Are most short-period Cepheids overtone pulsators?

Details Are most short-period Cepheids overtone pulsators? Are most short-period Cepheids overtone pulsators?

Jan 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...324l..27b&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 324, Jan. 1, 1988, p. L27-L29.

Astronomy and Astrophysics

Astrophysics

20

Cepheid Variables, Harmonic Generators, Stellar Oscillations, Harmonics, Pulsars, Stellar Evolution, Stellar Mass

Scientific paper

Data given and analyzed recently by Coulson et al. (1986) and Gieren (1982) provide a consistent set of Wesselink radii and Wesselink masses, for which the internal error bars appear to be small enough that a quantitative discussion appears to be warranted. When it is assumed that all Cepheids pulsate in the fundamental mode, a steep discontinuity in mass is found for periods around 6.5 days. When short-period Cepheids are interpreted as first-overtone pulsators as required theoretically (Christy, 1966; Stobie, 1969), the discontinuity disappears and the mass-period relation passes through the bump and beat masses for Cepheids.

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