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The Double-Mode Cepheid V371 Persei Redux, Edward G. Schmidt
The Double-Mode Cepheid V371 Persei Redux, Edward G. Schmidt
Edward Schmidt Publications
A metallicity of [Fe/H] = –0.05 to –0.40 was derived from four spectra of the peculiar beat Cepheid V371 Per. This conflicts with previous estimates ranging from –0.7 to –1.0 based on the period ratio. It is suggested that the discrepancy may be resolved by assuming near solar metallicity but a low mass. This is in accord with a suggestion by Sandage and Tammann that the AHB3 (or BL Her) stars are Population I analogs of short-period type II Cepheids. Further pulsational modeling is needed to clarify the status of this star and to understand the AHB3 stars.
V371 Per — A Thick-Disk, Short-Period F/1o Cepheid, P. Wils, A. A. Henden, S. Kleidis, Edward G. Schmidt, D. L. Welch
V371 Per — A Thick-Disk, Short-Period F/1o Cepheid, P. Wils, A. A. Henden, S. Kleidis, Edward G. Schmidt, D. L. Welch
Edward Schmidt Publications
V371 Per was found to be a double-mode Cepheid with a fundamental mode period of 1.738 days, the shortest among Galactic beat Cepheids, and an unusually high period ratio of 0.731, while the other Galactic beat Cepheids have period ratios between 0.697 and 0.713. The latter suggests that the star has a metallicity [Fe/H] between −1 and −0.7. The derived distance from the Galactic plane places it in the thick disk or the Halo, while all other Galactic beat Cepheids belong to the thin disk. There are indications from historical data that both the fundamental and first overtone periods have …