The deenition of the model to t 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 t of several models (described in poster GOLF.II, Roca Cort es et al.). Therefore the effects of asymmetrical line shapes, a common background for all modes, xed relative power in the components of a multiplet and a constant splitting between the components of each multiplet on the resonant frequencies (and their errors) of the modes will be evaluated. Finally, a table of frequencies and splittings will be given.

Temporal behavior of global solar characteristics has been studied. A phenomenological model based on 20-year long measurements of the solar neutrino flux by Cl-Ar detector in Homestake was suggested to describe and to predict the measurements of neutrino counting rate, solar diameter and magnetic field. The correlation between the neutrino flux counting rate and the diameter and their anti-correlation over 30 years with magnetic field are demonstrated. The temporal behavior of the solar global magnetic field during the last 10 years is in excellent agreement with the prediction of the phenomenological model based on the neutrino registration taken until 1991. The temporal behavior of the acoustic oscillation power was studied. The origin of p-modes are discussed.

The study of the Sun as a variable star on a short time scale has been performed using the results of different experiments provided the measurements of global solar neutrino characteristics. The phenomenological model of temporal behavior was suggested based on 20-year long solar neutrino counting rate in Homestake detector. This model is used to describe and to predict the measurements of neutrino counting rate, solar diameter and magnetic field. From the comparison of this model with with observations follows clearly that the model is valid for description of neutrino flux measurements by Cl-Ar and Ga-Ge detectors and radius of the Sun and it works perfectly for the prediction of the global magnetic field. Temporal behavior of solar global magnetic field during last 7 years since 1994 up to now is in a good agreement with the prediction of the phenomonological model based on the neutrino registration in Homestake taken from 1971 to 1991. The correlation between neutrino flux counting rate and diameter and their anti-correlation with magnetic field are demonstrated. Comparison with the perturbations of the geomagnetic field has been performed.

The observations of solar oscillations by Ground Network GONG have been used to study the distribution of the acoustic power of radial and dipole modes. The data sets of about 2500 days long have been used to verify the variability of p-mode power distribution in time. The results confirm that the "quantization" of distributions takes place with the concentration of the power on several levels stable in time.

The observations of solar Global Oscillations by Ground Network GONG have been used to study spherical degree l = 0 - 8 modes. The set of the mode frequencies is presented. The properties of oscillations are discussed.

Using 1692-d GONG time series we measured the mean rotational splittings of solar acoustic modes of spherical degrees l = 0 - 8 with very high precision. We discuss the results of the inversions of the density, sound speed, and the rotation rate in the deep solar interior.

On the base of 1692-d time series of GONG data we investigated the correlation between radial and dipole solar acoustic mode power and between them and the solar activity.

Using GONG observations we investigated the distributions of running mean power of dipole doublets of solar p-modes for window size from 2 to 200 days. The results are similar to those obtained for the radial modes.

The GONG time series, 1692 days long, is used for the evaluation of the low-l (l = 0 - 8) p-mode parameters. The set of the mode frequencies, the most comprehensive up to date in radial orders n, is presented. The variations of mode profiles with time are discussed.

Using 1332-d time series of GONG data we investigated again the correlation of low-C solar acoustic mode power with solar activity. The correlation with CME daily event number remains very high. There is also the correlation with sunspot number at the same significance level. The significance of the crosscorrelation between different radial modes increased with increase of the incorporated statistics. The structures of several consequent large pulses in the power time series, evidenced by the auto-correlation analysis continue to appear also in the new data with nearly the same quasi-periodicities as were seen in 1010-d time series.

The set of the frequencies of solar acoustic modes with l = 0 - 6 and broad range of radial orders, including the lowest ever reported, was measured using 1260 days of GONG data. The comparison with other measurements and model frequencies is presented.

Using GONG observations we investigated the distributions of running mean power of radial solar p-modes for window size from 2 to 200 days. The results show the complicated character of the excitation sources. The possibility to formulate the inversion procedure for excitation source dependence on the radius, similar to well known inversions of sound speed and angular velocity, is discussed.

We determined the mean rotational splittings of solar oscillations of low spherical degrees l = 1 - 6 from 1260 days of GONG data. The length of the data set permitted to achieve a high level of an accuracy and to measure the lowest radial orders ever reported. The preliminary results of the inversion of the rotation rate of the Sun's deep interior confirm the value of equatorial angular velocity in the central regions higher than at the surface, and the presence of a local minimum in its profile near 0.18R..

The comparison of the power, accumulated by the different components of the same rotationally split l = 1 multiplet, is done using the spectra of 940 consecutive days of GONG. Current theoretical understanding of p-mode excitation and damping leads to the expectation of Lorentzian shapes for each component of a mode with the same parameters. Peak power density and line-width, and consequently the total component power are expected to be equal for all components of the multiplet. We discuss the significance and possible reasons of long-term departures from equality between the m = +/-1 components of the dipole solar p-modes.

We study the profile parameters of each radial order n solar oscillations of low spherical degrees l = 0, 1, 2, 3, 4, using 830 day time series obtained by GONG. The frequency and other parameters of a mode with fixed l, n, m have been determined from different data sets, where this mode is well visible. For each radial order the rotational splitting has been calculated from all possible combinations, providing the statistical estimation of this value and the standard error bar. The mean splitting for given l was calculated too, assuming its independence on the mode frequency in the first approximation.Frequencies and splittings of lowest degree modes (l = 1 - 4), combined with the data previously found bg GONG team for higher spherical degrees, have been used to infer the variation of the angular velocity of the Sun with radius. By using the SOLA helioseismic inversion procedure and the accurate GONG data we have been able to obtain averaging kernels confined to the solar core, thus giving a measure of the rotation rate of the Sun's deep interior. We speculate on the possible interpretation of the obtained results.