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\title{ON THE SOLAR SYSTEM BODIES OBSERVATIONS IN THE AIST-PROJECT}
\author{M.S.CHUBEY\\
Pulkovo Observatory,\\
Pulkovskoye Shosse 65/1, St.-Petersburg, 196140, Russia \\
e-mail: mchubey@gaoran.spb.su \and M.G.VYDREVICH \\
Research Institute "ELECTRON",\\
Prosp.M.Toreza 68, St.-Petersburg, 194223,  Russia \\
e-mail: mgv@eal.spb.su}
\date{}
\begin{document}
\maketitle

{\sl ABSTRACT.} In accordance with the scanning law in the AIST space
project every celestial object brighter $V\approx 18^m$ can be observed
$\approx 160~ times$ during three years. Two mosaics from 28 CCDs
$800\times800~$ with pixel size $16\times16 \mu m^2$ (or $1.32^{\prime\prime}
\times 1.32^{\prime\prime}$) in focal planes of two telescopes are planned
to be used. We assess that accuracy of the astrometric position vector
$\sigma_r$ from the {\sl Time Delay and Integration (TDI)} mode single
transit through one CCD-array for nonstellar shape object in the range
of magnitudes from $V=6^m$ to $V=16^m$ can be acquired on the level
of 0.02 of the pixel size.

Preliminary the astrometric and photometric limits of
values from this modelling can be summarized as:\\
\centerline{$\sigma_r \leq 0.03^{\prime\prime}$,~~ $\sigma_v \leq 0.02^m$.}
We use the realistic signal acquisition model and discuss the problem
of detecting of the Solar system bodies images in {\sl TDI} mode.

\end{document}
