1999A&A...342L..13I

We use an updated self-consistent kinetic/gasdynamic model of the solar wind/interstellar flow interaction to compute the Lyman-α absorption by hydrogen atoms of both interstellar and solar origin generated in the heliospheric interface. We apply this model to the direction of the star Sirius. We show that the neutralized, compressed solar wind from the heliosheath explains the extra absorption at positive redshifts observed in the Lyman-α line with the HST/GHRS. This removes the need for the interstellar hot gas previously proposed to explain this extra absorption. We also show that extra absorption in the blue wing can possibly be explained by H atoms formed in an astrosphere around Sirius, providing the stellar wind is at least as massive and fast as the solar wind.