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High inclination black hole X-ray binaries exhibit blueshifted ionizedabsorption lines from disk winds, whose launching mechanism is still in debate.The lines are predominantly observed in the high/soft state and disappear inthe low/hard state, anti-correlated with the jet. We have tested if the thermalwinds, which are driven by the irradiation of the outer disk by the X-rays fromthe inner disk, can explain these observed properties or whether we need amagnetic switch between jet and wind. We use analytic thermal-radiative windmodels to predict the column density, ionisation parameter and velocity of thewind given the broadband continuum shape and luminosity determined from RXTEmonitoring. We use these to simulate the detailed photo-ionised absorptionfeatures predicted at epochs where there are Chandra high resolution spectra.These include low/hard, high/soft and very high states. The model was found towell reproduce the observed lines in the high/soft state, and also successfullypredicts their disappearance in the low/hard state. However, the simplestversion of the thermal wind model also predicts that there should be strongfeatures observed in the very high state, which are not seen in the data.Nonetheless, we show this is consistent with thermal winds when we includeself-shielding by the irradiated inner disk atmosphere. These results indicatethat the evolution of observed wind properties in different states duringoutbursts in H 1743-322 can be explained by the thermal wind model and does notrequire magnetic driving.

Application of the Thermal Wind Model to Absorption Features in the Black Hole X-ray Binary H 1743-322