The local I-V phase difference to investigate the background spatial distribution

Details The local I-V phase difference to investigate the background spatial distribution The local I-V phase difference to investigate the background spatial distribution

Jan 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001esasp.464..661m&link_type=abstract

Proceedings of the SOHO 10/GONG 2000 Workshop: Helio- and Asteroseismology at the Dawn of the Millennium, 2-6 October 2000, Sant

Computer Science

2

Sun: Oscillations

Scientific paper

The phase difference between the intensity and velocity (I-V) is claimed to be a powerful tool for understanding the nature of the solar oscillations. The identification of a solar background in the intensity-velocity l-ν diagram has been associated to a possible signature of the source of the resonant oscillations. Many attempts have been accomplished to match the results from the models to the recent I-V values obtained from the observations. In this paper we present the I-V phase computed with a different approach: the local analysis. The global behaviour enhanced by the spherical harmonic decomposition is now mixed to the local, non-resonant, phenomena. Nevertheless, where convection is negligible, still two phase regimes, or populations, are significant. The advantage of this method consists of the capability to follow the distribution on the disk of I-V at different frequencies and correlate to the solar structures. The background locations are found where the velocity power is low. The results from some days of full-disk images with a 4"/pixel resolution in the sodium D lines are shown and a possible source of the solar background is suggested.

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