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The Hydrodynamic Evolution of Impulsively Heated Coronal Loops: Explicit Analytical Approximations

  • Authors: Markus J. Aschwanden and David Tsiklauri

ASCHWANDEN & TSIKLAURI 2009 The Astrophysical Journal Supplement Series 185 171.

  • Provider: AAS Journals

Caption: Figure 5.

Maximum density enhancement with respect to the RTV density, n p / n RTV as a function of the ratio of loop half-length to heating scale height, L/ s H , for a set of eight hydrodynamic numerical simulations performed by Tsiklauri et al. (2004), for s H = 8.75 Mm and loop half-lengths of L = 9, ..., 55 Mm (diamonds). The scaling law of Serio et al. (1981) yields consistent predictions for L/ s H gsim 3, but overpredicts the density enhancements for higher values of L/ s H gsim 3 where no stationary loop solutions exist due to the Rayleigh–Taylor instability. Numerical hydrodynamic simulations yield maximum density enhancements of n p / n RTV ≲ 2 for stationary solutions (Winebarger et al. 2003a, 2003b). For dynamic simulations of impulsive heating and subsequent cooling maximum (Tsiklauri et al. 2004), maximum density enhancements of n max/ n RTV ≈ 0.5(1 + L/ s H ) are obtained.

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