The evolutionary stellar population synthesis method is a link between the studies of stellar and galaxy. The integrated spectra of the stellar population as the most important output of the evolutionary stellar population synthesis model has often been used for the analysis of galaxies spectra. The calculation of the integrated spectra is based on the interpolated calculation of stellar spectra, the stellar spectral library isused for this kind of interpolated calculation. The empirical stellar spectral library avoids the defects of the theoretical stellar spectral library and has been widely used for the interpolated calculation of stellar spectra, but the irregular distribution of stars in the empirical library makes the interpolated calculation difficult. We build a new stellar spectral interpolator based on the radial basis function network and use it for theinterpolated calculation of the stellar spectra based on the empirical spectral library. For our spectral interpolator, we constrain the radial basis function by the local density of stars in the spectral library, thus, the spectral interpolator has better applicability to the different libraries. At last, we use our spectral interpolator to calculate the integrated spectra of the YunnanIII model based on the empirical stellar spectral library. Moreover, as an application of the evolutionary stellar population synthesis model, we build a cluster model, which can be used to create a template library for fitting the cluster observation data. The model is based on the simple idea that different stellar population parameters will affect the mass distribution of stars in a cluster, which in turn affects the distribution of stars in the cluster. For this model, we use Monte-Carlo methodto simulate the stellar population comprising binary stars and get the photometric and spectroscopic results of the stars in a stellar population, then we use the King-Michie model to give the distribution of stars in different radius of the model cluster, and get the integrated photometric and spectroscopic results in different radius of the model cluster. This model can help to get the basic parameters of the stellar population in the cluster.
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