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tokens: in two distinct emission regions. We used compTT plus compPS , or two compTB . The dominant emission results, by the Comptonization, in a disk geometry of seed photons at 0.1 keV by a plasma with keV and optical depth 3. This emission can be interpreted as arising in a region above the accretion disk and contributes to the 70 of the total flux. We call this component hard Comptonization. In addition, a secondary emission component, described by a spherical geometry, is due to seed photons at 0.8 keV Comptonized by a plasma with keV and optical depth 8 using a compTT model or with keV using a compTB . This emission can be interpreted as originating from a region closer to the neutron star around the boundary layer and contributes about 30 of the total flux. We call this component soft Comptonization. The persistent emission spectrum of the LMXB GS 1826-23, observed jointly by Chandra and RXTE, has been described by Thompson et al. ( 2005 ) with a similar model. This model uses dual Comptonization of 0.3 keV soft photons by a plasma with keV and , which is interpreted as emission from accretion disk corona, plus Comptonization of hotter 0.8 keV photons by a 6.8 keV plasma, which is interpreted as emission from the boundary layer. The parameters are therefore very similar to those reported here for 4U 1705-44. Moreover, a dual Comptonization model was successfully applied to the broadband spectra of the low/hard state of the black hole candidate Cyg X-1 by Makishima et al. ( 2008 ) with Suzaku data, by Di Salvo et al. ( 2001 ) and Frontera et al. ( 2001 ) with Beppo SAX data, and by Gierliski et al. (2007) and Ibragimov et al. ( 2005 ), who used simultaneous Ginga, RXTE and GRO/OSSE data. Takahashi et al. ( 2008 ) modeled the spectra of GRO J1655–40 taken with Suzaku in a similar way. Recently, the two compTB model was applied to six neutron star LMXBs (see Seifina et al. 2015 ). This model describes a scenario in which the Keplerian disk is connected to the neutron star by the transition layer (see Titarchuk et al. 1998 ), where the hot electrons scatter off the soft photons from the neutron star photosphere of temperature and the soft disk photons of temperature giving rise to two Comptonized components. We stress that no reflection component is needed in the two scenarios described above. 5.2. Banana states and high energy tail The absorbed Comptonized component with reflection does not describe the soft/high state spectrum. In addition to a dominating Comptonized emission, the continuum broadband spectrum of the source during the soft state requires a blackbody component at lower energies and a hard component to model the hard tail or excess. The dual Comptonization scenario successfully describes the broadband spectra of the banana state in that it models the soft dominating emission and the hard tail well. Contrary to the island state, the dominating Comptonization emission is soft and is expected to originate in the hot plasma