We present time-series VI photometry of the metal-rich globular cluster NGC 6316. Our color-magnitude diagrams show a predominantly red-clump horizontal branch morphology with no evidence of the blue extensions seen in NGC 6388 and NGC 6441. Our data are in good agreement with published estimates of the reddening and metallicity provided the cluster has an absolute distance modulus of 15.5 mag. We have discovered more than one dozen long-period variable stars in our field of view and argue that at least seven of them are members of NGC 6316. We have also discovered four RR Lyrae variables, although only one of them probably belongs to the cluster. The specific frequency of RR Lyrae stars in NGC 6316 is found to be less than 0.4, making it clear that this cluster is a normal, metal-rich globular and is not an analog of NGC 6388 and NGC 6441. We recommend long-term photometric monitoring of NGC 6316 to clarify the nature of the RR Lyrae member candidates, as well as the pulsation classes of the long-period variables.

We describe a photometric survey for variable stars in twelve metal-rich globular clusters, and provide results for the first two clusters.The census of variable stars in metal-rich globular clusters ([Fe/H] > -0.8 dex) is badly incomplete. Most of the clusters have not been searched to the depth of the horizontal branch. This hinders comparisons of the formation rate and mechanisms of cluster RR Lyrae variables with the more frequently occurring field RR Lyrae stars. RR Lyrae stars in and toward the clusters also provide accurate estimates of the reddening toward these low-latitude objects.To remedy this situation, we obtained time series observations in the V and / passbands for each of the twelve target clusters. We used the 0.9-m telescope at the Cerro Tololo Inter-American Observatory and a large-format CCD. We chose the exposure times to ensure good photometry of the long period variables on the red giant branch and of the RR Lyrae variables.We reported the results for our first cluster, NGC 6441, in Layden et al. (1999). The results for our second cluster, NGC 6316, are as follows. The color-magnitude diagram displays the red clump morphology of a typical metalrich globular cluster. We detected about 20 long-period variable stars (seven probable cluster members), two eclipsing binaries (foreground), and at least 6 RR Lyrae variables. All of the RR Lyrae variables appear to lie in the foreground, with the possible exception B32, which has the correct color and magnitude to be a cluster member. B32 also lies close to the cluster center. However, our best period estimate for B32 is 2.075 d, suggestive of an Anomalous or Type II Cepheid lying behind the cluster. More observations are required to confirm this period. Using the apparent colors of three foreground RRab stars, we determined the reddening to be E(B -V) = 0.62 ± 0.03 mag (following the method of Mateo et al. 1995).