Ejection of the inner accretion disk in GRS 1915+105: The magnetic rubber-band effect

We examine theoretically the behaviour of the inner accretion disk in GRS 1 915+105 when soft X-ray dips are present in the X-ray light curve. We assum e the presence of a radial shock in the accretion disk, as in some of the T wo Component Advective Flow (TCAF) solutions. We discuss the behaviour of t he flux tubes inside a TCAF (which we name Magnetized TCAF or MTCAF model f or brevity) and compare various competing forces on the flux tubes. In this MTCAF model, we find that the magnetic tension is the strongest force in a hot plasma of temperature greater than or similar to 10(10) K and as a res ult, magnetic flux tubes entering in this region collapse catastrophically, thereby occasionally evacuating the inner disk. We postulate that this mag netic "rubber-band" effect induced evacuated disk matter produces the blobb y components of outflows and IR/radio jets. We derive the size of the post- shock region by equating the time scale of the Quasi-Periodic Oscillations to the infall time of accreting matter in the post-shock region and found t he shock location to be similar to 45-66 r(g). We calculate the transition radius r(tr), where the Keplerian disk deviates into a sub-Keplerian flow, to be similar to 320 r(g). Based on the derived X-ray spectral parameters, we calculate the mass of this region to be similar to 10(18) g. We conclude that during the X-ray dips the matter in the post-shock region, which mani fests itself as the thermal-Compton component in the X-ray spectrum, is eje cted, along with some sub-Keplerian matter in the pre-shock region.