Using $\mathit{uvby}\beta $ -photometry, the Eddington pulsation constant can be determined for $\beta $ Cephei variables, which are mostly stars B0.5-2V-III. Therefore, the known relations between the effective surface temperature and the indexes of $\mathit{uvby}\beta $ -photometry are analyzed for B-stars. These relations were determined using the empirical data from small numbers of stars. Therefore, the representative calibration sample is formed from 104 stars B0-4V-III, for which the effective surface temperature and the indexes of $\mathit{uvby}\beta $ -photometry ( $c_{1}$ , $(b- y)$ , $m_{1}$ , $\beta $ ) are known. Using this sample, for stars B0-4 the relations between $c_{0}$ , $(b- y)_{0}$ , $m_{0}$ , $\beta $ and the effective surface temperature are determined in luminosity classes V, IV and III. It is established new indexes of $(b- y)_{0} '$ , $m_{0} '$ and $\beta '$ that are $((b- y)_{0} - (b- y)_{0(\mathrm{V}+\mathrm{IV})})/ ((b- y)_{0(\mathrm{V}+\mathrm{IV})} - (b- y)_{0(\mathrm{III})})$ , $(m_{0} - m_{0(\mathrm{IV}+\mathrm{V})})/(m_{0(\mathrm{IV}+\mathrm{V})} - m_{0(\mathrm{III})})$ and $(\beta - \beta _{(\mathrm{IV}+\mathrm{V})})/(\beta _{(\mathrm{IV}+\mathrm{V})}- \beta _{\mathrm{III}})$ , respectively. Using the condition of $(b- y)_{0} ' = m_{0} ' = \beta '$ at a constant metallicity, the accurate relations between $c_{0}$ , $(b- y)_{0}$ , $m_{0}$ , $\beta $ , $\beta '$ and the surface effective temperature are determined for stars B0-4V-III. It is found that in $\mathit{uvby}\beta $ -photometry for stars B0-4V-III the known temperature calibrations have average errors of (4 – 9)%. The new accurate temperature calibration has an error of about 1%. It is found that the Eddington pulsation constant depends very loosely on the pulsation period for $\beta $ Cephei variables.
