Rotation, turbulence and evidence for magnetic fields in southern dwarfs

Details Rotation, turbulence and evidence for magnetic fields in southern dwarfs Rotation, turbulence and evidence for magnetic fields in southern dwarfs

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997mnras.284..803s&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 284, Issue 4, pp. 803-810.

Astronomy and Astrophysics

Astronomy

87

Convection, Turbulence, Stars: Late-Type, Stars: Magnetic Fields, Stars: Rotation

Scientific paper

We model high-resolution spectra using a simple radiative transfer analysis to derive projected rotational velocities (v sin i) and macroturbulent velocity dispersions (v_mac) for 49 southern dwarf stars (including many first-ever measurements). We compare our results with previous values, and estimate rotation periods (P_rot) and sin i values where possible. We confirm that v_mac generally decreases with decreasing temperature for T_eff >= 5000 K. Magnetically active stars tend to show enhanced values of v_mac. This may be due to a difference in the mean stellar convective properties, a change in the mean stellar temperature structure, or a combination of both. We identify a group of stars that exhibit correlations between the derived velocities and line Lande g_eff values, implying the presence of significant surface magnetic flux.

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