Conveners
Poster Session 2.6
- Istvan Ballai (University of Sheffield)
Solar electrons beams are accelerated in the corona, into the solar wind and beyond in the Solar system through eruptive mechanisms at the surface of the Sun such as flares. These beams of non-thermal electrons evolve as a function of distance from the Sun, interacting with the background plasma and growing Langmuir waves as they propagate. Subsequent radio and X-ray wavelength emission is...
This contribution focus on the analysis of the distribution function of different physical magnitudes of the solar wind. The data set comes from the ACE spacecraft located at the L1 point and covers almost two solar cycles, from 1998 to 2017.
We propose a bi-Gaussian distribution, formed by the addition of two Gaussian distribution functions, to characterize the solar wind. Each Gaussian...
High-energy particles penetrate spacecraft and to a different extent affect the performance of instruments flown on board space missions. Consequently, spacecraft carry particle detectors for both diagnostics and scientific purposes that allow to monitor the galactic cosmic-ray and solar energetic particle fluxes during the whole mission elapsed time. These data allow us to disentangle long...
Coronal Mass Ejections (CMEs) are some of the most energetic solar events that expel plasma and magnetic field into the interplanetary medium. Stealth CMEs represent a special type of solar eruptions that, in most cases, can be clearly seen in coronagraph observations, but lack distinct source signatures. We simulate consecutive CMEs ejected from the southernmost part of an initial...
The observations of the resonantly scattered ultraviolet emission of the coronal plasma obtained with UVCS-SOHO, properly designed to measure the wind outflow speed by applying the Doppler dimming diagnostics, noticeably fostered the investigation of the wind in the inner solar corona. Metis on Solar Orbiter complements the UVCS spectroscopic observations, by simultaneously imaging the...
Both coronal holes and active regions are source regions of the solar wind. The distribution of these coronal structures across both space and time is well known, but it is unclear how much each source contributes to the solar wind.
We have used photospheric magnetic field maps from the past four solar cycles to estimate what fraction of magnetic open solar flux is rooted in active regions,...
Interest in predicting space weather conditions constantly pushes the advance of state-of-the-art three-dimensional(3D) magnetohydrodynamic (MHD) models of the solar corona and the solar wind, which need to be validated with observational data. Tomography of the solar corona is the only observational technique that can currently provide empirical data of the solar atmosphere in a 3D global...
