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In this paper a linear relationship in stellar optical spectra has been found by using a spectroscopical method used on optical light sources where it is possible to organize atomic data in a linear structure. This method is based on a new intensity formula in optical emission spectroscopy (OES). Like the HR-diagram , it seems to be possible to organize the luminosity of stars from different spectral classes. From that organization it is possible to determine the temperature and density of stars using the new intensity formula. These temperature -and density values agree well with literature values. It is also possible to determine the mean electron temperature of the optical layers (photospheres) of the stars as it is for atoms in the laboratory plasmas. The mean value of the ionization energies of the different elements of the stars has shown to be very significant for each star. This paper also shows that the hydrogen Balmer absorption lines follow the new intensity formula. Keywords: stellar optical spectra, linear relationship, temperature measurements and density measurements.

Determination of temperature and density of the stars using the new intensity formula