Emission Measures and Heating Mechanisms for Stellar Transition Regions and Coronae

TL;DRAbstract

In order to determine the heating mechanisms for stellar transition regions and coronae we try to determine the damping lengths for the mechanical flux(es) responsible for the heating. For the lower part of the transition regions (30,000 < T≤100,000 K) the damping lengths are consistent with Shockwave damping. This appears to be also true for the upper part of the transition region in Procyon, while for the upper part of the solar transition region the damping length is much larger.

Chat with Paper

AI Agents for this Paper