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Stellar dynamos with Ω × J effect

В. В. Пипин, N. Seehafer

Open publisher page 19 citations

Abstract

Context. The standard dynamo model for the solar and stellar magnetic fields is based on the mechanism, namely, an interplay between differential rotation (the Ω effect) and a mean electromotive force generated by helical turbulent convection flows (the α effect). There are, however, a number of problems with the α effect and dynamo models. Two of them are that, in the case of the Sun, the obtained cycle periods are too short and the magnetic activity is not sufficiently concentrated at low latitudes.

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What this paper is about

Context. The standard dynamo model for the solar and stellar magnetic fields is based on the mechanism, namely, an interplay between differential rotation (the Ω effect) and a mean electromotive force generated by helical turbulent convection flows (the α effect). There are, however, a number of problems with the α effect and dynamo models. Two of them are that, in the case of the Sun, the obtained cycle periods are too short and the magnetic activity is not sufficiently concentrated at low latitudes.

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Available abstract

Context. The standard dynamo model for the solar and stellar magnetic fields is based on the mechanism, namely, an interplay between differential rotation (the Ω effect) and a mean electromotive force generated by helical turbulent convection flows (the α effect). There are, however, a number of problems with the α effect and dynamo models. Two of them are that, in the case of the Sun, the obtained cycle periods are too short and the magnetic activity is not sufficiently concentrated at low latitudes.

Key concepts: Physics, Dynamo, Differential rotation, Astrophysics, Dynamo theory, Stellar rotation, Solar dynamo, Context (archaeology)

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