Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sp22a07s&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SP22A-07
Astronomy and Astrophysics
Astrophysics
7500 Solar Physics, Astrophysics, And Astronomy, 7554 X Rays, Gamma Rays, And Neutrinos
Scientific paper
There have been many claims of correlation between solar neutrino measurements and various solar indices, including coronal brightness. These claims have been greeted with skepticism, largely on the grounds that there is no obvious mechanism to explain the correlation. We review our recent comparative analysis of GALLEX-GNO neutrino data and SOHO-MDI measurements of internal solar rotation, which yields evidence of rotational modulation of the solar neutrino flux. We attribute this modulation to the influence of internal magnetic structures on neutrino propogation. The coronal X-ray flux also exhibits rotational modulation. From this viewpoint, some kind of correlation between neutrino measurements and X-ray measurements is to be expected. We compare the spectra of the two time series with each other and with the distribuition of rotation frequencies in the solar interior. We also examine the correlation spectrum, which gives information about the frequencies responsible for correlation, and about the relative phases of the two oscillations. In order to relate these new studies with earlier studies (which did not involve spectrum analysis), we process the X-ray data in just the same way that the neutrino experiments process the solar neutrino flux. In this way we obtain a sequence of proxy X-ray measurements corresponding to the same start times, end times, and decay time, that apply to the GALLEX-GNO runs. We can then carry out a simple correlation analysis of the neutrino and X-ray run sequences. We shall present the results of these studies and compare these results with earlier claims of correlation between neutrino measurements and solar indices. We wish to acknowledge support by NASA grants NAS 8-37334 and NAGW-2265 and NSF grant ATM-9910215.
Sturrock Peter Andrew
Weber Mark A.
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