A pulsation phase-dependent dust shell model of OH 26.5 + 0.6

Details A pulsation phase-dependent dust shell model of OH 26.5 + 0.6 A pulsation phase-dependent dust shell model of OH 26.5 + 0.6

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...358..588s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 358, Aug. 1, 1990, p. 588-594. Research supported by the University of Minn

Astronomy and Astrophysics

Astrophysics

18

Energy Distribution, Energy Spectra, Infrared Stars, Mira Variables, Radiative Transfer, Stellar Envelopes, Cosmic Dust, Pulsed Radiation, Radio Stars, Stellar Luminosity, Stellar Mass Ejection

Scientific paper

The spectral energy distribution of the radio-luminous OH/IR star 26.5 + 0.6 was modeled 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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