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Matteo Cantiello deleted file Observational_evidence_exists_for.tex
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Observational evidence exists for stellar wind inhomogeneities on small
and on large scales. While the latter will be discussed in Sect.~\ref{magnetic},
here we consider only small scale wind structure, or wind clumping.
In Sect.~\ref{micro}, we discussed that waves produced by the FeCZ could lead to velocity fluctuations at the stellar surface.
In order to induce wind clumping, those waves should induce density fluctuations
at the stellar surface. Through the occurrence of porosity or shifts in the ionisation
balance of the gas the mass-loss rate may be affected.
For this to happen, the amplitude of the velocity
fluctuations at the surface should be on the same order of the sound speed.
Alternatively, the velocity fluctuations
might directly affect the local mass-loss rate through the Doppler effect,
if the amplitude of the velocity fluctuations is on the same order
as the speed of the wind flow, which, at the base of the wind, is approximately
the sound speed. As the sound speed at the surface in our
massive main sequence models is on the order of a few times $10\kms$,
we consider here those stellar models potentially capable to produce wind
clumping for which the convective velocities
in the upper part of the FeCZ $\vca \geq 2.5\kms$,
as this allows energetically to have surface velocity amplitudes
above $\sim 10\kms$ (cf. Sect.~\ref{micro}).