Energy balance in a magnetically confined coronal structure observed by OSO-7

Details Energy balance in a magnetically confined coronal structure observed by OSO-7 Energy balance in a magnetically confined coronal structure observed by OSO-7

Aug 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975soph...43..359n&link_type=abstract

Solar Physics, vol. 43, Aug. 1975, p. 359-376.

Physics

23

Energy Transfer, Force-Free Magnetic Fields, Oso-7, Solar Corona, Solar Magnetic Field, Solar Spectra, Energy Dissipation, Energy Distribution, Far Ultraviolet Radiation, Heat Flux, Magnetic Field Configurations, Magnetohydrodynamic Waves, Satellite Observation, Solar Flux, Spectroheliographs, Stellar Structure, Ultraviolet Spectroscopy, X Ray Spectroscopy

Scientific paper

A model of a coronal region of enhanced Fe XV and Fe XVI emission is developed and its energy balance is examined using extreme ultraviolet observations from OSO-7 together with calculations of possible force-free coronal magnetic field configurations. The coronal emissions overlying the photospheric boundary between regions of opposite magnetic polarity are found to be associated with generally nonpotential (current-carrying) magnetic fields in the forms of arches with footpoints in regions of opposite polarity. The orientation of these arches relative to the neutral line changes with degree of ionization of the emitting ion (which we infer from our limb observations to be a function of height) and may be evidence of differing electric currents along various field lines. The appearance of a coronal arch, seen side-on, can conveniently be represented by a parabola and a detailed analysis shows this to be a realistic approximation that should be generally useful in analyzing two-dimensional pictures of coronal structures.

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