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GT\,Cep is a semi-detached close binary system with an orbital period of 4.91days, containing a massive star. I have obtained spectroscopic observations andderived radial velocities of both components. Combining the analyses of radialvelocities and available photometric observations we have measured the absoluteparameters of both components of GT\,Cep. The components are shown to be aB2\,V primary with a mass M$_p$=10.70$\pm$0.50 M$_{\odot}$ and radiusR$_p$=6.83$\pm$0.19 R$_{\odot}$ and a A0\,IV secondary with a massM$_s$=2.58$\pm$0.14 M$_{\odot}$ and radius R$_s$=7.56$\pm$0.21 R$_{\odot}$. Myanalyses show that GT\,Cep is a classical Algol-type binary with a less massivesecondary filling its $Roche$ lobe. Using the UBVJHK magnitudes and theinterstellar reddening of E(B-V)=0.61 I estimated the mean distance to thesystem as 854$\pm$43\,pc. The O-C residuals have been analyzed as theconsequence of a light-time effect superimposed on an upward parabola. Myanalysis indicates that the eclipsing binary revolves around a third-body witha period of about 57.5 yr in an orbit with a radius of 40 $AU$. The lower limitfor the mass of the third star has been estimated to be 7 M$_{\odot}$ for theinclination between $70^{o}$ and $90^{o}$.

The early B-type eclipsing binary GT\,Cephei: a massive triple system?