Energy transfer from the photosphere to the corona: observational aspects
Abstract
The outer solar atmosphere, and indeed the entire heliosphere, is powered by the reservoir of non-radiative energy that exists in the forms of electromagnetic field and kinetic energy below the solar surface. A small fraction of that reservoir leaks away into the solar corona where it powers the EUV and X-ray glow, the solar wind, and on occasion large flares. I will review observational constraints on the physical pathways that are most important in this coupling, guided by theoretical consideration. I will focusing in particular on recent space-based observations by IRIS, Hinode, and SDO that together cover the domain from below the solar surface into the the high corona.
- Publication:
-
40th COSPAR Scientific Assembly
- Pub Date:
- 2014
- Bibcode:
- 2014cosp...40E2936S