We report on the results of spectral analysis of the dipping source XB 1254–690 observed by the BeppoSAX satellite .
We find that the X-ray dips are not present during the BeppoSAX observation , in line with recent RXTE results .
The broad band ( 0.1–100 keV ) energy spectrum is well fitted by a three-component model consisting of a multicolor disk blackbody with an inner disk temperature of \sim 0.85 keV , a comptonized spectrum with an electron temperature of \sim 2 keV , and a bremsstrahlung at a temperature of \sim 20 keV .
Adopting a distance of 10 kpc and taking into account a spectral hardening factor of \sim 1.7 ( because of electron scattering which modifies the blackbody spectrum emitted by the disk ) we estimated that the inner disk radius is R _ { in } \sqrt { \cos i } \sim 11 km , where i is the inclination angle of the system with respect to the line of sight .
The comptonized component could originate in a spherical corona or boundary layer , surrounding the neutron star , with optical depth \sim 19 .
The bremsstrahlung emission , contributing \sim 4 \% of the total luminosity , probably originates in an extended accretion disk corona with radius \sim 10 ^ { 10 } cm .
In this scenario we calculated that the optical depth of this region is \sim 0.71 and its mean electron density is N _ { e } \sim 2.7 \times 10 ^ { 14 } cm ^ { -3 } .
This last component might also be present in other low mass X-ray binaries , but , because of its low intrinsic luminosity , it is not easily observable .
We also find an absorption edge at \sim 1.27 keV with an optical depth of \sim 0.15 .
Its energy could correspond to the L-edge of Fe XVII , or K-edge of Ne X or neutral Mg .