Name: Geomagnetic storms and solar eruptions: from Sun to Earth
Start: 2017-01-31T09:30:00+01:00
End: 2017-01-31T15:30:00+01:00
Location: Space Pole

Geomagnetic storms and solar eruptions: from Sun to Earth

Tuesday, 31 January 2017 - 09:30

Monday, 30 January 2017
Tuesday, 31 January 2017

09:30 Coffee & Welcome
Coffee & Welcome
09:30 - 10:00
Room: RMI meeting room
10:00 Modeling Space Weather from the Sun to Earth and beyond - Raluca Ilie (University of Illinois at Urbana-Champaign)
Modeling Space Weather from the Sun to Earth and beyond
- Raluca Ilie (University of Illinois at Urbana-Champaign)
10:00 - 10:40
Room: RMI meeting room Developed at University of Michigan, the Space Weather Modeling Framework (SWMF) is a high-performance, flexible and robust computational framework designed for simulating the global space environment. SWMF integrates numerical models from numerous physics domains that can be customized to self-consistently simulate physical processes and coupled domains from the solar surface to the upper atmosphere of the Earth and extending to many planetary environments. This allows studying these complex, multi-scale space plasmas and their interactions on a system level, promoting a global understanding of the processes driving space weather, and advancing us toward physics-based prediction of the near-Earth environment. This presentation will illustrate recent advancements made within the SWMF, with a focus on the Geospace Suite, allowing for enhanced modeling and predictive capabilities, thanks to a suite of self-consistently coupled, first-principle models describing these interconnected and collocated plasma environments. The Geospace Suite consists of the Global Magnetosphere, Inner Magnetosphere, Ionosphere Electrodynamics and Polar Wind Outflow modules and is primarily used to describe and predict the conditions in the near- Earth environment.
10:40 Q&As
Q&As
10:40 - 10:45
Room: RMI meeting room
10:45 Coronal Mass Ejections and Geomagnetic Storms - Marilena Mierla (Royal Observatory of Belgium)
Coronal Mass Ejections and Geomagnetic Storms
- Marilena Mierla (Royal Observatory of Belgium)
10:45 - 11:05
Room: RMI meeting room Coronal mass ejections (CMEs) are huge expulsions of plasma and magnetic field from the Sun into the interplanetary space. When interacting with the Earth's magnetosphere they can create major geomagnetic storms which can have a direct impact on our technological life. In this presentation a summary on the recent results regarding the propagation of CMEs and their impact on the magnetosphere will be given. The limitations of the actual observations and models used for forecasting the arrival time of the CMEs to the Earth will be also outlined.
11:05 Q&As
Q&As
11:05 - 11:10
Room: RMI meeting room

