Plasma Condensation in Solar Coronal Loops -- I. Basic Processes

Physics

Scientific paper

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Sun: Corona, Sun: Transition Region, Sun: Uv Radiation

Scientific paper

In the first part of this work, we report numerical calculations of the condensation of plasma in short coronal loops, which has several interesting physical consequences. We propose a connection between small, cool loops, which presumably constitute the solar transition region, and prominences in the sense that the same physical mechanism governs their dynamics, namely the onset of instability and runaway cooling due to strong radiative losses. We show that the temporal evolution of these loop models exhibits a cyclic pattern of chromospheric evaporation, condensation, motion of the condensation region to either side of the loop, and finally loop reheating with a period of 4000 - 8000 s for a loop of 10 Mm length. Furthermore, we have synthesized transition region lines from these calculations which show strong periodic intensity variations, making condensation in loops a candidate to account for observed transient brightenings of solar transition region lines. Remarkably, all these dynamic processes take place for a heating function which is constant in time and has a simple exponential height dependence. In the second part of this work (Müller et al., 2003b), we apply this concept to large coronal loops.

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