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We present results of our modeling the H-alpha line profile along the 2006 RSOph outburst. At day 1.38 the very broad component of the H-alpha profile waspossible to fit by a bipolar wind model. The model corresponds to a very fastacceleration of the wind particles, and the line luminosity of about 2900(d/1.6 kpc)^2 solar luminosities to the mass-loss rate of around (1-2) x 10E-4solar masses per year. During days 10-30 the broad component shrank to FWZI =1800 km/s. It could be associated with expanding ring and its satellitecomponents at about +/- 2430 km/s with bipolar jets. Later observations made atday 57 and 209 indicated a decrease in both the mass-loss rate (1xE-5 - 1xE-6solar masses per year) and the wind acceleration. During the quiet phase,emission bumps observed sporadically in the line wings could reflect clumpyejections by the central star.

A non-spherical mass outflow from RS Oph during its 2006 outburst