Non-spherical Mass Outflow from RS Ophiuchi During its 2006 Outburst

We present results of our modeling of the H alpha line profile during the 2006 outburst of RS Oph. At day 1.38 it was possible to fit the very broad component of the Ha by a bipolar wind model. The model corresponds to a very fast acceleration of the wind particles, and the line luminosity of similar to 2900(d/1.6 kpc)(2) L-circle dot, to a mass-loss rate of similar to (1 - 2) x 10(-4) M(circle dot)yr(-1). During days 10 - 30 the broad component shrank to FWZI similar to 1800 km s(-1). It could be associated with expanding ring and its satellite components at similar to +/- 2 430 km s(-1) with bipolar jets. Later observations made at; clay 57 and 209 indicated a decrease in both the mass-loss rate (similar to 1 x 10(-5) -1 x 10(-6) M(circle dot)yr(-1)) and the wind acceleration. During the quiet, phase, emission bumps observed sporadically in the line wings could reflect clumpy ejections by the central star.