  We analyzed spectral variations of $\sim 8.5$ days long RXTE monitoring
observations of Her X-1 in December 2001. This set of observations enables, for
the first time, frequent continuous monitoring (111 pointings in $\sim 8.5$
days) of the source with RXTE including $\sim 1.7$ days long low state part and
the following $\sim 6.8$ days long short high state part. We used absorbed
power law model with iron line energy complex modeled as a Gaussian to fit both
the 3-60 keV PCA-HEXTE overall short high state spectrum and 3-20 keV
individual PCA spectra. Additional partial cold absorber model was used for
both cases. Using 3-20 keV individual PCA spectra, absorption in anomalous dips
and preeclipse dips in short high state were compared. Decreasing ratio of
unabsorbed flux to absorbed flux with increasing unabsorbed flux in anomalous
and preeclipse dips was interpreted as an evidence of the fact that the regions
causing opaque obscuration and soft absorption are not geometrically far away
from each other. Higher iron line peak energies in low state and short high
state ($\sim 6.6-6.9$ keV) were interpreted as a clue of the presence of iron
line components other than K$\alpha$ emission line.
