Dynamical model of the interaction between the magnetic field and the mass motions in solar active regions

Details Dynamical model of the interaction between the magnetic field and the mass motions in solar active regions Dynamical model of the interaction between the magnetic field and the mass motions in solar active regions

Aug 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...164..377b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 164, no. 2, Aug. 1986, p. 377-382.

Astronomy and Astrophysics

Astrophysics

2

Solar Activity, Solar Magnetic Field, Stellar Models, Sunspots, Dynamic Models, Magnetohydrodynamics, Mass Flow, Time Dependence

Scientific paper

The necessity of including a time dependence in the usual MHD equations (incompressible, infinite conductivity) for a realistic description of the interaction between the magnetic field and mass motions in sunspots is demonstrated. The essence of the nonlinear coupling is first examined through a particular class of solutions, separable with respect to time and space variables. The classical Evershed flow is recovered, and time-decay laws in tanh t and 1/cosh t for the magnetic and the velocity fields (respectively) are found. This shows that these two fields are anticorrelated in time. A more physical model is then built, which expresses the vectors V and B as functions of potentials U, A, and B. It appears that the property derived in a previous work (Berton, 1985), namely that the vectors V and B lie in the same vertical plane, is a condition of stationarity for the horizontal field Bh, and should be violated for time-dependent fields to occur.

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