ESA spacecraft model magnetic boundaries

7 January 2011

In some respects, Earth and Venus may be regarded as near-twins, since they are similar in size, mass and internal structure. However, although the central region of each planet is iron-rich, Venus rotates very slowly compared with Earth and this affects the behaviour of its liquid metal core.

Whereas Earth's active internal dynamo is able to create an all-embracing magnetic field, Venus is unable to generate an internal magnetic field. As a consequence, Venus has a much smaller magnetosphere, which is induced by the interaction between the plasma in its sparse outer atmosphere and the solar wind.

Earth's magnetic environment and its interaction with the variable solar wind have been explored by orbiting spacecraft for decades, resulting in a good understanding of the location and width of the outer boundary of the magnetosphere, the so-called magnetopause. However, only a few spacecraft have orbited the second planet from the Sun, and there are still many gaps in our understanding of the Sun-Venus connection.

In order to fill some of the gaps in our knowledge, a team of European scientists have developed a model of the magnetopause, which takes into account the different plasma conditions at both planets. The study, published in the journal Planetary and Space Science, uses data obtained by ESA's Venus Express orbiter and the four spacecraft of ESA's Cluster flotilla in Earth orbit.

The team selected data collected on 27 June 2006 for their study. On that day, Venus Express crossed the planet's magnetopause several times, enabling it to sample not only the magnetic field but also the main properties of the electron and ion environment (density, bulk velocity and energy), as measured by the ASPERA-4 plasma instrument.

A few hours later, the Cluster quartet crossed the terrestrial magnetopause, on the dawn flank of the magnetosphere. Particle data from the Cluster ion spectrometer and magnetic field data from the magnetometer gave a multi-point description of the conditions at the edge of Earth's magnetic bubble.

The near-simultaneous joint observations by Venus Express and Cluster enabled the team to complete a comparative study of the solar wind interaction with the outer magnetospheric layers of Venus and Earth. The scientists were also able to compare the spacecraft data with the results of kinetic models of plasma interfaces which they had adapted for the magnetopauses of the two planets. It was the first time that this type of kinetic model had been tested on two very different plasma environments.

"We chose that day because we knew that the spacecraft were crossing the planets' magnetopauses at the same time and the conditions were comparable," explained Marius Echim of the Institute for Space Sciences, Romania, and the Belgian Institute for Space Aeronomy in Brussels, who was lead author of the paper.

Although Earth and Venus were not in the same solar wind stream, the particles from the Sun were flowing steadily outward at about 300 km/s. Furthermore, there were no major fluctuations in the magnetic field, ion temperature and density.

"We were able to compare the two magnetopauses, including their thickness, current density and several electrodynamic properties," said Echim.

"Our results suggest that the kinetic structure of the magnetopause at Venus is dominated by ions of solar wind origin, with some contribution from the planetary plasma. The structure of the terrestrial magnetopause is different, with the terrestrial plasma and magnetic field playing the major role in determining its shape and electrodynamic properties.

"The thickness of the magnetopause is also different: roughly 1500 km across for Earth, compared with about 200 km for Venus.

"Our model had never previously been applied to Venus, so we were pleased to see that it predicted the conditions very well. It was also able to provide a much higher time resolution than the plasma instrument on Venus Express, showing in much greater detail how the ions and electrons interact with the magnetopause."

According to Echim, the model also could be applied to other planets, particularly Mars, which has localised pockets of remnant magnetic field, and Saturn, which is being explored by the Cassini orbiter.

"The comparative study of planetary plasma environments contributes to a better understanding of the general principles that govern magnetospheric configuration and dynamics, in particular the role of the solar wind state and of the planetary plasma environment," he said.

Such studies also help to predict the conditions experienced by orbiting spacecraft. The ability to model and predict the location of the planetary magnetopause is important, since major changes in solar wind pressure can cause the magnetic field to balloon in and out. In extreme cases, geostationary satellites may fly outside the protection of the magnetic bubble, putting them under direct assault by solar flares and coronal mass ejections.

Other authors of the paper were: R. Maggiolo and J. De Keyser of the Belgian Institute for Space Aeronomy, Brussels; T. L. Zhang of the Space Research Institute in Graz, Austria; G. Voitcu from the Institute for Space Sciences in Romania; and S. Barabash and R. Lundin of the Swedish Institute for Space Physics in Kiruna.

Reference Publication

Echim, M., et al., Comparative investigation of the terrestrial and Venusian magnetopause: Kinetic modelling and experimental observations by Cluster and Venus Express, Planetary and Space Science, May 2010. DOI: 10.1016/j.pss.2010.04.019

Contacts

Marius Echim

Space physics department

Institut d'Aeronomie Spatiale de Belgique (IASB)

Brussels, Belgium

and Institute for Space Sciences (ISS), Bucharest, Romania

Phone: +32 2 3730418

Email: marius.echim oma.be

Matt Taylor

Cluster Project Scientist

Directorate of Science and Robotic Exploration

ESA, The Netherlands

Phone: +31 71 565 8009

Email: Matthew.Taylor esa.int

Håkan Svedhem

Venus Express Project Scientist

Directorate of Science & Robotic Exploration

ESA, The Netherlands

Phone: +31 71 565 3380

Email: hsvedhem rssd.esa.int