Relaxation of magnetic field relative to plasma density during solar flares

Transition Region Emission and Energy Input to Thermal Plasma During the Impulsive Phase of Solar Flares

The energy released in a solar flare is partitioned between thermal and nonthermal particle energy and lost to thermal conduction and radiation over a broad range of wavelengths. It is difficult to determine the conductive losses and the energy radiated at transition region temperatures during the impulsive phases of flares. We use UVCS measurements of O VI photons produced by 5 flares and subs...

Relative Timing of Solar Flares Observed at Different Wavelengths

The timing of 503 solar flares observed simultaneously in hard X-rays, soft X-rays and Hα is analyzed. We investigated the start and the peak time differences in different wavelengths, as well as the differences between the end of the hard X-ray emission and the maximum of the soft X-ray and Hα emission. In more than 90% of the analyzed events, a thermal preheating seen in soft X-rays is presen...

Reconstruction of Solar Coronal Linear Force-Free Magnetic Field

Magnetic Field Amplification and Blazar Flares

Recent multiwavelength observations of PKS 0208-512 by SMARTS, Fermi, and Swift revealed that γ-ray and optical light curves of this flat spectrum radio quasars are highly correlated, but with an exception of one large optical flare having no corresponding gamma-ray activity or even detection. On the other hand, recent advances in SNRs observations and plasma simulations both reveal that magnet...

Solar flares as cascades of reconnecting magnetic loops.

A model for the solar coronal magnetic field is proposed where multiple directed loops evolve in space and time. Loops injected at small scales are anchored by footpoints of opposite polarity moving randomly on a surface. Nearby footpoints of the same polarity aggregate, and loops can reconnect when they collide. This may trigger a cascade of further reconnection, representing a solar flare. Nu...