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Matteo Cantiello added The_stars_in_Fig_2__.tex
over 8 years ago
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The stars in Fig. 2 form two distinct branches that gradually merge as the
stars evolve leftwards towards lower \numax. Most stars fall on the
``normal'' upper branch of $V^2\approx 1.5$, in agreement with previous
results \citep{Mosser_2011}.
The lower branch, with suppressed dipole modes, agrees remarkably well with
theoretical predictions (black curve). This prediction
assumes that all the wave energy leaking into the stellar core is trapped by
a magnetic greenhouse effect caused by strong internal magnetic fields
\citep{Fuller15}.
The decrease of the suppression towards lower \numax\ is a consequence of
the weaker coupling between acoustic waves in the envelope and gravity
waves in the core \citep{Fuller15}.
With this large sample we have been able to separate the stars in Fig.2
into five different mass intervals, from 0.9 to 2.1\msol. It is striking
how strongly the relative population on the lower branch (stars with
suppressed dipole modes) depends on mass.
