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T. E. Nordgren (USNO - NPOI), B. F. Lane (Caltech), R. B. Hindsley (NRL)
Direct diameter observations of Cepheid variables are used to recalibrate the Barnes-Evans Cepheid surface brightness relation. Sixty separate Cepheid diameter measurements from four different optical interferometers are used to calculate surface brightnesses as a function of pulsation phase. The linear fit to Cepheid surface brightness versus color is in agreement with functions in the literature found using interferometric observations of non-variable giant and supergiant stars.
The author(s) of this abstract have provided an email address for comments about the abstract: nordgren@nofs.navy.mil