Abstract
The variation of the width of coronal current-carrying magnetic loops with height is considered. Two invariants are taken into consideration: conservation of the longitudinal magnetic field flow through the tube cross-section, and conservation of the electric current through the cross-section. It is shown that, if gas kinetic pressure inside the tube is low in comparison with the longitudinal magnetic field pressure, the tube width does not vary with height in the corona, which is typical for most magnetic loops observed in the corona. Otherwise, when the gas kinetic pressure exceeds the longitudinal magnetic field pressure, the tube width increases within the double scale of height of the inhomogeneous atmosphere. The increase in width with height is typical for certain postflare loops that feature higher parameters of temperature and plasma concentration.
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References
Aschwanden, M.J. and Hardi, P., The width distribution of loops and strands in the solar corona—are we hitting rock bottom?, Jan 4, 2017. https://arxiv.org/abs/1701.01177v1.
Aschwanden, M.J. and Nightingale, R.W., Elementary loop structures in the solar corona analyzed from trace triplefilter images, Astrophys. J., 2005, vol. 633, pp. 499–517.
Kano, R. and Tsuneta, S., Scaling law of solar coronal loops obtained with YOHKOH, Astrophys. J., 1995, vol. 454, pp. 934–944.
Katsukawa, J. and Tsuneta, S., Magnetic properties at footpoints of hot and cool loops, Astrophys. J., 2005, vol. 621, pp. 498–511.
Sharykin, I.N. and Kosovichev, A.G., Dynamics of electric currents, magnetic field topology, and helioseismic response of solar flare, Astrophys. J., 2015, vol. 808, no. 1, id 72.
Zaitsev, V.V. and Khodachenko, M.L., Energy release in corona magnetic loops, Radiophys. Quantum Electron., 1997, vol. 40, nos. 1–2, pp. 114–138.
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Zaitsev, V.V., Kronshtadtov, P.V. On the Constancy of the Width of Coronal Magnetic Loops. Geomagn. Aeron. 57, 841–843 (2017). https://doi.org/10.1134/S001679321707026X
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DOI: https://doi.org/10.1134/S001679321707026X