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We have found remarkably different manifestations of a bright point flare in X‐ray and radio (microwave) wavelengths, unlike previous observations. In X‐rays, the BP flare was relatively simple while in radio, the bright point flare had a large scale component and a transient moving component. The large scale structure may be the radio counterpart of large scale structures sometimes seen during X‐ray BP flares. The transient component was also compact and moved away from the location of the X‐ray BP flare with a speed of ∼60 km s−1. The compact source also showed fast time structure which suggests nonthermal emission mechanism for the transient sources.

We have provided evidence that certain coronal X‐ray structures such as flaring X‐ray bright points and X‐ray jets give rise to nonthermal radio emission in the form of metric type III bursts. We have shown an example of a metric type IV/flare continuum being associated with the rupture of a flaring loop‐top and the ejection of X‐ray emitting material.

Flare blast waves and shocks piston driven by coronal mass ejections (CMEs) have been proposed to be responsible for generating type II radio bursts in the solar corona. The idea for piston‐driven shocks came primarily from temporal association of shocks and CMEs. Our compilation of CME events with simultaneous radio observations with positional information supports idea of flare blast waves.

The Solar Probe will deliver a 133.5 kg science payload into a 4 R(S) perihelion solar polar orbit to explore in situ one of the last frontiers in the solar system - the solar corona. Using a payload of 12 scientific experiments, it will be possible to answer many long-standing fundamental problems concerning the structure and dynamics of the outer solar atmosphere, including the acceleration, storage, and transport of energetic particles near the sun and in the inner heliosphere.