Abstract
We examine a binary model for symbiotic stars to account for their radio properties. The system is comprised of a cool, mass-losing star and a hot companion. Radio emission arises in the portion of the stellar wind photo-ionized by the hot star. Computer simulations for the case of uniform mass loss at constant velocity show that when less than half the wind is ionized, optically thick spectral indices greater than +0.6 are produced. Model fits to radio spectra allow the binary separation, wind density and ionizing photon luminosity to be calculated. We apply the model to the symbiotic star H1–36.
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© 1985 D. Reidel Publishing Company
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Taylor, A.R., Seaquist, E.R. (1985). Radio Emission from Symbiotic Stars: A Binary Model. In: Hjellming, R.M., Gibson, D.M. (eds) Radio Stars. Astrophysics and Space Science Library, vol 116. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-5420-5_22
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DOI: https://doi.org/10.1007/978-94-009-5420-5_22
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-8892-3
Online ISBN: 978-94-009-5420-5
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