V 1016 Cygni and HM Sagittae - Binary stellar systems

Details V 1016 Cygni and HM Sagittae - Binary stellar systems V 1016 Cygni and HM Sagittae - Binary stellar systems

Jan 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...117..209t&link_type=abstract

Astronomy and Astrophysics, vol. 117, no. 2, Jan. 1983, p. 209-214.

Astronomy and Astrophysics

Astrophysics

51

Binary Stars, Brightness Distribution, Periodic Variations, Stellar Spectrophotometry, Stellar Systems, Ubv Spectra, Visible Spectrum, Continuous Spectra, Cool Stars, Emission Spectra, Hot Stars, Infrared Spectra, Spectral Energy Distribution, Stellar Envelopes

Scientific paper

During the period from 1978 to 1981, systematic photometric observations of the peculiar objects V 1016 Cyg and HM Sge in the UBVRJHKLMN system were carried out. They have shown that the IR brightness of V 1016 Cyg continues to undergo the variations, first seen by Harvey in the early seventies, having an amplitude ΔK ≈ 1m and a characteristic time scale of about 450d. Similar variations in the IR light were observed in HM Sge as well. In September 1980, photometric observations of V 1016 Cyg and HM Sge were carried out along with spectrophotometric ones at wavelengths ranging from 3400 to 7500 Å with Δλ = 50 Å, the results of these observations are presented. It is shown that the above-mentioned features of the photometric behavior of these stars along with their spectral characteristics cannot be explained in terms of the model of a single star being at the stage of planetary nebula formation. The presence of a cool stellar component in these systems is corroborated by the energy distribution pattern in the infrared range, that has undergone significant changes in V 1016 Cyg over the past ten years. The appearance of cool-star emission against the background of dust envelope emission in the V 1016 Cyg and HM Sge systems seems to be due to the scattering and evaporation of the dust particles surrounding primarily cool stars under the effect of the hard UV radiation of hot outburst stars.

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