34th Solar Physics Division Meeting, June 2003
Session 10 Transequatorial and other Coronal Structures
Oral, Tuesday, June 17, 2003, 9:00am-12:00noon, Auditorium

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[10.09] Can Steady-state Mass Flows Explain the Non-hydrostatic Cool EUV Coronal Loops in Active Regions?

S. Patsourakos, J. A. Klimchuk (NRL)

Recent EIT/TRACE observations of cool (\approx 1-1.5 MK) EUV coronal loops in active regions showed that these loops are very often characterized by greatly enhanced pressure scale-heights and densities compared to the predictions of static equilibrium theory. It has been suggested that mass flows may explain these over-dense and over-pressure loops. We investigate this conjecture by the means of 1D hydrodynamic simulations of steady-state mass flows in coronal loops. The mass flows in our calculations are driven by asymmetric heating that decreases exponentially along the loop from one footpoint all way to the other. By considering several representative cases for the magnitude and the length scale of the applied asymmetric heating, we determine how steady-state mass flows affect the thermodynamic structure of coronal loops and assess whether they can lead to enhanced pressure scale-heights and densities. Research supported in part by NASA and ONR.

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Bulletin of the American Astronomical Society, 35 #3
© 2003. The American Astronomical Soceity.