Observational Constraints on Models of the Solar Background Spectrum

Details Observational Constraints on Models of the Solar Background Spectrum Observational Constraints on Models of the Solar Background Spectrum

May 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...516..939s&link_type=abstract

The Astrophysical Journal, Volume 516, Issue 2, pp. 939-945.

Astronomy and Astrophysics

Astronomy

32

Convection, Sun: Atmosphere, Sun: Granulation, Sun: Oscillations

Scientific paper

We discuss the properties of the solar background signal as observed in high-quality, l-nu power and phase difference spectra of the continuum (C), velocity (V), and line intensity (I) fluctuations of the Ni I 6768 Å line. These spectra were generated from high-resolution images acquired by the Michelson Doppler Imager on board SOHO. We confirm that the background signal in the velocity power spectra can be reproduced by a composite model with two quasi-stationary components, describing large-scale and small-scale convective motions, and a periodic component. The line and continuum intensity power spectra require additional quasi-stationary and periodic components. The extra quasi-stationary component dominates the intensity and continuum background signals over the spectral region where the I-V phase difference spectra show essentially constant negative phase difference: i.e., below and in between the p-mode ridges (called the plateau-interridge regime by Deubner et al.). Since the I-V phase between the p-mode ridges is not random, the solar background beneath the p-modes must be considered as coherent. We thus speculate that the negative phase regime may be the manifestation of a correlated background. Such a background has been proposed to explain the opposite sense of the asymmetries of the p-mode line profiles in velocity and brightness oscillations.

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