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Fig. 1


Synthetic HB morphology produced by tidally enhanced stellar wind for different metallicities at a fixed age of 13 Gyr. The metallicities from the top panel to the bottom panel are Z = 0.02, 0.001, 0.0001, for which the primary mass are 0.98, 0.83, and 0.80 M, respectively. HB stars in RR Lyrae strip (defined by the vertical region of 3.80 ≤ log    Teff ≤ 3.875 in the H-R diagram, Koopmann et al. 1994; Lee et al. 1990) are denoted by crosses. Other HB stars are denoted by solid dots. The label of B:V:R in this figure is the number ratio of HB stars located in the region bluer than (or to the left of), within, and redder than (or to the right of) the RR Lyrae instability strip in the H-R diagram.

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