This paper sets about a brief review of the current knowledge of ground based interferometry, and then, using the relevant information from this up-to-date technique, its tentative application to the study of solar granular structures. As a matter of fact, most of the fundamental processes in the photosphere take place on very small spatial scales and understanding the formation of the solar granulation, pores as well as tiny photospheric faculae, requires insight into the magnetic network where the thermal instabilities are initiated. The study of fine scale structures, typically of about 15 milliarcsec (11 km) by interferometry, i.e. to a resolution not accessible through classical optical telescopes, is certainly the key to open the door to new scenarios in solar physics. By the way, similar phenomena are likely to be accountered in other type of stars. Particular attention is paid to the role of imaging reconstruction at very high angular resolution. Some of the thus achievable solar programmes are listed, mainly with solar granulation. The new type of instrumentation involved should be in the 90's commissioned. At last, it is pointed out that solar interferometry could be also performed in space, as earlier suggested by J.L. DAME and C. AIME to ESA, for the study of flares, prominences or coronal loops, which are closely linked to the photosphere, and for the 2000's horizon. Some problems inherent to this whole prospect (ground and space) are listed, and discussion is welcomed for determining adequate programmes, and also to highlight promising directions for future investigations.