  We show how previous works (Fuhrmann et al., van 't Veer-Menneret &
Megessier) demonstrate the efficiency of the use of Balmer line profiles for
effective temperature determination. In agreement with them, we insist on the
physical interest of this method based on the behaviour of these lines with the
variations of the parameters involved in the treatment of the convective
transport. The comparison between Fuhrmann's results and ours, independently
obtained, exhibits a quite good agreement. We show new results of effective
temperature, gravity and metallicities for a few of our programme stars,
ranging from solar to overabundant metallicities.
