ON THE ANOMALOUS BALMER LINE STRENGTHS IN GLOBULAR CLUSTERS

Spectral feature index diagrams with integrated globular clusters and simple stellar population models often show that some clusters have weak H{beta}, so weak that even the oldest models cannot match the observed feature depths. In this work, we rule out the possibility that abundance mixture effects are responsible for the weak indices unless such changes operate to cool the entire isochrone. We discuss this result in the context of other explanations, including horizontal branch morphology, blue straggler populations, and nebular or stellar emission fill-in, finding a preference for flaring in M giants as an explanation for the H{beta} anomaly.