The model fitted to the observed spectra also allows the measurement of the linewidth and power of each mode (see poster II). The linewidths are related to the damping mechanisms and the energies give information on the excitation mechanisms. Here the results of these parameters as well as the relative energy shared by the components of a given

The definition of the model to fit to the observed spectra depends on the physics we are assuming is present in the phenomena we are observing. Here we present the results obtained following the fit of several models (described in poster II). Therefore the effects of asymmetrical line shapes, a common background for all modes, fixed relative power

Data acquired by GOLF experiment onboard SOHO during ~20 months has been analysed. GOLF is a disk-integrated sunlight experiment therefore biased to observe very low ell modes (ell 3). However the excellent ratio signal to background (S/B) achieved permits also the detection of some modes with 4 ell 6 and those from n >= 8 up to the cut-off

Below 1.3 mHz the solar background level increases as well as the energy of the solar acoustic modes decreases. This situation yields the detection of low degree p-modes extremely difficult because the signal to background ratio is very small (S/B ll 1). Yet, these modes are of paramount importance to be able to infer the structure of the solar

A combination of inverse and forward analysis techniques has been applied to p-modes rotational splittings in order to infer the solar rotation rate in the deeper radiative regions (r 0.45Rodot). In this analysis, we first infer the rotation distribution down to 0.45Rodot using a 2D inversion method. We then use that rotation rate to discuss the

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