By Y. Ryabov, G. Yankovsky
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A few systems (primarily those discovered in the Magellanic Clouds) are similar in many respects to the spectrum of UV Aur, which shows the strong CN bands visible in carbon stars. 12; Baldwin, Frogel, and Persson 1973; Kenyon and Gallagher 1983). If the late-type stars in symbiotics are all class III giants, then it is very straightforward to measure their spectral types (and therefore their effective temperatures). Allen adopted this viewpoint, and obtained spectral types for a large fraction of southern symbiotic stars.
On the other hand, systems containing red giants losing mass via a stellar wind are predicted to be luminous radio sources. , Watanabe and Kodaira 1978), ^5GHz^l00AU for the hot stellar sources discussed earlier (r/,=10 5 K, R=0A RQ). Such a nebula is optically thick at v~15 GHz and should have Sv = 2 mJy at v = 5 GHz, well within the range of the VLA. 4 Summary The simple model developed in the preceding pages proposes that symbiotic stars are binaries composed of (i) a late-type giant star, (ii) a hot component, and (iii) an ionized nebula.
Typical values of a for optically thin and optically thick constant density nebulae are - 0 . 0, respectively. It is probably more realistic to suppose that the nebula has a density profile given by nccr~2, appropriate to the equation of continuity at constant outflow velocity. 2. 5 x 10"6(v/10 km s~l)(S6 cm/1 Jy)3/4 (d/l kpc)3/2 M o yr" 1 . 3, and the results do not cluster around any of the expected values. 6. 6, rather than larger as observed. 6, and derived values for their mass loss rates also appear in the Table.
An Elementary Survey of Celestial Mechanics by Y. Ryabov, G. Yankovsky