3400-7500 Å Energy Distribution and JHKLM Photometry of Solar-Type Stars
Irina N. Glushneva (Sternberg Astronomical Institute, University of Moscow)


4. Conclusion

For 8 stars of spectral types G1.5-G3 (BS 483, BS 7503, BS 4030, BS 6060, BS 88, HD 213575, BS 7504, and BS 7783) energy distributions in the range 3400 - 7500 AA and JHKLM photometry were produced.

The energy distribution data were compared with solar energy distribution using three sets of the most reliable data. The comparison showed that energy distribution in the spectra of BS 483, BS 6060, BS 7783 and HD 213575 are the nearest to the solar energy distribution in the range 3400 - 7500 AA. Synthetic color B-V indices calculated on the basis of obtained energy distribution data are in very good agreement with observed B-V indices of WBVR photometric system realized at Tien'-Shan' Highmountain Station. The mean difference of the synthetic and observed B-V indices is only 0.m006.

Comparison of the observed infrared indices of stars V-J, V-H, V-K, V-L, and V-M with corresponding solar indices shows that scattering in the color indices of stars around the Sun, according to the data obtained by different authors, exceeds the accuracy of infrared measurements declared by various authors.

The J-H, J-K,J-L and J-M indices of the observed stars are nearer to the solar ones obtained by means of the comparison with solar type stars than to the synthetic solar indices.

Discrepancies between observed infrared stellar color indices and synthetic solar ones may be due to the differences of response curves used in the process of integrating and realized in observations. So direct determinations of color indices of the Sun in the JHKLM photometric system are important.

It is interesting to note that according to our observations, J-K, J-L, J-M of 16 Cyg A and 16 Cyg B are equal and the difference between their J-H is 0.m02.

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