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On the Anisotropy in Expansion of Magnetic Flux Tubes in the Solar Corona

  • Authors: A. Malanushenko and C. J. Schrijver

Malanushenko & Schrijver 2013 The Astrophysical Journal 775 120.

  • Provider: AAS Journals

Caption: Figure 20.

Model of how the emission measure scales with height for the flux tubes in Figure 19. The functions plotted are n 2 (dotted line), n 2 B −1/2 (dashed line), and n 2 B −1 (solid line). We assume a hydrostatic atmosphere n∝exp (− z/ z 0) with z 0 = 50 Mm for all curves and the field strength dropping like that of a point dipole, B( z) = z 0/ z 3 (the constant for B is chosen such that all three curves intersect at one density scale height).

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