  We present results from Chandra and XMM-Newton observations of the
low-ionization broad absorption line (LoBAL) quasar H 1413+117. Our spatial and
spectral analysis of a recent deep Chandra observation confirms a microlensing
event in a previous Chandra observation performed about 5 years earlier. We
present constraints on the structure of the accretion flow in H 1413+117 based
on the time-scale of this microlensing event. Our analysis of the combined
spectrum of all the images indicates the presence of two emission peaks at
rest-frame energies of 5.35 keV and 6.32 keV detected at the > 98% and > 99%
confidence levels, respectively. The double peaked Fe emission line is fit well
with an accretion-disk line model, however, the best-fitting model parameters
are neither well constrained nor unique. Additional observations are required
to constrain the model parameters better and to confirm the relativistic
interpretation of the double peaked Fe Kalpha line. Another possible
interpretation of the Fe emission is fluorescent Fe emission from the back-side
of the wind. The spectra of images C and D show significant high-energy broad
absorption features that extend up to rest-frame energies of 9 keV and 15 keV
respectively. We propose that a likely cause of these differences is
significant variability of the outflow on time-scales that are shorter than the
time-delays between the images. The Chandra observation of H 1413+117 has made
possible for the first time the detection of the inner regions of the accretion
disk and/or wind and the high ionization component of the outflowing wind of a
LoBAL quasar.
