Cycle times of early M dwarf stars: mean field models versus observations. Issue Volume 15:Issue S354(2019) (June 2019)

• Record Type: Journal Article
• Authors: Küker, Manfred; Rüdiger, Günther; Oláh, Katalin; Strassmeier, Klaus G.
• Editors: Kosovichev, Alexander; Strassmeier, Klaus; Jardine, Moira
• Is Part Of: Proceedings of the International Astronomical Union. Volume 15:Issue S354(2019)
• Page Start: 116
• Page End: 119
• Publication Date: 2019-06
• Subjects: Stars: late-type, -- stars: magnetic field, -- stars: activity, -- magnetohydrodynamics (MHD), -- turbulence; Astronomy -- Congresses; Astronomy -- Periodicals; 520
• DOI: 10.1017/S1743921319010007
• Languages: English
• ISSNs: 1743-9213

Abstract

Abstract: Observations of early-type M stars suggest that there are two characteristic cycle times, one of order one year for fast rotators ( P r ot < 1 day) and another of order four years for slower rotators. For a sample of fast-rotating stars, the equator-to-pole differences of the rotation rates up to 0.03 rad d−1 are also known from Kepler data. These findings are well-reproduced by mean field models. These models predict amplitudes of the meridional flow, from which the travel time from pole to equator at the base of the convection zone of early-type M stars can be calculated. As these travel times always exceed the observed cycle times, our findings do not support the flux transport dynamo.