Infrared light curves of the contact binary 44 i Bootis

Details Infrared light curves of the contact binary 44 i Bootis Infrared light curves of the contact binary 44 i Bootis

Feb 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....94..350b&link_type=abstract

Astronomy and Astrophysics, vol. 94, no. 2, Feb. 1981, p. 350-358.

Astronomy and Astrophysics

Astrophysics

6

Binary Stars, Infrared Radiation, Light Curve, Stellar Luminosity, Stellar Spectrophotometry, Fourier Analysis, Mass Ratios, Stellar Atmospheres, Stellar Mass, Stellar Temperature

Scientific paper

Accurate infrared light curves (λ=2.25μm) are given for the W UMa type system 44 ι Bootis, three of which were secured within a single night. The coverage of a period of the variable is made as complete as possible with typically more than one hundred individual observations. This program was initiated in an attempt to determine the source for perturbations of the visible light curves of ι Bootis published by many authors. It fell short of its aim since the binary proved to be in a low activity phase of its history at the time of the observations (1978 March).' Maxima are very nearly equal and asymmetries of minima are shown to be at a very low level where they merge in with noise and uncertainties on the atmospheric correction. On the other hand, Fourier cosine terms which are predicted by the standard model for close or contact binary, are detected up to the eighth overtone. The photometric solution of the system is studied through new multicolour photometric observations (visual binary ADS 9494 whose component A cannot be separated for the moment). We adopt the spectral energy distribution of a F8V star for ι Boo A together with that of a G2III star for ι Boo (B+ C) and ΔV= 0.4 mag for the yellow magnitude difference between A and B + C, which gives the better fit to the observations. Luminosities and radii of the eclipsing system components are however class V data and they are strong arguments against the adoption of a K2V spectral energy distribution. Expansion of a common low pressure atmosphere through the inner lagrangian surface is tentatively suggested as a possible explanation of the luminosity class discrepancy. A forthcoming paper will be devoted to the determinations of the elements of 44 ι Bootis (W UMa system) by the method of light curve synthesis.

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