We present two sets of synthetic horizontal-branch (HB) models which h
ave been computed using the evolutionary tracks of Sweigart (1987) (Y(
MS) = 0.20, 0.25, 0.30; Z = 10(-4), 10(-3)) and of Lee & Demarque (199
0) (Y(MS) = 0.20, 0.23; 10(-4) less-than-or-equal-to Z less-than-or-eq
ual-to 4 10(-3)). Three different values (0.01, 0.02, and 0.03 M.) for
the width sigma(M) of the HB mass distribution have been considered f
or each of the (Y, Z) combinations that may be obtained for the two em
ployed sets of evolutionary tracks. This gives a total of 60 possibili
ties which have been analyzed. In each of these cases the mean HB evol
utionary mass has been varied so as to yield from very blue to very re
d HB morphologies. An extensive tabulation of the morphological and pu
lsational results thereby obtained is given for selected cases (Lee &
Demarque's tracks, Y(MS) = 0.23). Such models enable a thorough study
of some of the properties of the Galactic globular cluster system, inc
luding very important issues such as the cluster ages and the long-sta
nding Oosterhoff dichotomy and second parameter problems, as well as t
he Sandage period-shift effect. According to recent theoretical sugges
tions, the enhancement of alpha-elements in halo stars may play a role
in what concerns the interpretation of HB properties. In this sense,
we make an initial exploration of the present tables, addressing some
of the above problems in the light of the adopted theoretical evolutio
nary and pulsational frameworks for HB stars and RR Lyrae pulsation.