A Transition of Dynamo Modes in M Dwarfs: Narrowing Down the Spectral Range Where the Transition Occurs Based in part on observations made at l'Observatoire de Haute Provence (CNRS) and at Pic-du-Midi Observatory, France. Also based on data obtained from the SOPHIE archive (OHP) and from the FEROS, HARPS, and UVES archives (European Southern Observatory)

Houdebine et al. combined Ca ii data with projected rotational velocities (v sin i) to construct rotation-activity correlations (RAC) in K-M dwarfs. The RAC slopes were used to argue that a transition between dynamo modes occurs at a spectral type between M2 and M3. H17 suggested that the dynamo transition corresponds to a transition to complete convection (TTCC). An independent study of GAIA data led Jao et al. to suggest that the TTCC sets in "near M3.0V," close to the H17 result. However, the changes in a star that cause TTCC signatures in GAIA data might not lead to changes in Ca ii emission at an identical spectral type: the latter are also affected by magnetic effects, which depend on certain properties of convection in the core. Here, we use Ca ii emission fluxes in a sample of ∼600 M dwarfs, and attempt to narrow down the transition from one dynamo mode to another: rather than relying on RAC slopes, we quantify how the Ca ii emission flux varies with spectral type to identify "steps" where the flux decreases significantly across a narrow range of spectral types. We suggest that the dynamo mode transition may be narrowed down to between M2.1 and M2.3. This is close to, but earlier than, the TTCC location identified by Jao et al. We suggest that the transition in dynamo mode may be related to the existence of a small convective core, which occurs for a finite time interval in certain low-mass stars.