Planetary system around Vega
  We applied our earlier numerical method to compute the thermal emission from a dusty resonant structure around Vega and compared the new observational evidence for a ring arc at 95 AU near Vega with our modeling. Our high resolution simulations indicate that Vega may have an outerm ost 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. Radii of the observed clumps (and planet's orbital radius) may be smaller, e.g. ~60-75 AU. In this case the planet stays approximately on the line between the two possible positions above. From our modeling we make following conclusions: 1.Dust clumps rotate around Vega exactly wi th the planet orbital speed, 0.6-1.2 deg/year, as function of orbital radius of parent planet. 2. Orbital radius of the planet is approximately the same as the orbital radius of clumps (90-100 AU from observation by Koerner, Sargent & Ostroff, 2001 or 60-75 AU from observation by Wilner, Holman, Ho & Kuchner, 2002). 3. The most dense clump is ahead of the planet in the direction of the orbital motion. 4. The orbit of the planet may be circular or with a small eccentricity. 5. Absence of dust i n the inner part of Vega planetary system is a signature of inner planet(s) with orbital radii <50-60 AU. 
N. Gorkavyi, T. Taidakova (Schafer Corp.)