Abstract
The photometric U orbital variations of the symbiotic binary AG Peg, caused by occultation of a bright gaseous region by the M giant in this system, are used to determine the geometry of this region whose existence is explained in the framework of the colliding winds model. The emission of the bright region varies and a particular value of its mean density of 2–3 1010 cm-3 has been derived. The causes for the irregular variations of the light in the orbital minimum and maximum are discussed. It is also obtained, when the mass-loss rate of the hot companion of the system decreases to about 5 10-10 Ms ⊙ yr-1, this bright region will disappear.
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Tomov, N., Tomova, M. A Colliding-Winds Interpretation of the U Orbital Variation of the Symbiotic Binary AG Pegasi. Astrophysics and Space Science 278, 311–317 (2001). https://doi.org/10.1023/A:1013126728911
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DOI: https://doi.org/10.1023/A:1013126728911