Doppler Imaging of Rapidly-Rotating M Stars |
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| Authors: | Klaus G Strassmeier |
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| Institution: | (1) Astrophysical Institute Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany |
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| Abstract: | With the advent of 8–12m-class telescopes and powerful new spectrographs, we can now extend the Doppler-imaging technique to the cool (and faint) end of the main sequence. At a spectral type of approximately M2, stars are thought to become fully convective and cannot possess an overshoot layer between a radiative core and a convective envelope which, as in the case of the Sun and similar stars, likely harbors the dynamo. Therefore, one could expect a fundamentally different magnetic-field topology than on the Sun and thus a qualitatively different surface temperature distribution with new, hitherto unknown, magnetic activity phenomena. Unfortunately, most single M stars do not rotate sufficiently fast for Doppler imaging and one has to “use” binaries or pre-main-sequence stars in which M stars appear spun up or, in binaries, synchronized to the orbital motion. |
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| Keywords: | M stars Stellar activity Active chromospheres Doppler imaging |
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