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The high-mass accreting binary Cyg X-3 is distinctly different from low-massX-ray binaries (LMXBs) in having powerful radio and $\gamma$-ray emitting jetsin its soft spectral state. However, the transition from the hard state to thesoft one is first associated with quenching of the hard-state radio emission,as in LMXBs. The powerful soft-state jets in Cyg X-3 form, on average, $\sim$50d later. We interpret the initial jet quenching as due to the hard-statevertical magnetic field quickly diffusing away in the thin disc extending tothe innermost stable circular orbit in the soft state, or, if that field isproduced in situ, also cessation of its generation. The subsequent formation ofthe powerful jets occurs due to advection of the magnetic field from the donor.We find this happens only above certain threshold accretion rate associatedwith appearance of magnetically driven outflows. The $\sim$50 d lag is of theorder of the viscous timescale in the outer disc, while the field advection ismuch faster. This process does not happen in LMXBs due to the magnetic fluxesavailable from their donors being lower than that for the wind accretion fromthe Wolf-Rayet donor of Cyg X-3. In our model, the vertical magnetic field inthe hard state, required to form the jets both in Cyg X-3 and LMXBs, is formedin situ rather than advected from the donor. Our results provide a unifiedscenario of the soft and hard states in both Cyg X-3 and LMXBs.

Jets in the soft state in Cyg X-3 caused by advection of the donor magnetic field and unification with low-mass X-ray binaries