TY - JOUR

T1 - Non-local memory effects of the electromotive force by fluid motion with helicity and two-dimensional periodicity

AU - Hori, Kumiko

AU - Yoshida, Shigeo

N1 - Funding Information:
We thank Professor Sei-ichiro Watanabe and two anon-ymous reviewers for helpful comments. This study was partly supported by the 21st Century COE Program ‘‘Dynamics of the Sun–Earth–Life Interactive System (SELIS)’’ of Nagoya University, Inoue Foundation for Science and Center for Computational Astrophysics, CfCA, of National Astronomical Observatory of Japan. A part of the numerical computations were carried out on general common use computer system at CfCA. Data visualization of figure 19 was carried out on general common use computer system at the Information Technology Center, Nagoya University.
Copyright:
Copyright 2008 Elsevier B.V., All rights reserved.

PY - 2008

Y1 - 2008

N2 - In mean-field dynamo theory, the electromotive force term 〈u′× B′〉 due to small-scale fields connects the small-scale magnetic field with the large-scale field. This term is usually approximated as the α-effect, assumed to be instantaneous in time and local in space. However, the approximation is valid only when the magnetic Reynolds number Rm is much less than unity, and is inappropriate when Rm ≳1, which is the condition satisfied in the Earth's core or solar convection zone. We introduce a function φqr as a non-local and non-instantaneous generalization of the usual α-effect and examine its behaviour as a function of Rm in the range 1/64 ≤Rm ≤10 for a kinematic dynamo model. We use the flow of G.O. Roberts 1972 (Phil, Trans. Roy. Soc. London Ser. A, 1972, 271, 411-454), which is steady and has non-zero helicities and two-dimensional periodicity. As a result, we identify three regions in Rm space according to the behaviour of the function φqr: (i) Rm ≲ 1/4, where the function φqr is local and instantaneous and can be approximated by the traditional α and β effects, (ii) 1/4 ≲ Rm ≲ 4, where the deviation from the traditional α and β effects increases and non-localness and non-instantaneousness increase, and (iii) Rm ≳ 4, where boundary layers develop fully and non-localness and non-instantaneousness are prominent. We show that the non-local memory effect for Rm ≳ 4 strongly affects the dynamo action and explains an observed augmentation of the growth rate in the dispersion relation. The results imply that the non-local memory effect of the electromotive force should be important in the geodynamo or the solar dynamo.

AB - In mean-field dynamo theory, the electromotive force term 〈u′× B′〉 due to small-scale fields connects the small-scale magnetic field with the large-scale field. This term is usually approximated as the α-effect, assumed to be instantaneous in time and local in space. However, the approximation is valid only when the magnetic Reynolds number Rm is much less than unity, and is inappropriate when Rm ≳1, which is the condition satisfied in the Earth's core or solar convection zone. We introduce a function φqr as a non-local and non-instantaneous generalization of the usual α-effect and examine its behaviour as a function of Rm in the range 1/64 ≤Rm ≤10 for a kinematic dynamo model. We use the flow of G.O. Roberts 1972 (Phil, Trans. Roy. Soc. London Ser. A, 1972, 271, 411-454), which is steady and has non-zero helicities and two-dimensional periodicity. As a result, we identify three regions in Rm space according to the behaviour of the function φqr: (i) Rm ≲ 1/4, where the function φqr is local and instantaneous and can be approximated by the traditional α and β effects, (ii) 1/4 ≲ Rm ≲ 4, where the deviation from the traditional α and β effects increases and non-localness and non-instantaneousness increase, and (iii) Rm ≳ 4, where boundary layers develop fully and non-localness and non-instantaneousness are prominent. We show that the non-local memory effect for Rm ≳ 4 strongly affects the dynamo action and explains an observed augmentation of the growth rate in the dispersion relation. The results imply that the non-local memory effect of the electromotive force should be important in the geodynamo or the solar dynamo.

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U2 - 10.1080/03091920802260466

DO - 10.1080/03091920802260466

M3 - Article

AN - SCOPUS:56549107284

VL - 102

SP - 601

EP - 632

JO - Geophysical and Astrophysical Fluid Dynamics

JF - Geophysical and Astrophysical Fluid Dynamics

SN - 0309-1929

IS - 6

ER -