  We present an analysis of the neutron star High Mass X-ray Binary (HMXB) 4U
1909+07 mainly based on Suzaku data. We extend the pulse period evolution,
which behaves in a random-walk like manner, indicative of direct wind
accretion. Studying the spectral properties of 4U 1909+07 between 0.5 to 90 keV
we find that a power-law with an exponential cutoff can describe the data well,
when additionally allowing for a blackbody or a partially covering absorber at
low energies. We find no evidence for a cyclotron resonant scattering feature
(CRSF), a feature seen in many other neutron star HMXBs sources. By performing
pulse phase resolved spectroscopy we investigate the origin of the strong
energy dependence of the pulse profile, which evolves from a broad two-peak
profile at low energies to a profile with a single, narrow peak at energies
above 20 keV. Our data show that it is very likely that a higher folding energy
in the high energy peak is responsible for this behavior. This in turn leads to
the assumption that we observe the two magnetic poles and their respective
accretion columns at different phases, and that these accretions column have
slightly different physical conditions.
