  The radiation from the central regions of active galactic nuclei, including
that from the accretion disk surrounding the black hole, is likely to peak in
the extreme ultraviolet $\sim 13 -100$ eV. However, due to Galactic absorption,
we are limited to constrain the physical properties, i.e. the black hole mass
and the accretion rate, from what observations we have below $\sim 10$ eV or
above $\sim 100$ eV. In this paper we predict the thermal and ionization states
of warm absorbers as a function of the shape of the unobservable continuum. In
particular we model an accretion disk at $kT_{in} \sim 10$ eV and a {\it soft
excess} at $kT_{se} \sim 150$ eV. The warm absorber, which is the highly
ionized gas along the line of sight to the continuum, shows signatures in the
$\sim 0.3 - 2$ keV energy range consisting of numerous absorption lines and
edges of various ions, some of the prominent ones being H- and He-like oxygen,
neon, magnesium and silicon. We find that the properties of the warm absorber
are significantly influenced by the changes in the temperature of the accretion
disk, as well as by the strength of the {\it soft excess}, as they affect the
optical depth particularly for iron and oxygen. These trends may help develop a
method of characterising the shape of the unobservable continuum and the
occurrence of warm absorbers.
