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N.N. Gorkavyi, T.A. Taidakova (Schafer Corp.)
We have applied our numerical method (Taidakova & Gorkavyi, 1999, The Dynamics of Small Bodies in the Solar System. Kluwer, 393) to compute the thermal emission of a dusty resonant structure around Vega (Gorkavyi et al. 2000, Disks, Planetesimals, and Planets, ASP; Ozernoy, Gorkavyi, Mather & Taidakova, 2000, ApJ, 537, L147).We compared the new evidence for a ring arc at 95 AU near Vega (Koerner,Sargent & Ostroff, astro-ph/0109424, 24 Sept 2001) with our modeling. Our high resolution (10 AU) simulations indicate that Vega may have a outermost planet at a distance of 90-100 AU with coordinates near 18 35'16.25" (right ascension, B1950)and 38 44'15" (declination). Another symmetrical position, 18 35'14.75" and 38 44'32.5", of the planet is also possible. We can make a choice between these two positions after measuring of the direction of revolution of the resonant pattern, which must be have an angular velocity of 0.6 deg/yr. The mass of the outermost planet will be estimated in a future paper (from preliminary consideration, this mass may be smaller than mass of Jupiter).Our simulations in one planet approximation show that it must have the bright emission from inner symmetrical dust disk with radius <30-40 AU. From observation by Koerner, Sargent & Ostroff we can conclude that there is no disk up to very small distances. From our simulations we can predict very massive inner (<50-60 AU) planet(s), which destroyed inner circumstellar dust disk by gravitational scattering. If weak dusty inner clamps have resonant link to inner planets, they must revolve around Vega much faster than the outermost arc.
The author(s) of this abstract have provided an email address for comments about the abstract: ngorkavyi@schaferdc.com