2001NewA....6..403Z

The spectrum of HD46223 was established from the optical to the far UV and normalized by the spectrum of a non-reddened star of same spectral type. The resulting spectrum is separated into two components. One is the direct starlight. The second is an additional component of light scattered at small angles. In the optical the spectrum is dominated by direct starlight which decreases exponentially due to the linear extinction ∝e-2E(B-V)/λ. Scattered light begins to be noticeable in the near-UV. The near-UV rise of the scattered light is interrupted in the 2200Å bump region. The wavelength dependence of the scattered light is established in the far-UV, where scattered light dominates the extinction curve. A 1/λ4 dependence is found, proving the presence of grains small compared to UV wavelengths. The mathematic expressions of the different components mentioned above give a good fit to the extinction curve in the direction of the star. On a mathematic standpoint the fit can be completed by a Lorentzien for the 2200Å bump region. The physical interpretation of the bump may be more difficult to achieve since the paper shows the possibility that only scattered light is extinguished in the bump region. Consequences for the grain size distribution which is necessary to explain the different aspects of scattering in interstellar clouds, for the value of RV, and problems raised by this interpretation of the spectrum of HD46223, are considered at the end of this paper.