Properties of low altitude plasma jets associated with Type III Radio Bursts and UV to X-ray Emissions

Magnetic reconnection is still not an understood process for the conversion of magnetic field energy into plasma motion and energised / heated plasma during solar events. The standard picture involves two plasmas with antiparallel magnetic fields ≤B moving together, resulting in a current sheet along their joint boundary. Triggered by reconnection the magnetic field lines are changing into a different topology. Accelerated particles escape along the new magnetic field lines forming visible pairs of jets, with one jet on each side of each end of the current sheet. In this work we will show a direct evidence of magnetic reconnection events in new SDO observations of the double-sided jets. The radio, EUV, optical and X-ray observations provide strong evidence for the standard but long-unproven model that type III electrons are energised in or near reconnection regions, producing radio and X-ray emissions as they move away from and towards the Sun.

Based on a large set of data from the Atmospheric Imaging Assembly (AIA) and SECCHI instruments on NASA's SDO and STEREO B spacecraft; radio dynamic spectra and images from the Murchison Widefield Array (MWA), calibrated and background-subtracted dynamic spectra from the Learmonth radio spectrograph, and RHESSI spacecraft we will discuss the properties of the double jets.