  The `Bloated Stars Scenario' proposes that AGN broad line emission originates
in the winds or envelopes of bloated stars (BS). Alexander and Netzer (1994,
1996) established that ~ 5e4 BSs with dense, decelerating winds can reproduce
the observed emission line spectrum and line profiles while avoiding rapid
collisional destruction. Here, I investigate a third prediction of the model,
related to the size of the broad line region, by deriving the emission line
response to variations in the ionizing continuum (`line reverberation') and
comparing it to observations. The expected time lags, as well as the order of
response of the various lines, strongly depend on the typical variability time
scale of the ionizing continuum. The BS model studied here corresponds to a
bright Syfert 1 galaxy (Sy1) or a low luminosity QSO. I find that the BS model
is consistent with the observed correlation between the Balmer lines time lags
and the AGN luminosity, which at present is the only line reverberation
information available for this luminosity class. The model displays also some
of the anti-correlation between the time lags of the metal emission lines and
their degree of ionization that has been observed in a few low-luminosity Sy1s.
However, the bright Sy1 model results differs from the low-luminosity Sy1 data
in that the Hb time lag is relatively shorter and the CIV time lag relatively
longer.
