Intermittency in the photosphere and corona as derived from the Hinode data

Details Intermittency in the photosphere and corona as derived from the Hinode data Intermittency in the photosphere and corona as derived from the Hinode data

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsp21b..01a&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SP21B-01

Physics

4430 Complex Systems, 4475 Scaling: Spatial And Temporal (1872, 3270, 4277), 7524 Magnetic Fields, 7554 X-Rays, Gamma Rays, And Neutrinos, 7839 Nonlinear Phenomena (4400, 6944)

Scientific paper

Recent studies undoubtedly demonstrate that the magnetic fields in the photosphere and corona are strongly non-Gaussian and can be represented as intermittent structures, which offers new views on the underlying physics. In particular, such problems as the existence in the corona of localized areas with extremely strong resistivity (required to explain magnetic reconnection of all scales) and the interchange between small and large scales (required in study of the photosphere/corona coupling), to name a few, can be easily captured by the concept of intermittency. This study is focused on simultaneous time variations of intermittency properties derived in the photosphere, chromosphere and corona. We analyzed data for NOAA AR 10930 acquired between Dec 08, 2006 12:00 UT and Dec 13, 2006 18:45 UT. Photospheric intermittency was inferred from Hinode magnetic field measurements, while intermittency in the transition region and corona was derived from Nobeyama 9 GHz radio polarization measurements, high cadence Hinode/XRT/Be-thin data as well as GOES 1-8Å~ flux. Photospheric dynamics and its possible relationship with the intermittency variations were also analyzed by calculating the kinetic vorticity. For this case study we found the following chain of events. Intermittency of the photospheric magnetic field peaked after the specific kinetic vorticity of plasma flows in the AR reached its maximum level (4 hour time delay). In turn, gradual increase of coronal intermittency occurred after the peak of the photospheric intermittency. The time delay between the peak of photospheric intermittency and the occurrence of the first strong (X3.4) flare was approximately 1.3 days. Our analysis seems to suggest that the enhancement of intermittency/complexity first occurs in the photosphere and is later transported toward the corona.

Affiliated with

Also associated with

No associations

Rating

Intermittency in the photosphere and corona as derived from the Hinode data does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Intermittency in the photosphere and corona as derived from the Hinode data, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Intermittency in the photosphere and corona as derived from the Hinode data will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1401900