Optical and infrared photometry of TX Canum Venaticorum

Details Optical and infrared photometry of TX Canum Venaticorum Optical and infrared photometry of TX Canum Venaticorum

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983pazh....9...36t&link_type=abstract

(Pis'ma v Astronomicheskii Zhurnal, vol. 9, Jan. 1983, p. 36-40) Soviet Astronomy Letters (ISSN 0360-0327), vol. 9, Jan.-Feb. 19

Astronomy and Astrophysics

Astronomy

3

Giant Stars, Infrared Photometry, Infrared Spectra, Main Sequence Stars, Stellar Spectrophotometry, Variable Stars, Visible Spectrum, Light Curve, Near Infrared Radiation, Radiant Flux Density, Stellar Color, Stellar Magnitude, Ubv Spectra

Scientific paper

The results of four years of UBVRJHK photometric measurements of the object TX CVn over a wide region of the spectrum, from 0.36-2.2 microns, are presented. In the optical region, the star has been fading and simultaneously becoming redder: the amplitude of the light variation has been roughly 0.6 m in U and 0.2 m in R. In the spring of 1979 the near-infrared emission was highly unstable, with the brightness fluctuations on successive nights reaching about 0.4 m. Comparison of color indices against normal indices shows that, beginning with the R band at 0.7 microns, the radiation of TX CVn comes chiefly from the cool component. To within + or - 1 subtype, in 1981 the radiation of the system was that of a normal K5 giant and a B9 main sequence star. The rest of the time excess optical emission was present, probably coming from a hot spot. The K-band flux density of the K5 giant implies a distance to TX CVn of about 1.1 kpc.

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