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Variations of the Low l Solar Acoustic Spectrum Correlated with the Activity Cycle

Published online by Cambridge University Press:  12 April 2016

P.L. Pallé ,
C. Régulo  and
T. Roca Cortés
P.L. Pallé
Affiliation:
Instituto de Astrofisica de Canarias,38200 La Laguna. Tenerife, Spain
C. Régulo
Affiliation:
Instituto de Astrofisica de Canarias,38200 La Laguna. Tenerife, Spain
T. Roca Cortés
Affiliation:
Instituto de Astrofisica de Canarias,38200 La Laguna. Tenerife, Spain

Abstract

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Solar cycle variation of the frequencies and of the power of solar acoustic oscillations are investigated. Integrated sunlight data from 1977 to 1988 obtained at the Observatorio del Teide (Izaña, Tenerife), using a resonant scattering spectrophotometer, is analyzed in 60 day time strings and their power spectra are calculated from 2 to 3.8 mHz. To study the frequency variation, each power spectrum is cross-correlated with the one corresponding to the 1981 series and the shifts of the centroids of the cross-correlation peaks are calculated. The results show a clear variation in frequency of the cross-correlation peaks of −0.37 ± 0.04 μHz peak to peak as solar activity cycle goes from maximum to minimum. Moreover, this effect is found to depend on the l value of the modes, being absent for l = 0 and of 0.42 ± 0.06 μHz for l = 1. These results can be interpreted as an amplitude modulation between modes of the same multiplet, probably as a consequence of the action of strong magnetic fields. As low l modes penetrate deeply into the Sun’s interior, these observations suggest changes in its structure correlated with the solar activity cycle. When the power of the modes is calculated, using the same series as before, and its change along the solar cycle is studied, a variation of ~ 40% is found, the power being higher when solar activity is at its minimum. If this effect is independent of the l value of the p-modes, the results can be interpreted in terms of a change in the efficiency of the excitation mechanism of such modes. Indeed, if turbulent convection is such a mechanism, a change in the characteristic size of the granulation would account for the observed effect. Alternatively, another explanation could be a selective change in the efficiency of the excitation and/or damping mechanisms of the l ≤ 3 modes in front of other l value modes.

Type
Part 3: Helioseismology
Information
International Astronomical Union Colloquium , Volume 121: Inside the Sun , 1990 , pp. 349 - 355
Copyright
Copyright © Kluwer 1990

References

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