  High inclination black hole X-ray binaries exhibit blueshifted ionized
absorption lines from disk winds, whose launching mechanism is still in debate.
The lines are predominantly observed in the high/soft state and disappear in
the low/hard state, anti-correlated with the jet. We have tested if the thermal
winds, which are driven by the irradiation of the outer disk by the X-rays from
the inner disk, can explain these observed properties or whether we need a
magnetic switch between jet and wind. We use analytic thermal-radiative wind
models to predict the column density, ionisation parameter and velocity of the
wind given the broadband continuum shape and luminosity determined from RXTE
monitoring. We use these to simulate the detailed photo-ionised absorption
features predicted at epochs where there are Chandra high resolution spectra.
These include low/hard, high/soft and very high states. The model was found to
well reproduce the observed lines in the high/soft state, and also successfully
predicts their disappearance in the low/hard state. However, the simplest
version of the thermal wind model also predicts that there should be strong
features observed in the very high state, which are not seen in the data.
Nonetheless, we show this is consistent with thermal winds when we include
self-shielding by the irradiated inner disk atmosphere. These results indicate
that the evolution of observed wind properties in different states during
outbursts in H 1743-322 can be explained by the thermal wind model and does not
require magnetic driving.
