  GX 301-2, a bright HMXB with an orbital period of 41.5 days, exhibits stable
periodic orbital intensity modulations with a strong pre-periastron X-ray
flare. Several models have been proposed to explain the accretion at different
orbital phases, invoking accretion via stellar wind, equatorial disk, and
accretion stream from the companion star. We present results from exhaustive
orbital phase resolved spectroscopic measurements of GX 301-2 using data from
the Gas Slit Camera onboard MAXI. Using spectroscopic analysis of the MAXI data
with unprecendented orbital coverage for many orbits continuously, we have
found a strong orbital dependence of the absorption column density and
equivalent width of the iron emission line. A very large equivalent width of
the iron line along with a small value of the column density in the orbital
phase range 0.10-0.30 after the periastron passage indicates presence of high
density absorbing matter behind the neutron star in these orbital phase range.
A low energy excess is also found in the spectrum at orbital phases around the
pre-periastron X-ray flare. The orbital dependence of these parameters are then
used to examine the various models about mode of accretion onto the neutron
star in GX 301-2.
