Other
Scientific paper
Jun 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007apj...662.1231k&link_type=abstract
The Astrophysical Journal, Volume 662, Issue 2, pp. 1231-1244.
Other
7
Stars: Circumstellar Matter, Radio Continuum: Stars, Stars: Individual: Constellation Name: Ag Pegasi, Stars: Variables: Other, Stars: Winds, Outflows
Scientific paper
AG Pegasi has been observed at high angular resolution and sensitivity at the Very Large Array (VLA) at 5 GHz in four epochs between 1984 and 1991. Analysis of the radio visibilities indicate that a mass of 4.0+/-0.5×10-5 Msolar is concentrated in the inner nebula and is moving outward at a velocity of 53+/-4 km s-1 (D=600 pc assumed). In order to explain the observed morphology of the inner nebula, a new colliding winds model is derived, which includes the effects of orbital motion (CWo model). Orbital effects cannot be ignored in AG Pegasi since the orbital timescale (2.25 yr; Meinunger 1981) is short compared to the likely timescale of wind collision (symbiotic nova eruption beginning ~1850 Merrill 1959). When these effects are considered, the interaction front between binary stellar winds is wrapped into spiral walls whose density decreases outward with 1/r2. Distinctive geometries are found to arise depending on which wind dominates the interaction, the late-type wind from the symbiotic ``cool component,'' or the high-velocity wind from the ``hot component.'' Application of the CWo model to AG Peg suggests that the observed transient lobe enhancements of the inner nebula arise due to changes in the mass-loss rate from the hot component. Hot component mass-loss rates ranging between 2.1 and 6.0×10-8 Msolar yr-1 are derived. The model is also successful in reproducing the radio spectrum of the central unresolved object of the system. A position angle of -15deg+/-10deg is inferred for the orbital pole as projected on the plane of the sky.
Kenny Harold Timothy
Taylor Russ A.
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