The corona temperature distribution produced by the DYN model


Speaker: Thanassis Katsiyannis


The detection of ultra-relativistic electrons in low Earth orbit


Speaker: Thanassis Katsiyannis


Ionospheric sporadic layers at middle latitudes


Speaker: Zbysek Mosna


First estimation of the suprathermal electron momentum in the upper ionosphere


Speaker: Hanane Marif


The ionospheric electron population is divided into two groups. The ambient electrons are thermalized. Their energy is usually smaller than one electronvolt. Their densities and temperatures are the usual ones measured by incoherent scatter radars, or modelled by international codes such as IRI. 

The auroral polarisation: A new measurement technique for monitoring the upper atmosphere


Speaker: Jean Lilensten


For the last years, we have been discovering the polarisation of the auroral red line both in the cusp (Svalbard) and in the auroral oval (Skibotn). We have proven that its Degree of Linear Polarisation (DoLP) varies accordingly to the geomagnetic activity. In the last 2 winters, two major steps have been achieved, that will be reported in this contribution.

My work at SIDC: how can it benefit your work?


Speaker: Cis Verbeeck


As project manager of EUI at ROB, my main task is to coordinate scientific, technical and operational aspects of EUI, including active participation in the EUI Consortium and Solar Orbiter community.

The editorial office of the SWSC Journal - An inside look


Speaker: Jan Janssens


Lessons learned by analysing LASCO images


Speaker: Marilena Mierla


LASCO instrument onboard SOHO mission has different filters and polarisers to observe the solar corona. These images are analysed in order to see the differences among them. Aspects like signal to noise, background intensities etc. are detailed and discussed. The work is done in preparation for the PROBA3 mission.

Date: 6 May 2015

How to do 3D reconstruction of CMEs


Speaker: Marilena Mierla


In this seminar I will present various 3D reconstruction methods for coronal mass ejections (CMEs).

The most popular one is triangulation (Inhester 2006), using view directions from two spacecraft. The method consists in identifying the same object in a pair of images, by calculating the lines of sight that belong to the respective pixels in the image and back-tracking them into the 3D space.

What do we see in white-light coronagraph images?


Speaker: Marilena Mierla


1. The components of the solar corona   2. The coronagraph   3. Data pre-processing   4. CME visualization   5. Thomson scattering   6. H-alpha emission in WL coronagraph images   7. CME propagating into the heliosphere   8. Summary 

Date: 15 May 2013



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