Emilie Richer

• PhD in Physics
• Laboratoire de Physique des Plasmas, French National Centre for Scientific Research

The interaction of the solar wind (SW) with the magnetic field of The analysis of MESSENGER orbital observations led Anderson et al (2011) to propose a dipole centered on the spin axis of the planet with a northward offset equal to 484±11 km to represent the intrinsic magnetic field of Mercury at northern latitudes higher than 30°. The magnetic mom...

The interaction of the solar wind (SW) with the magnetic field of Mercury is investigated by means of a three dimensional parallelized multispecies hybrid model. A comparison between two mathematical representations of Mercury's intrinsic magnetic field is studied. The first model is an Offset Dipole (OD) having the offset and dipolar moment report...

The purpose of this work is to study the interactions between the Solar Wind (SW) and Mercury and/or Mars by means of numerical simulations. In the context of previous observations made Mariner 10 and MESSENGER, and the preparation of the future mission Bepi Colombo, we developed a three-dimensional and parallel hybrid model of the interaction of t...

The reflection of solar wind protons on the Martian bow shock (BS) is investigated by means of three-dimensional simulation models. A two steps approach is adopted to allow a detailed analysis of the reflected population. Firstly, the 3-dimensional hybrid model of Modolo et al. (2005) is used to compute a stationary state of the interaction of the...

In the frame of the HELIOSARES project (PI F.Leblanc) dedicated to the modeling of Mars environment (neutral and charged species) from the lower atmosphere to the solar wind, a modeling effort has been conducted to parallelize a multi-species hybrid simulation code. This code now provides a kinetic description of the ions with a rather improved spa...

The three flybys of Mariner 10, the numerous terrestrial observations of Mercury's exosphere and the recent flybys of MESSENGER [1] have brought important information about the Hermean environment. Mercury's intrinsic magnetic field is principally dipolar and its interaction with the Solar Wind (SW) creates a small and very dynamic magnetosphere. M...

Due to the absence of strong intrinsic magnetic field, the Martian atmosphere/exosphere is directly in contact with the Solar Wind, exchanging part of its momentum and energy. This coupling occurs via ionization processes and contributes to the erosion of the neutral environment of the planet. Several space missions (past, active and future), such...

Ganymede is the only magnetized moon in the solar system embedded in its large parent's planet magnetosphere. Its internal magnetic field interacts strongly with the Jovian magnetospheric plasma and makes unique this interaction. Thermal magnetospheric ions co-rotate at about 180km/s and are mainly composed of oxygen ions and protons. Few MHD model...

Ganymede is the only magnetized moon in the solar system embedded in its large parent's planet magnetosphere. Its internal magnetic field interacts strongly with the Jovian magnetospheric plasma and makes unique this interaction. Thermal magnetospheric ions co-rotate at about 180km/s and are mainly composed of oxygen ions and protons. Few MHD model...

When the solar wind interacts with a small obstacle like Mars, protons and alpha particles behave quite differently at scales of the order of the size of the obstacle. Although alpha particles can contribute up to about 20% to the solar wind momentum and energy flux their contribution to the interaction has not yet been investigated. Meanwhile rece...

Having run a self-consistent three-dimensional simu-lation of the Martian bow shock we subsequently in-vestigate the reflection of solar wind protons on the planetary bow shock by means of test particles mov-ing in the stationnary electromagnetic field generated during the self-consistent simulation. This two-step approach allows to identify reflec...