Photometric and spectrophotometric observations of CH Cygni in the period 1978-1982

Details Photometric and spectrophotometric observations of CH Cygni in the period 1978-1982 Photometric and spectrophotometric observations of CH Cygni in the period 1978-1982

Jun 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...135..325i&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 135, no. 2, June 1984, p. 325-329.

Astronomy and Astrophysics

Astronomy

21

Red Giant Stars, Stellar Spectrophotometry, Ubv Spectra, Visual Photometry, Bolometers, Infrared Astronomy, Radiant Flux Density, Spectra, Spectral Energy Distribution, Stellar Envelopes, Stellar Luminosity, Stellar Models

Scientific paper

The authors present results obtained from photometric (in the UBVRJHKLMNQ system) and spectrophotometric (in the range of 0.33 to 1.1 μm) observations of CH Cygni, carried out in the period 1978 - 1982. The maximum UV emission of the star was observed in the spring of 1982. However, the bolometric luminosity of the UV source never exceeded 10% of that of the cool star, classified as M6III. The relatively small bolometric luminosity of the hot source does not enable to reject the single-star model with a hot spot in the atmosphere of the red giant for explaining the phenomenon of CH Cyg. In the middle of 1977, the luminosity of the hot radiation source increased, at the same time, the flux from the circumstellar dust envelope started growing. A possible explanation is that the emission of the hot source appearing against the background of the red giant, inevitably has a pronounced effect upon the envelope luminosity.

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