The advantages of high resolution UV spectroscopy for the investigation of the solar atmosphere are stressed while the limitations in the areas of instrumentation and diagnosis are discussed. The recent achievements (made essentially by Skylab, OSO-8 and rocket instruments) are reviewed and discussed. It is shown that high resolution UV solar spectroscopy has improved our knowledge of the dynamics of the upper layers of the solar atmosphere. Within the present instrument capabilities the birth of coronal expansion is shown to take place at the top of the transition region. The existence of downward flows over the bright regions of the network is evidenced from redshifts or transition region and chromospheric optically thin lines: velocities as large as 22 km s-1 have been measured in O vi. Short period waves (95 s) have been detected in lines of Si ii at chromospheric levels in addition to the well known 300s and 180 s photospheric and chromospheric oscillations. There is strong evidence that optically thin chromospheric and transition region lines are broadened by a nonthermal velocity component which is maximum at 1.3 × 105 K and decreases at higher temperatures. This may indicate the presence of unresolved acoustic or magnetohydrodynamic waves so oftenly set fourth as the source of chromospheric and coronal heating. Contradictions between the various results are pointed out and discussed. They might be attributed to the different angular resolution of the instruments, a key parameter for future space observations. It is suggested that the Solar Optical Telescope (SOT) and the Grazing Incidence Solar Telescope (GRIST) which are presently under phase A studies at NASA and ESA be considered as a tandem of instruments to fly on Spacelab in the 1980's. Both their angular and spectral resolution appear sufficient to resolve most of the problems under discussion today.