On the nature of the AM phenomenon or on a stabilization and the tidal mixing in binaries. II. Metallicity and pseudo-synchronization.

Details On the nature of the AM phenomenon or on a stabilization and the tidal mixing in binaries. II. Metallicity and pseudo-synchronization. On the nature of the AM phenomenon or on a stabilization and the tidal mixing in binaries. II. Metallicity and pseudo-synchronization.

Oct 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...326..655b&link_type=abstract

Astronomy and Astrophysics, v.326, p.655-661

Astronomy and Astrophysics

Astrophysics

24

Stars: Chemically Peculiar, Binaries: Close, Turbulence, Diffusion, Hydrodynamics

Scientific paper

We reveal sufficient evidences that for Am binaries the metallicity might depend on their orbital periods, P_orb_, rather than on vsini. In particular, δm_1_ index seems to decrease with increasing orbital period up to at least P_orb_=~50d, probably even up to P_orb_=~200d. This gives further support to our "tidal mixing + stabilization" hypothesis formulated in Part I. Moreover, while the most metallic Am stars seem to have rather large periods the slowest rotators are found to exhibit substantially shorter P_orb_. A questioning eye is thus cast on the generally adopted view that Am peculiarity is caused by a suppressed rotationally induced mixing in slowly rotating `single' stars. The observed anticorrelation between rotation and metallicity may have also other than the `textbook' explanation, namely being the result of the correlation between metallicity and orbital period, as the majority of Am binaries are possibly synchronized. We further argue that there is a tendency in Am binaries towards pseudo-synchronization up to P_orb_=~35d. This has, however, no serious impact on our conclusions from Part I; on the contrary, they still hold even if this effect is taken into account.

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