Speaker
Description
Solar prominences are composed of thin threads that outline particular magnetic field lines of the prominence structure. Observations have shown the presence of Alfvénic waves in threads, which are probably driven at the photosphere. Wave dissipation could be a relevant heating mechanism in prominences. In this work, we construct 1D equilibrium models of partially ionized prominence threads that satisfy an energy balance between radiative cooling, thermal conduction and, optionally, Alfven wave heating. The obtained models have a cold region, corresponding to the thread itself, an extremely thin prominence-corona transition region, and a coronal region. The properties of the equilibria are explored by performing a parameter survey. For instance, the thread length decreases with increasing central temperature. When wave heating is included, we find that the thread length increases with the wave energy flux, and no equilibrium is possible when the wave heating rate is larger than radiative losses at the thread core. Additionally, the effects of gravity and the magnetic field geometry are investigated.
| Sessions | Wave generation, energy transport, dissipation and heating |
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