Spectral energy distributions and physical parameters of the atmospheres of main-sequence A stars with infrared excesses - Comparison with normal stars

Details Spectral energy distributions and physical parameters of the atmospheres of main-sequence A stars with infrared excesses - Comparison with normal stars Spectral energy distributions and physical parameters of the atmospheres of main-sequence A stars with infrared excesses - Comparison with normal stars

Aug 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997azh....74..591g&link_type=abstract

Astronomicheskij Zhurnal, vol. 74, p. 591

Astronomy and Astrophysics

Astronomy

Main Sequence Stars, Stellar Atmospheres, Spectral Energy Distribution, Atmospheric Physics, Infrared Stars, Stellar Spectra, Stellar Magnitude, Physical Properties, Infrared Astronomy Satellite, Ubv Spectra, Stellar Temperature

Scientific paper

For eight stars with infrared excesses greater than 0.5 m in the IRAS bands, we obtained the energy distribution over the range 3200-7600 A and measured their infrared JHKLM magnitudes. Similar observations were performed for 21 stars of various subclasses of the spectral type A with excesses no greater than 0.3 m. Based on the energy distribution derived from the response curves of the photometric UBV and WBVR systems, we computed the synthetic B-V color indices, which are in good agreement with the photometric observations. A comparison of the normalized energy distribution in the spectra of A stars with infrared excesses greater than 0.5 m in the IRAS bands and the mean energy distribution for stars of the corresponding subclasses shows that the maximum difference does not exceed 10 percent both in the ultraviolet (3200-4000 A) and in the near infrared (up to 7600 A). In all of the stars studied, we detected no excesses in the JHKLM bands that were greater than the accuracy of our measurements. Using the method of infrared fluxes and comparing the observed energy distribution with theoretical models of Kurucz, we determined the effective temperatures and angular diameters of the stars. For three stars, we estimated the parameters of their dust shells.

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