Hot Stellar Populations in Globular Cluster Cores

Details Hot Stellar Populations in Globular Cluster Cores Hot Stellar Populations in Globular Cluster Cores

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.6095d&link_type=abstract

HST Proposal ID #6095

Computer Science

Hst Proposal Id #6095 Stellar Populations

Scientific paper

The goal of this program is to use both the resolving power and the far-UV imaging capability of HST to study the nature of hot stellar populations and their radial gradients in the cores of globular clusters. We propose to survey dense globular cluster cores in the far-UV, B, and V passbands using WFPC2. We will discover all UV-bright stars at or above the turnoff, producing for the first time a nearly complete census of these populations. Magnitudes in the far-UV, B and V passbands permit an estimate of temperature, bolometric luminosity, and placement in the color-magnitude diagram. Numerous ground-based studies show that population gradients exist in concentrated globular cluster cores, and IUE spectra and some early HST data show they are also seen in the far-UV. Some centrally concentrated hot stellar population must be present, e.g., faint BHB stars, blue stragglers, stripped red giant cores, merged stars, or some new, as yet unknown type of object. These phenomena may be relevant for the origins of x- ray sources and millisecond pulsars in globular clusters. The data we propose to obtain would provide essential input for theoretical models. We should also be capable of detecting stars in brief UV-bright phases of evolution, as short as 10^5 - 10^6 yr. The frequency of UV-bright stars per Lsun can be used to place limits on their evolutionary lifetimes, thus constraining their origin. The normal far-UV phases of stellar evolution may help explain the UV-rising flux

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