Program: GS-2009A-C-9

Direct detection of winds from giant stars in globular clusters remains elusive although stellar evolution of low mass stars requires mass loss on the red giant branch in order to reproduce the horizontal branch morphology. The \ion{He}{1} 1.0830\micron\ line observed in field metal-poor stars shows that fast ($\sim$100 km/s) winds occur in warm giants and also red horizontal branch stars in amounts with evolutionary significance. We propose to use PHOENIX to measure the \ion{He}{1} 1.0830\micron\ line in giants and horizontal branch stars of the globular cluster M4 to detect fast mass outflows. Wind speeds may allow material to escape the cluster and solve the mystery of the missing interstellar medium in globular clusters. Non-LTE semi-empirical modeling of the winds based on these profiles combined with existing high resolution optical spectra, will establish stellar mass loss rates for metal-poor stars.