Indirect imaging of active RS CVn stars
The RS CVn system HR1099 has been monitored over its orbital period to study spectroscopic variability in photospheric lines and in Ha. The observations were made at the CAT 1.4m ESO telescope with the Coude CES spectrometer and reticon, which permit a resolution of 105 and high S/N. The information provided by the variability of profiles, together with the limits of the Doppler imaging methods are also presented. Profiles are calculated with rotational broadening of immaculate and spotted stars. A line synthesis code including a model for the inhomogeneous temperature distribution of the primary star allowed us to calculate a series of spectra at different orbital phases. Different inversion algorithms were applied to test the image reconstruction of HR1099, showing the role of such constraints as chi-square adjustment of the spectra and maximum entropy of the input image.
KeywordsStellar Surface Synthetic Spectrum Orbital Phasis Primary Star Photospheric Line
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- Cameron & Horne, in Cool Stars, Stellar Systems and the Sun, eds. M. Zeilik and D.M. Gibson, p. 205.Google Scholar
- Crivellari et al, 1987, Astron. Ast., 174, 127.Google Scholar
- Fekel F., 1983, Astroph. J. 268, 274.Google Scholar
- Foing et al, 1988, in preparation.Google Scholar
- Gondoin P., 1986, Astron. Ast. 160, 73.Google Scholar
- Jankov S. 1987, DEA Univ Paris VII/LPSP.Google Scholar
- Jankov S., Foing B., 1987,in preparation.Google Scholar
- Rodono M. et al. 1986, Astron. Ast., 165, 135.Google Scholar
- Vogt S. and Penrod, 1983, P.A.S.P., 95, 565.Google Scholar