately to the maximum in the image.

    NOTE: When the thick shutter is out, there are problems with pile-up (e.g. 00:40:16 UT).

  • 100-200 keV, two footpoints are dominating the image
  • 30-80 keV, again the two footpoints plus some more sources are seen
  • 20-30 keV
  • 15-20 keV

    here are the same files convert to png files (not as nice resolution):

    footpoints seem to flare simultaneously (above 100 keV) and are about equal in intensity

    Separation of footpoints seen above 100 keV

    NOTE: The footpoints are separating over several minutes. the separation speed is 3 arcsec per minute (36 km/s). Hence, in a flare with only a 40 second peak, this kind of separation is hard to see.