Other
Scientific paper
Jan 2012
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21934511h&link_type=abstract
American Astronomical Society, AAS Meeting #219, #345.11
Other
Scientific paper
For the Sun and higher mass M dwarfs, the magnetic field is understood to be anchored at the boundary between the convective and radiative zones. For lower mass fully convective M dwarfs, another type of dynamo must be at work. Examining the chromospheric activity from M dwarfs with a range of masses to test for a change in the character of chromospheric activity yields interesting clues to the nature of the dynamos within fully convective stars. One method to examine the character of the chromospheric activity is a measurement of the degree of variability of the target stars compared to nearby photometrically stable companion stars of like brightness. Measurement of the degree of variability showed that for V-I less than 3.6 the target stars displayed a degree of variability ranging from equal to 20 times greater than companion stars. While for targets stars with V-I greater than 3.6, the degree of variability was equal to that displayed by companion stars. With all the targets stars of V-I greater than 3.6, demonstrating chromospheric activity, the lack of variability may indicate that chromospherically active regions are evenly distributed. Additionally each target star was examined for any periodic behavior in its variability. For 30 stars within the sample, periods were found ranging from around 20 days upwards to 45 days. With a majority published values of Praesepe M dwarf rotational periods being smaller than the range seen within this study, these periods may represent another type of periodicity within active M dwarfs.
Hamper Randall
Honeycutt Kent
QUEST2 Collaboration
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