Conveners
Poster Session 8.5
- Alessandro Bemporad (Istituto Nazionale di Astrofisica (INAF))
We present high-resolution and multiline spectropolarimetric observations of a C2-class solar flare (SOL2019-05-06T08:47). The rise, peak, and decay phases of the flare were recorded continuously and simultaneously in the Ca II K, Ca II 8542 Å, and Fe I 6173 Å lines with the CRISP and CHROMIS instruments at the Swedish Solar Telescope. At the flare footpoints, a non-LTE multiline inversion...
In the standard eruptive flare model, magnetic reconnection originates in a thin current sheet; created by the inflow of oppositely orientated magnetic fields under a rising magnetic flux rope. The current sheet is notoriously difficult to observe directly, primarily due to the small size of the region. However, insights into current sheet dynamics can be revealed by the behaviour of flare...
The chromospheric hydrogen Lyman-alpha line at 1216A is the brightest emission line in the solar spectrum, and yet studies of solar flares at this wavelength have been scarce in the recent literature. Changes in the Sun’s Lyman-alpha output can drive changes in the dynamics and composition of planetary atmospheres, and Lyman-alpha is also a significant radiator of solar flare energy providing...
ASPIICS/Proba-3 is a giant white-light coronagraph developed by ESA and will be launched in mid-2013. Proba-3 will consists from two satellites flying synchronously, the first one carrying the external occulter (EO) and the second one ~150 behind, carrying the optical telescope. The telescope will be placed in the shadow of the EO with high accuracy. The coronagraph is equipped with a filter...
The Lyman Continuum (LyC; 912Å) is the free-bound transition of a free electron to the ground state of an ambient Hydrogen nuclei. LyC has been shown to be a powerful tool for probing the chromospheric plasma conditions during solar flares. By fitting the LyC spectrum, the departure coefficient of hydrogen, b1, and the colour temperature, Tc, can be determined. Where b1 is a measure of the...
Type II solar radio bursts are believed to be caused by magnetohydrodynamics (MHD) shock-accelerated electrons in the solar corona. Often type II radio bursts can display fine structure in dynamic spectra. However, the cause of this fine structure and its relation to the shock is currently unclear. Here we present results from imaging analysis of type II radio burst fine structures observed by...
