  The transient X-ray binary pulsar A0535+262 was observed with Suzaku on 2005
September 14 when the source was in the declining phase of the August-September
minor outburst. The ~103 s X-ray pulse profile was strongly energy dependent, a
double peaked profile at soft X-ray energy band (<3 keV) and a single peaked
smooth profile at hard X-rays. The width of the primary dip is found to be
increasing with energy. The broad-band energy spectrum of the pulsar is well
described with a Negative and Positive power-law with EXponential (NPEX)
continuum model along with a blackbody component for soft excess. A weak iron
K_alpha emission line with an equivalent width ~25 eV was detected in the
source spectrum. The blackbody component is found to be pulsating over the
pulse phase implying the accretion column and/or the inner edge of the
accretion disk may be the possible emission site of the soft excess in
A0535+262. The higher value of the column density is believed to be the cause
of the secondary dip at the soft X-ray energy band. The iron line equivalent
width is found to be constant (within errors) over the pulse phase. However, a
sinusoidal type of flux variation of iron emission line, in phase with the hard
X-ray flux suggests that the inner accretion disk is the possible emission
region of the iron fluorescence line.
