Other
Scientific paper
Oct 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000mnras.318..381y&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 318, Issue 2, pp. 381-386.
Other
28
Techniques: Interferometric, Stars: Agb And Post-Agb, Stars: Individual: Chi Cygni, Stars: Oscillations, Stars: Variables: Other
Scientific paper
We report the direct detection of cyclic diameter variations in the Mira variable χ Cygni. Interferometric observations made between 1997 July and 1999 September, using the Cambridge Optical Aperture Synthesis Telescope (COAST) and the William Herschel Telescope (WHT), indicate periodic changes in the apparent angular diameter at a wavelength of 905nm, with amplitude 45per cent of the smallest value. The star appears largest at minimum light. Measurements made at a wavelength of 1.3μm over the same period suggest much smaller size changes. This behaviour is consistent with a model in which most of the apparent diameter variation at 905nm is caused by a large increase in the opacity of the outer atmospheric layers (which is mostly owing to titanium oxide) near minimum light, rather than by physical motions of the photosphere. The 1.3-μm waveband is relatively uncontaminated by TiO, and so much smaller size changes would be expected in this band. The latest non-linear pulsational models predict maximum physical size close to maximum light, and increases in opacity near minimum light that are too small to reproduce the diameter variation seen at 905nm. This suggests either that the phase-dependence of the model pulsation is incorrect, or that the opacities in the models are underestimated. Future interferometric monitoring in uncontaminated near-infrared wavebands should resolve this question.
Baldwin John E.
Boysen Roger C.
Haniff Christopher A.
Pearson David
Rogers James
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