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Fractional Stellar Convection Zone Depth and the Generation of Magnetic Flux: An Empirical Approach

Published online by Cambridge University Press:  04 August 2017

Mark S. Giampapa
Mark S. Giampapa*
Affiliation:
Harvard-Smithsonian Center for Astrophysics 60 Garden Street Cambridge, MA 02138, U.S.A.

Abstract

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I present preliminary results from an observational investigation of very late M dwarf stars utilizing the Multiple Mirror Telescope facility. I find that dwarf stars later than spectral type M5 do not necessarily exhibit Hα line emission, contrary to the assertion by Joy and Abt (1974). The preliminary results I discuss herein tentatively suggest, but do not prove, that the generation of significant magnetic fields and magnetic flux is severely inhibited in fully convective stars.

Type
II. Rotation — Activity — Cycle — Age Connection: Observations
Information
Symposium - International Astronomical Union , Volume 102: Solar and Stellar Magnetic Fields: Origins and Coronal Effects , 1983 , pp. 187 - 192
Copyright
Copyright © Reidel 1983 

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