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We present an analysis of the neutron star High Mass X-ray Binary (HMXB) 4U1909+07 mainly based on Suzaku data. We extend the pulse period evolution,which behaves in a random-walk like manner, indicative of direct windaccretion. Studying the spectral properties of 4U 1909+07 between 0.5 to 90 keVwe 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 atlow energies. We find no evidence for a cyclotron resonant scattering feature(CRSF), a feature seen in many other neutron star HMXBs sources. By performingpulse phase resolved spectroscopy we investigate the origin of the strongenergy dependence of the pulse profile, which evolves from a broad two-peakprofile at low energies to a profile with a single, narrow peak at energiesabove 20 keV. Our data show that it is very likely that a higher folding energyin the high energy peak is responsible for this behavior. This in turn leads tothe assumption that we observe the two magnetic poles and their respectiveaccretion columns at different phases, and that these accretions column haveslightly different physical conditions.

Staring at 4U 1909+07 with Suzaku