Magnetohydrodynamic modeling of coronal bright points

Details Magnetohydrodynamic modeling of coronal bright points Magnetohydrodynamic modeling of coronal bright points

Aug 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...319..971w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 319, Aug. 15, 1987, p. 971-983.

Computer Science

Numerical Analysis

9

Magnetohydrodynamics, Solar Corona, Solar Wind, Stellar Models, Chemical Composition, Density Distribution, Numerical Analysis, Photosphere, Solar Magnetic Field, Velocity Distribution

Scientific paper

Coronal bright points are known to be magnetic in nature. The authors have developed a two-dimensional MHD code to investigate the response of a stratified atmosphere to a localized magnetic structure. If a bright point occurs at a region where flux tubes of opposite polarity have encountered by chance, in the presence of stratification, a net upward mass flux results. Upflow velocities of up to one half of the Alfvén speed are produced. The implications of these results for mass outflows from bright points in coronal holes are discussed.

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