Fig. 17

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RV curve integrals (=ΔR/p) vs. log P determined from the VELOCE best fit models. Short-period Cepheids (Ppuls < 10 days) are separated into low- and high-amplitude stars using a peak-to-peak RV threshold of 20 km s−1 and color coded in purple (≤ 20 km s−1) and blue (>20 km s−1). Long-period (P > 10d) FU Cepheids exhibit a strikingly (~5.6–6.6×) steeper trend than short-period Cepheids. We introduce an ad hoc distinction among three sequences for P > 10 d FU Cepheids into stars exhibiting large (yellow), intermediate (green), and small (orange) radius variations. The right panel shows a close-up view to more easily distinguish among short-period Cepheids, where a large number of Cepheids are found between the well-defined envelopes made up of FU and FO Cepheids, respectively. Stars near the edges are labeled to facilitate identification.
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