  We present a systematic theory-motivated study of the thermodynamic stability
condition as an explanation for the observed accretion disk wind signatures in
different states of low mass black hole binaries (BHB). The variability in
observed ions is conventionally explained either by variations in the driving
mechanisms or the changes in the ionizing flux or due to density effects,
whilst thermodynamic stability considerations have been largely ignored. It
would appear that the observability of particular ions in different BHB states
can be accounted for through simple thermodynamic considerations in the static
limit. Our calculations predict that in the disk dominated soft thermal and
intermediate states, the wind should be thermodynamically stable and hence
observable. On the other hand, in the powerlaw dominated spectrally hard state
the wind is found to be thermodynamically unstable for a certain range of 3.55
<= log \xi <= 4.20. In the spectrally hard state, a large number of the He-like
and H-like ions (including e.g. Fe XXV, Ar XVIII and S XV) have peak ion
fractions in the unstable ionization parameter (\xi) range, making these ions
undetectable. Our theoretical predictions have clear corroboration in the
literature reporting differences in wind ion observability as the BHBs
transition through the accretion states Lee et al. 2002; Miller et al. 2008;
Neilsen & Lee 2009; Blum et al. 2010; Ponti et al. 2012; Neilsen & Homan 2012).
While this effect may not be the only one responsible for the observed gradient
in the wind properties as a function of the accretion state in BHBs, it is
clear that its inclusion in the calculations is crucial to understanding the
link between the environment of the compact object and its accretion processes.
