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During the bright outburst in 2011, the black hole candidate IGR J17091-3624exhibited strong quasi-periodic flare-like events (on timescales of tens ofseconds) in some characteristic states, the so-called heartbeat state. From thetheoretical point of view, these oscillations may be modeled by the process ofaccretion disk instability, driven by the dominant radiation pressure andenhanced heating of the plasma. Although the mean accretion rate in this sourceis probably below the Eddington limit, the oscillations will still have largeamplitudes. As the observations show, the source can exhibit strong windoutflow during the soft state. This wind may help to partially or evencompletely stabilize the heartbeat. Using our hydrodynamical code GLADIS, wemodeled the evolution of an accretion disk responsible for X-ray emission ofthe source. We accounted for a variable wind outflow from the disk surface. Weexamined the data archive from the Chandra and XMM-Newton satellites to findthe observed limitations on the wind physical properties, such as its velocityand ionization state. We also investigated the long-term evolution of thissource, which lasted over about 600 days of observations, using the datacollected by the Swift and RXTE satellites. During this long period, theoscillations pattern and the observable wind properties changed systematically.We found that this source probably exhibits observable outbursts of appropriatetimescales and amplitudes as a result of the disk instability. Our modelrequires a substantial wind component to explain the proper variabilitypattern, and even complete suppression of flares in some states. The windmass-loss rate extracted from the data agrees quantitatively well with ourscenario.

Interplay between heartbeat oscillations and wind outflow in microquasar IGR J17091-3624