Behavior of Li abundances in solar-analog stars. Evidence for line-width dependence

Details Behavior of Li abundances in solar-analog stars. Evidence for line-width dependence Behavior of Li abundances in solar-analog stars. Evidence for line-width dependence

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007a%26a...468..663t&link_type=abstract

Astronomy and Astrophysics, Volume 468, Issue 2, June III 2007, pp.663-677

Astronomy and Astrophysics

Astrophysics

35

Stars: Abundances, Stars: Atmospheres, Stars: Fundamental Parameters, Stars: Late-Type, Sun: Fundamental Parameters

Scientific paper

Context: It is known that the surface lithium abundances of field solar-analog G dwarfs show a large dispersion of ⪆2 dex (among which our Sun is located at the lower end) despite the similarity of stellar parameters, and planet-host stars tend to show comparatively lower Li abundances in the narrow T_eff range. Aims: To investigate the reason for these phenomena, an extensive study of Li abundances and their dependence on stellar parameters was carried out for a homogeneous sample of 118 selected solar analogs based on high-dispersion spectra obtained at Okayama Astrophysical Observatory. Methods: The atmospheric parameters were spectroscopically determined by using the equivalent widths of Fe i and Fe ii lines, the ages/masses were estimated from stellar evolutionary tracks, and the width of the macrobroadening (rotation plus macroturbulence) function as well as Li abundances (A_Li) were established by spectrum-fitting analyses. Results: The resulting A_Li vs. T_eff relation revealed a characteristic inverse-triangle-like distribution enclosed by two clear-cut boundaries (the slanted one running from ~5900 K to ~5800 K and the vertical one at ~5700 K), while the Sun is located around its lowest apex. More significantly, A_Li in this region of large dispersion was found to closely correlate with the macrobroadening width (v_r+m), which is considered to be the most important parameter. Conclusions: With a reasonable assumption that the difference of rotational velocity is mainly responsible for the variety of v_r+m, we may conclude that the stellar angular momentum plays the decisive role in determining the surface Li abundances of solar-analog stars in the T_eff range of ~5900-5700 K. The low-Li tendency of planet-host stars may thus be interpreted in terms of rotational characteristics.
Based on observations carried out at Okayama Astrophysical Observatory (Okayama, Japan). Tables 2-6 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/468/663

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