This section summarizes results presented above as well as those
described in Paper I.
We surveyed a total of six fields covering most of the central part
of 
Cen and identified 70 periodic variables.
This sample includes 6 previously known variables. RR Lyr stars are excluded
from these statistics - a separate paper devoted to them is in
preparation.
The most interesting result is identification of 3 detached eclipsing
systems which are located at the base of the subgiant branch of the
cluster. These are OGLEGC15, OGLEGC17 and OGLEGC51.
Further observations of these systems can lead to direct determination of
masses and radii of turnoff stars in 
Cen. An accurate
determination of the cluster distance would be also obtained from
such data. Another detached or semi-detached binaries identified in our survey
are OGLEGC14 and OGLEGC52. The former one is a blue straggler (assuming
it is a cluster member) while the latter is located slightly above
the horizontal branch of the cluster.
We obtained light curves for 34 SX Phe stars. All of them are
located among blue stragglers and are likely members of the
cluster. 20 out of 34 of identified SX Phe stars shows
variability with a full range not exceeding 0.1 mag in the V-band.
Detected SX Phe stars constitute about 12% of the blue straggler
population of 
Cen.
Several contact or nearly-contact binaries were identified. Most of them are located among blue stragglers but some systems are present among upper main-sequence and turnoff stars. Most of identified contact binaries are likely members of the cluster.
Three low-amplitude variables with periods from the range 19-33 days were identified on the subgiant branch (OGLEGC22, OGLEGC35 and OGLEGC69). These stars belong most likely to the so called "spotted" variables. Another likely variable of this type is OGLEGC30 whose position on the CMD is unknown due to lack of information about its color.
Acknowledgements
This project was supported by NSF grants AST 92-16494 and AST-9313620 to Bohdan Paczynski and AST 92-16830 to George Preston. JK was supported by the Polish KBN grants 2P03D-008-08 and BST 501/17/95. MK, MS and AU were supported by the Polish KBN grant 2P03D-029-08.