We have modeled the spectral energy distribution of the radio-luminous OH/IR star 26.5+0.6 as a function of pulsation phase using standard radiative transfer techniques but with more self-consistent input parameters based partly on pulsation model calculations. The changes in spectral shape and overall intensity are easily explained in terms of the radial movement of the dust condensation radius with the changing luminosity of the star. The derived amplitude of the bolometric light curve is only 1.2 mag, considerably less than expected.
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- Infrared: sources
- Stars: circumstellar shells
- Stars: long-period variables
- Stars: pulsation