  The present sequence of two articles reports on a custom-built toolkit
implementing a technique similar to multi-directional medical tomography to
simulate and visualize the composite 3D structure of winds from hot close
double stars. In such hot binaries, the light sources scanning and probing the
composite wind volume are the bright "surfaces" (photospheres) of the
individual stars. Then, as the Keplerian orbit is traced out and the geometry
presented to the observer varies, each star constitutes an analyzer upon its
companion's wind. In contrast to medical tomography, however, these targets are
too far to be resolved spatially so we resort to modeling the ultraviolet (UV)
spectral lines of certain wind ions (e.g., N+4, Si+3, C+3) whose shapes vary
with Keplerian phase as the stars revolve around their common centre of mass.
The flagships of the toolkit are the Spectrum Analyzer and Animator (SA 2 ) and
the Binary 3D Renderer (B3dR). The SA 2 is the subject of the present article
(paper I). It automates (a) the derivation of light curves from the observed
spectra and (b) the generation of synthetic binary wind-line profiles which
reproduce the morphologies and variabilities of the observed wind profiles. The
second tool, the B3dR is discussed in paper II.
