  We present results from the analysis of the two EXOSAT observations of the
low mass X-ray binary (LMXRB) 4U1957+11. The 1-20keV spectrum of the source is
best fitted by a power law model with exponential cutoff, that provides an
approximation of a thermal Comptonisation spectrum. The cutoff energy (~2keV),
as well as the X-ray colours, are intermediate between those of ultrasoft
sources containing black hole candidates (BHCs) and those of soft LMXRBs
containing an old accreting neutron star. We find no evidence for a black body
spectral component. During the 1985 observation, the source flux was 10% higher
than in the 1983 observation, and the ME spectra provide evidence for a high
energy tail (up to ~16keV), which strengthens the similarity with the spectra
of high state BHCs. However the source luminosity was only ~5 10^36 ergs/s.
During the 1985 observation the GSPC spectra revealed the presence of a 100eV
EW iron K-line emission feature with a centroid energy of 7.06+/-0.09keV; this
value is among the highest measured by {\it EXOSAT}. The ME light curves showed
only a low-amplitude variability on timescales of a few hours. No evidence for
a periodic modulation with periods between 0.016 and 13000~s was found.
