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First Results of Joint OVSA and HESSI Observations

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Title: First Results of Joint OVSA and HESSI Observations


1
First Results of Joint OVSA and HESSI Observations
Dale E. Gary1, Edward J. Schmahl2 1New Jersey
Institute of Technology 2University of Maryland
2
Joint Observations of Five Solar Bursts
  • We present 5 solar bursts observed jointly in
    microwaves with Owens Valley Solar Array (OVSA)
    and in hard X-rays with the Ramaty Hi-Energy
    Solar Spectroscopic Imager (RHESSI).
  • A spectral comparison of the 5 bursts in both
    microwaves and hard X-rays is presented in the
    accompanying figures.
  • We examine one event, 2002 Mar 18, in more
    detail, both spectrally and spatially.

3
2002 Feb 20
4
2002 Feb 23
5
2002 Feb 25
6
2002 Mar 18
7
2002 Mar 29
8
  • Ask to see this animation of the RHESSI spectrum
    for the 2002 Mar 18 burst on a laptop computer!

9
OVSA Radio Spectra (2002 Mar 18)
10
Spectral Results (2002 Mar 18)
  • Thermal part of X-ray emission rises and falls
    relatively smoothly.
  • gt 25 keV X-rays vary in several acceleration
    episodes, apparently independently of the thermal
    emission.
  • In first acceleration episode, gt 25 keV X-rays
    progressively harden (from d 7.5-4.7) .
  • At the same time, the OVSA spectral peak
    increases monotonically.
  • Spectral peak can increase due to three effects
    increase in NL, increase in B, or decrease in d
    (Dulk 1985).

11
RHESSI Images (2002 Mar 18)
12-25 keV
25-50 keV
12
BBSO Context (2002 Mar 18)
13
Spatial Results (2002 Mar 18)
  • Thermal part of X-ray emission fills a small
    loop, about 20 long.
  • gt 25 keV X-rays come from a smaller source at one
    end of the loop.
  • OVSA source is compact, and all frequencies
    appear to be nearly cospatial.

14
Conclusions
  • After only four months OVSA and RHESSI have
    jointly observed at least a dozen events.
  • We have presented some preliminary comparisons of
    5 events.
  • The outstanding spectral resolution of RHESSI
    allows detailed comparison with OVSA microwave
    spectra.
  • The thermal components seen by RHESSI are only
    weakly detected with OVSA.
  • Comparisons of spatial source structure have not
    yet been done, but will be done as soon as
    possible.
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