Abstract
M dwarfs are generally too faint to allow spectra with sufficient S/N ratios for Doppler imaging to be obtained in short enough exposure times. Using a large number of photospheric absorption lines, we use a sophisticated cross-correlation technique to derive absorption profiles with S/N ratios of 350. The surface images of RE 1816 +541 reveal a moderately spotted surface, with starspots appearing at all latitudes. We attempt to measure the surface differential rotation differential rotation rate and find a lower limit on the time it takes the equator to lap the poles of 80 +/- 9 days. This is in close agreement with other results and extrapolations of current theoretical predictions.
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Barnes, J., Cameron, A.C. (2001). Doppler Images of the M Dwarf RE 1816 +541. In: Boffin, H.M., Cuypers, J., Steeghs, D. (eds) Astrotomography. Lecture Notes in Physics, vol 573. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-45339-3_18
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DOI: https://doi.org/10.1007/3-540-45339-3_18
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