Conveners
Poster Session 4.6
- Istvan Ballai (University of Sheffield)
Interplanetary Coronal Mass Ejections (ICMEs) are among the main drivers of Space Weather and are responsible for the strongest variations in the near-Earth solar-wind conditions. Forecasting the Time of Arrival and Speed of Arrival of an ICME more than an hour ahead is a rather complicated task, since it means propagating a poorly determined plasma and magnetic field structure into an...
The determination of solar wind outflow velocity is fundamental to probe the mechanisms of wind acceleration in the corona. Using the Doppler dimming technique, we studied the effects that the chromospheric Lyα line profile shape causes on the determination of the outflow speed of coronal HI atoms. Starting from UV observations (SOHO/UVCS) of the coronal Lyα line and simultaneous measurements...
We analyze the measurements of the solar diameter made at the Basilica of San Petronio (Bologna, Italy) from 1655 to 1736 using a meridian line. This series includes the Maunder Minimum, a period of abnormally low solar activity between 1645 and 1715. Some authors have suggested an increase of the solar diameter during the Maunder Minimum. We have applied statistical analyses to compare the...
A pair of off-limb eruptions was observed by the Extreme Ultraviolet Imager (EUI) onboard Solar Orbiter (SolO) on 2021 April 23/24. At the time, the spacecraft was at 0.87 AU from the Sun. As seen from Earth, SolO was roughly near the Sun’s east limb (as seen from the Earth) and in quadrature with Parker Solar Probe (PSP), which was at the Sun’s far side. The eruptions are remarkably well...
We implemented multiple data analysis and machine learning algorithms to extract information of solar active regions that can be used in the future to perform CME and flare forecasting.
We use the data set produced by Angryk et al. (Sci.Data,2020) containing 51 magnetic field parameters and the associated X-ray activity of solar active regions from 2010 to 2018. We performed a data...
Solar flares are powered by the evolution of the magnetic field, but it is still impossible to deterministically predict whether an active region will flare or not solely based on photospheric information. Observational case studies of the upper solar atmosphere reveal increased levels of magnetic reorganization, dynamics, and temperature variation prior to solar flares. Whether such...
Solar flares have direct consequences on the Earth’s ionosphere. The enhancement of extreme ultraviolet (EUV) and X-ray emission during a flare results in the rapid increase of ionization on the entire dayside ionosphere causing a sudden ionospheric disturbance (SID). While SIDs occur in all regions of the ionosphere, the effect on the lowest-lying D-region (60-100km in altitude) is the most...