11:10 Coffee
Coffee
11:10 - 11:25
Room: RMI meeting room
11:25 Space Weather Effects in the Earth's Ionosphere and Below: An Overview of the NASA ICON Mission and Recent Insights on Geomagnetically Induced Currents - Farzad Kamalabadi (University of Illinois at Urbana-Champaign)
Space Weather Effects in the Earth's Ionosphere and Below: An Overview of the NASA ICON Mission and Recent Insights on Geomagnetically Induced Currents
- Farzad Kamalabadi (University of Illinois at Urbana-Champaign)
11:25 - 12:05
Room: RMI meeting room
12:05 Q&As
Q&As
12:05 - 12:10
Room: RMI meeting room
12:10 Double layers in the upward and downward current regions of the aurora - Herbert Gunell (Belgian Institute for Space Aeronomy)
Double layers in the upward and downward current regions of the aurora
- Herbert Gunell (Belgian Institute for Space Aeronomy)
12:10 - 12:30
Room: RMI meeting room
12:30 Q&As
Q&As
12:30 - 12:35
Room: RMI meeting room
12:35 Geomagnetic storms: New results obtained with the "Energetic Particle Telescope" (EPT) along the LEO of PROBA-V. - Joseph Lemaire (BIRA-IASB, Université catholique de Louvain)
Geomagnetic storms: New results obtained with the "Energetic Particle Telescope" (EPT) along the LEO of PROBA-V.
- Joseph Lemaire (BIRA-IASB, Université catholique de Louvain)
12:35 - 12:55
Room: RMI meeting room With contributions from Benck, S. [2], Lopez-Rosson, G. [1] and Pierrard, V. [1][2] [1] BIRA-IASB [2] Center for Space Radiations, UCL, Louvain-La-Neuve Since May 2013, the Energetic Particle Telescope (EPT) is orbiting on a polar LEO at 820 km altitude, on board of PROBA-V (Cyamukungu et al., 2014 & Pierrard et al., 2014 respectively for the instrument description & preliminary results of the EPT). The fluxes of trapped electrons are measured by the EPT in 7 different energy channels ranging from 0.5 MeV to 20 MeV, We present the observations collected during the geomagnetic storm of 17 March 2015 (Dst: -231 nT), as well as during the two smaller storms in December 2015 (Dst = -45 nT & -150 nT). During the main phase of these storms, typical drop-outs are observed at low altitudes in all energy channels, in outer Radiation Belt drift shells (L > 4). Some of these drop-outs are followed by the penetration of relativistic electrons down to L = 2. The strong injection event of March 2015 filled up the slot region between the inner and outer Radiation Belts, for a period of a few days, as illustrated by the standard (L-t) maps that will be presented. These standard (L-t) maps also indicate that the outer belt electron fluxes were significantly enhanced after the geomagnetic storm, as compared to before the storm of March 2015. At the same time the MAGEIS/VAP-B detector, on board Van Allen Probes B flying along a GTO orbit, also observed enhanced relativistic electron fluxes after this storm event.Similar post-storm enhancements of energetic electron fluxes had been observed/reported earlier, but they had never been measured simultaneously (i) at low altitudes (along a LEO alike that of EPT/PROBA-V), and (ii) at large radial distances in the equatorial region (along a GTO orbit like that of MAGEIS/VAP-B). We will indicate how Betatron deceleration associated with the uplift of mirror points (during storm main-phases), and Betatron acceleration associated with a downward return of mirror points (during the recovery-phases) can explain the flux variations observed with the EPT. Indeed, the flux variations observed at low altitudes with the EPT are the consequence of Betatron deceleration and acceleration (also called Dst-effect) induced by the growth of the Ring Current, and by its subsequent decay during the slower recovery phase.The effect of concomitant non-resonant wave-particle interactions of whistler waves and ULF waves with trapped electrons during main-phases and recovery-phases, can account for enhancements of electron fluxes observed in the outer belt following some geomagnetic storm events. This is an alternative to the acceleration mechanism by resonant wave-particle interactions often invoked. Unlike the usual (B-L) flux maps, the EPT flux distributions are displayed in a new magnetic invariant coordinate system [Invariant-altitude (h_inv) & Magnetic-latitude (MagLat)] ; this coordinate system, which was introduced by Cabrera and Lemaire (2007), offers the key advantage to display more clearly and obviously low altitude distributions of trapped RB particles within McIlwain's reference dipole. Our (h_inv - MagLat) flux maps did enable us to uncover transient trapped electron populations during the main-phases of geomagnetic storms.
12:55 Q&As
Q&As
12:55 - 13:00
Room: RMI meeting room

13:00 Lunch
Lunch
13:00 - 14:00
Room: RMI canteen
14:00 CMEs and associated shock waves. Observations and Modelling with EUHFORIA. - Jasmina Magdalenic (Royal Observatory of Belgium)
CMEs and associated shock waves. Observations and Modelling with EUHFORIA.
- Jasmina Magdalenic (Royal Observatory of Belgium)
14:00 - 14:30
Room: RMI meeting room
14:30 Q&As
Q&As
14:30 - 14:35
Room: RMI meeting room
14:35 Predicting Geomagnetic Storms on the Basis of Solar Observations - Andrei Zhukov (Royal Observatory of Belgium)
Predicting Geomagnetic Storms on the Basis of Solar Observations
- Andrei Zhukov (Royal Observatory of Belgium)
14:35 - 14:55
Room: RMI meeting room
14:55 Q&As
Q&As
14:55 - 15:00
Room: RMI meeting room

15:00 Final Discussions
Final Discussions
15:00 - 15:30
Room: RMI meeting room