Conveners
Day 2 / Session 2
- Prayash Sharma Pyakurel (UC Berkeley)
Magnetic reconnection is a significant driver of energetic particles in flares both on the sun and the broader universe. Single x-line models fail to explain the large number of energetic electrons seen in flares. However, simulations reveal that reconnection becomes turbulent in the flare environment, consistent with observations of non-thermal broadening of spectral lines. Magnetic energy...
Magnetic reconnection is a ubiquitous astrophysical process that rapidly converts magnetic energy into some combination of plasma flow energy, thermal energy, and non-thermal energetic particles, including energetic electrons. Various reconnection acceleration mechanisms in different low-beta and collisionless environments have been proposed theoretically and studied numerically. However, none...
Nature's most powerful high-energy sources are capable of accelerating particles to high energy and radiate it away on extremely short timescales, even shorter than the light crossing time of the system. It is yet unclear what physical processes can produce such an efficient acceleration, despite the copious radiative losses. By means of fully-kinetic particle-in-cell simulations that include...
Fully convective M dwarfs display a diversity of magnetic phenomena, motivating questions of how these stars generate and sustain large scale coherent magnetic fields. We present an observational study that characterizes the relationship between age, stellar rotation, flares, and chromospheric activity for the volume-complete sample of M dwarfs with masses between 0.1 and 0.3 solar masses that...
