The Spectral Energy Distributions Of Binary and Multiple Systems:

The study of stars from a spectrophotometrical observational scope is a deep-rooted science, and it has been strengthened by the development of the theoretical atmospheric models by different scientists, which made it possible to determine a specific stellar elements like Teff, Log g, element abundance,etc... .

In our study we are focusing on the study of spectral energy distributions of binary and multiple stars. Those which has been selected from our Speckle Interferomtric list, and which haven't been resolved but by means of speckle interferometric or speckle masking methods using big telescops like BTA 6-meter telescope of SAO RAS.

Since we need to cover as much as possible of the spectra of the systems, we use a low resolution gratings ( 325 grooves/mm, 5.9Å /px reciprocal dispersion) within the UAGS spectrograph at the Cassegrain focus of the Carl Zeiss Jena (Zeiss-1000) 1-meter telescope of SAO RAS. And this enables us to get the required wide spectra.

The resultant spectra along with the results of speckle interferomtric observation will be used to build the models for the systems, and for this we use the Kurutcz theoretical models. As a result we get Teff, Log g , element abundance,and a theoretical spectral energy distribution for each of the components ( See figures 1 and 2) (for more information see publications).

Figure 1: Fitting between the observational entire SED of the subsystem 41Draconis with that calculated using the drawn model atmosphere parameters of each component.

Figure 2: Fitting between the observational entire SED of the subsystem 40Draconis with that calculated using the drawn model atmosphere parameters of each component.