Modelling Solar Oscillation Power Spectra: II. Parametric Model of Spectral Lines Observed in Doppler Velocity Measurements

Abstract

We describe a global parametric model for the observed power spectra of solar oscillations of intermediate and low degree. A physically motivated parameterization is used as a substitute for a direct description of mode excitation and damping as these mechanisms remain poorly understood. The model is targeted at the accurate fitting of power spectra coming from Doppler velocity measurements and uses an adaptive response function that accounts for both the vertical and horizontal components of the velocity field on the solar surface and for possible instrumental and observational distortions. The model is continuous in frequency, can easily be adapted to intensity measurements and extends naturally to the analysis of high-frequency pseudo modes (interference peaks at frequencies above the atmospheric acoustic cutoff).

References in corpus (2)

• On The Determination of MDI High-Degree Mode Frequencies
• An Improved Method for Fitting p-Mode Profile Asymmetries

Cited by in corpus (6)

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• Asymmetry of line profiles of stellar oscillations measured by Kepler for ensembles of solar-like oscillators: impact on mode frequencies and dependence on effective temperature
• Modelling the asymmetries of the Sun's radial $p$-mode line profiles
• Recent Developments in Helioseismic Analysis Methods and Solar Data Assimilation
• Velocity-intensity asymmetry reversal of solar radial p-modes