  We study the appearance of the neutron star - accretion disk system as seen
by a distant observer in the UV/X-ray domain. The observed intensity spectra
are computed assuming non-spherical geometry of the whole system, in which
outgoing spectrum is not represented by the flux spectrum, the latter being
valid for spherically symmetric objects. Intensity spectra of our model display
double bumps in UV/X-ray energy domains. Such structure is caused by the fact
that the the source is not spherically symmetric, and the proper integration of
intensity over emitted area is needed to reproduce observed spectral shape.
Relative normalization of double bump is self consistently computed by our
model. X-ray spectra of such a type were often observed in LMXB with accretion
disk, ultra luminous X-ray sources, and accreting black hole systems with hot
inner compact corona. Our model naturally explains high energy broadening of
the disk spectrum observed in some binaries. We attempted to fit our model to
X-ray data of XTE~J1709-267 from {\it XMM-Newton}. Unfortunately, the double
intensity bump predicted by our model for LMXB is located in soft X-ray domain,
uncovered by existing data for this source.
