Infrared observations of V 1016 Cygni

Details Infrared observations of V 1016 Cygni Infrared observations of V 1016 Cygni

Apr 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982azh....59..307i&link_type=abstract

(Astronomicheskii Zhurnal, vol. 59, Mar.-Apr. 1982, p. 307-311.) Soviet Astronomy, vol. 26, Mar.-Apr. 1982, p. 187-189. Transla

Astronomy and Astrophysics

Astronomy

8

Infrared Spectra, Peculiar Stars, Astronomical Photometry, Binary Stars, Cygnus Constellation, Spectrum Analysis, Stellar Envelopes

Scientific paper

Photometric observations of V 1016 in the UBVRJHKLMN system were made during 1978-1980. It was shown that the star's optical brightness (UBVR) remained constant during this time with an accuracy near 0.2 mag, whereas the IR emission underwent oscillations with an amplitude near 1 mag and a characteristic time of about 500 days. The shape of the IR spectrum of V 1016 Cyg at maximum IR brightness clearly indicates that presence of a cool component surrounded by a dust shell with a mass of about 0.0000003 solar mass in this system. An outer dust shell, surrounding both components and radiating in this IR region, has an inner radius of nearly 10 to the 15th cm and a mass of about 1 millionth solar mass. The luminosity of the hot star exceeds the luminosity of the cool one at its maximum brightness by almost four times and evidently comprises no less than 10 to the 38th ergs/sec.

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