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In this work, a mass-effective temperature-surface gravity relation (MTGR) isdeveloped for main sequence stars in the range of 6400 K < $T_{\rm eff}$ <20000 K with log$g$ > 3.44. The MTGR allows the simple estimation of the massesof stars from their effective temperatures and surface gravities. It can beused for solar metallicity and can be rescaled for any metallicity within -1.00< [Fe/H] < 0.7. The effect of alpha-enhanced compositions can also beconsidered with the help of correction terms.  It is aimed to develop an MTGR that can estimate the masses of main-sequencestars from their atmospheric parameters. One advantage of an MTGR over theclassical mass-luminosity relations is that its mass estimation is based onparameters that can be obtained by purely spectroscopic methods and, therefore,the interstellar extinction or reddening do not have to be known. The use ofsurface gravity ($g$) also relates an MTGR with stellar evolution and providesa more reliable mass estimation.  A synthetical MTGR is obtained from theoretical isochrones using aLevenberg-Marquardt chi-square minimization algorithm. The validity of the MTGRis then checked by testing over 278 binary components with precise absolutemasses. Very good agreement has been obtained between the absolute masses of278 binary star components and their masses estimated from the MTGR. Amathematical expression is also given to calculate the propagated uncertaintiesof the MTGR masses.  For the typical uncertainties in atmospheric parameters and metallicity, thetypical uncertainties in the masses estimated from the MTGR mostly remainaround 5-9%. The fact that this uncertainty level is only on average aboutthree times as large as that of the absolute masses indicates that the MTGR isa very powerful tool for stellar mass estimation. A computer code, mtgr.pro,written in GDL/IDL is also provided for the relation.

Mass-effective temperature-surface gravity relation for intermediate-mass main-sequence stars