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After describing the drivers of solar magnetism and convection in the first course, we will take more altitude in the solar atmosphere and reach the chromosphere. The steep drop in density and pressure and the temperature-gradient reversal produce a complete change in the observable structures (network, spicules, plages, prominences), in the solar dynamics and in the electromagnetic spectrum (emission lines, radio flux). The chromosphere is also the atmospheric layer where the solar flares can be observed and have been systematically recorded over many decades, even before the advent of spaceflight. We will review flare properties as observed in the chromosphere, and we will explore how the mostly-mechanical energy coming from the underlying convection is transported and converted into heat dissipation and particle acceleration via magnetic fields in the chromosphere. We will finally reach the so-called transition region, this very thin sheath that forms the interface between the chromosphere and the extremely hot corona, which will be our next stop in this outward journey through the Sun.
This seminar is the second of a series of seminars on the basics of solar and heliospheric physics, aimed at our ROB, IASB and RMI colleagues who have a sound knowledge of physics and mathematics but never had a formal education in solar and heliospheric physics. These talks will provide an overview of the most important aspects without going in too much detail. References for further reading are provided.