Rotation, turbulence and evidence for magnetic fields in southern dwarfs
- 1 February 1997
- journal article
- Published by Oxford University Press (OUP) in Monthly Notices of the Royal Astronomical Society
- Vol. 284 (4) , 803-810
- https://doi.org/10.1093/mnras/284.4.803
Abstract
We model high-resolution spectra using a simple radiative transfer analysis to derive projected rotational velocities (u sin i) and macroturbulent velocity dispersions (umac) for 49 southern dwarf stars (including many first-ever measurements). We compare our results with previous values, and estimate rotation periods (Prot) and sin i values where possible. We confirm that vmac generally decreases with decreasing temperature for Teff ≥ 5000 K. Magnetically active stars tend to show enhanced values of vmac. 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 Landé geft values, implying the presence of significant surface magnetic flux.Keywords
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