The aim of this study is a uniform system of equatorial spectrophotometric standards to be used with large and intermediatesize telescopes. We plan to obtain absolute energy distributions for 43 equatorial (lcl < 3O) intermediate-brightness (6.5m < V < 8.5m) stars in the spectral region of 3150-7550 A with a resolution of 50 A. The criterion for the selection of the standard stars is the following: at any time, a pair of stars should be observable near the sky meridian (hour angle < 1 h) - one early-type (B9-A2) star and one intermediate-type (GO-G5) star. It is important that both stars are equally observable from both hemispheres of the Earth. The homogeneity of the standard-star system is achieved with the attachment of all the stars to a single primary standard - the circumpolar star HD 221525 (V = 5.58; FOIII); we obtained the energy distribution for this star earlier (Tereshchenko and Glushkova, 1992). Note that we used this star as a primary standard in our work on a spectrophotometric version of the North Polar Sequence (Tereshchenko, 1994). Each star should be observed not less than four times in different nights; the expected standard deviations would be 2-4%. We plan also to observe the spectrophotometric standards in the UBVR system, too. We plan to carry out the spectrophotometric and photometric observations in the high-altitude conditions, on the 1-m and 0.5-m telescopes, with the concave-grating spectrograph and a: UBVB photometer. Partly, this work has already been done. To reveal random and systematic errors in the observations, as well as possible variability of some of the selected standard stars, check-up observations with different instruments in other conditions are highly desirable. In this connection, the author would like to attract the attention of other observers to this program. Table 1 lists the equatorial standard stars.