Emergence of solar magnetic flux from the convection zone into the photosphere and chromosphere

Journal Article · Thu Mar 01 04:00:00 EST 1990 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/185671· OSTI ID:6851584

Shibata, K; Nozawa, S; Matsumoto, R; Sterling, A C; Tajima, T ^[1]

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1. Aichi Univ. of Education, Kariya (Japan) Texas Univ., Austin (USA) Chiba Univ. (Japan) Kyoto Univ. (Japan)

A two-dimensional MHD code is used to study the nonlinear dynamics of solar magnetic flux emerging from the convection zone into the photosphere and chromosphere. An isolated horizontal magnetic flux with beta of about 4 is initially located in a convectively unstable layer (solar convection zone) beneath a two-temperature layered atmosphere (solar corona-chromosphere/photosphere). The combined effects of convection and magnetic buoyancy carry the magnetic flux from the convection zone into the photosphere, where it then expands through the photosphere and chromosphere. Gas slides down the expanding loop, resulting in its evacuation and subsequent rise due to enhanced magnetic buoyancy. Initially, weak convection zone magnetic flux (B of about 600 G) is amplified up to 1000 G or more after emerging into the photosphere. The resulting velocity fields are similar to those observed in arch filament systems. 19 refs.

• OSTI ID: 6851584
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 351; ISSN ASJOA; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
CHROMOSPHERE
CONVECTION
ENERGY TRANSFER
FLUID MECHANICS
HEAT TRANSFER
HYDRODYNAMICS
MAGNETIC FIELDS
MAGNETIC FLUX
MAGNETOHYDRODYNAMICS
MAIN SEQUENCE STARS
MASS TRANSFER
MECHANICS
NONLINEAR PROBLEMS
PHOTOSPHERE
SOLAR ATMOSPHERE
SOLAR FLUX
STABILITY
STARS
SUN
TWO-DIMENSIONAL CALCULATIONS
VELOCITY