Add to ORKG174-177In the present 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 possible to organize the luminosity of stars from different spectral classes. 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. The hydrogen Balmer absorption ...
Context.Profiles of hydrogen lines in stellar spectra are determined by the properties of the hydro...
This work communicates a review on Balmer series hydrogen beta line measurements and applications fo...
International audienceA new approximate method for calculating the opacity of the atomic lines in th...
A linear relationship in stellar optical spectra has been found by using the spectroscopical method ...
231-236The new intensity formula in optical emission spectroscopy for the use of ions has been deve...
The spectrum of light emitted by a star holds deep secrets about it. In particular it gives the temp...
The hydrogen Lyman-α (Lyα) line, a major source of ionization of metals in the circumstellar disks o...
As a preliminary step to derive the luminosity function the underlying hypothesis involved in the me...
The University of Michigan programme for the determination of the abundances of the elements in hot ...
Photometric measures of absorption line intensities in the spectra of forty-five B stars are given. ...
It Is shown that the photoelectric (B-V) colors of the metallic line stars are correlated with the s...
The importance of measuring absolute energy distributions of stars was realized more than thirty yea...
International audienceThe spectrum emitted by a star is determined by the conditions where the photo...
In this paper the present position concerning the meaning of spectral type among the O- and B-stars ...
Investigation of astrophysical plasmas, such as stellar atmospheres, require both knowledge of atomi...
Context.Profiles of hydrogen lines in stellar spectra are determined by the properties of the hydro...
This work communicates a review on Balmer series hydrogen beta line measurements and applications fo...
International audienceA new approximate method for calculating the opacity of the atomic lines in th...
A linear relationship in stellar optical spectra has been found by using the spectroscopical method ...
231-236The new intensity formula in optical emission spectroscopy for the use of ions has been deve...
The spectrum of light emitted by a star holds deep secrets about it. In particular it gives the temp...
The hydrogen Lyman-α (Lyα) line, a major source of ionization of metals in the circumstellar disks o...
As a preliminary step to derive the luminosity function the underlying hypothesis involved in the me...
The University of Michigan programme for the determination of the abundances of the elements in hot ...
Photometric measures of absorption line intensities in the spectra of forty-five B stars are given. ...
It Is shown that the photoelectric (B-V) colors of the metallic line stars are correlated with the s...
The importance of measuring absolute energy distributions of stars was realized more than thirty yea...
International audienceThe spectrum emitted by a star is determined by the conditions where the photo...
In this paper the present position concerning the meaning of spectral type among the O- and B-stars ...
Investigation of astrophysical plasmas, such as stellar atmospheres, require both knowledge of atomi...
Context.Profiles of hydrogen lines in stellar spectra are determined by the properties of the hydro...
This work communicates a review on Balmer series hydrogen beta line measurements and applications fo...
International audienceA new approximate method for calculating the opacity of the atomic lines in th...