According to our current understanding, solar flares occur when magnetic energy stored in the solar corona is rapidly converted into other forms. This process appears to be initiated by, if not fully explained by, fast magnetic reconnection occurring somewhere in the corona. I will describe some physical constraints on the process of energy release and conversion. First, magnetic energy...
Solar eruptive events are characterized by a complex interplay of energy release, transport, and conversion processes. A quantitative characterization of the different forms of energy therefore represents a crucial observational constraint for models of solar eruptions in general, as well as for magnetic reconnection, heating, and particle acceleration processes in particular. This talk will...
One of the striking observations from the NASA Parker Solar Probe (PSP) spacecraft is the prevalence in the inner heliosphere of large amplitude, Alfvenic magnetic field reversals termed 'switchbacks'. These $\delta B_R/B \sim \mathcal{O}(1$) fluctuations occur on a range of timescales, are spherically polarized, and occur in "patches" separated by intervals of more quiet, radial solar wind...
The large-scale magnetic configuration and plasma beta of solar flares are similar to those of the magnetotail during reconnection. Studies of suprathermal electrons in the magnetotail may thus shed light on suprathermal electron production during flares. We will discuss statistical analysis and case studies of MMS magnetotail measurements to test out the following: (1) whether the primary...
Solar flares release tremendous amounts of energy which is transported through the various layers of the Sun's atmosphere, resulting in heating, ionisation, mass flows, and non-thermal effects. The response of the plasma is detected by the radiation it produces. Often the radiation emitted during flares is formed under complex conditions, requiring forward modelling to guide the...
