When the Earth’s magnetic field and the interplanetary magnetic field are aligned, for example in a northward orientation as indicated by the white arrow in this figure, Kelvin–Helmholtz waves are generated at low (equatorial) latitudes. (Courtesy: ESA/AOES Medialab)

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Earth’s magnetic shield behaves like a sieve

The Earth’s magnetic field is more permeable than previously thought, according to researchers analysing data from the European Space Agency’s Cluster mission. The findings have implications for modelling the dangers posed by space weather and could also help us better understand the magnetic environments around Jupiter and Saturn.

The Cluster mission, launched in 2000, comprises four identical satellites flying in a tetrahedral formation in close proximity to Earth. With highly elliptical orbits, the satellites are able to sweep in and out of the Earth’s magnetic environment, building up a 3D picture of interactions between the solar wind and our planet. The solar wind is a stream of charged particles from the outer layers of the Sun blowing into the solar system. The Earth’s magnetic field is thought to form a protective barrier against it.

It is well known, however, that if the magnetic field of the incoming solar wind has the opposite orientation to the Earth’s magnetic field, then the field lines can break and join up again in a process known as “magnetic reconnection”. This process allows the plasma from the solar wind to breach the boundary of the Earth’s magnetic field – the magnetopause – where it can then potentially reach our planet.

Swirling vortices

In 2004 data from Cluster revealed that this mismatch in magnetic orientation was not a hard and fast rule – 40,000 km-long swirls of plasma were spotted along the magnetopause, creating gateways into the magnetosphere even when the two magnetic fields were aligned. By 2006, researchers had concluded that these vortices were likely caused by Kelvin–Helmholtz waves (KHWs), occurring when two mediums are flowing on either side of a boundary at different velocities. An earthly example is wind blowing over the boundary between the air and the ocean. In space, the boundary is the magnetopause, with the decelerated plasma on the Earth-side travelling slower than the solar-wind plasma beyond.

Once created, the amplitude of these instabilities can build up, tangling the magnetic field lines and triggering magnetic reconnection despite the field lines being aligned. This phenomenon was only thought to happen under special conditions, however. “We thought [it] was restricted to areas around the Earth’s equator,” Arnaud Masson, one of the scientists working on the Cluster mission, toldphysicsworld.com. Now, new analysis of Cluster data, initially obtained in 2003, shows the same thing happening at much higher latitudes, and at a wider range of magnetic-field alignments. “It seems that no matter what the orientation of magnetic fields, the same effect can occur,” explains Masson. “It appears that it happens all the time, rather than just in special circumstances.”

Modelling space weather

Knowing the range of conditions under which the solar wind can penetrate the Earth’s magnetic defences plays an important role in modelling space weather – a catalogue of effects including disruption to GPS navigation caused by interaction with the solar wind. “You have to know where the doors are open in our protective shield,” explains Masson. Chris Arridge, of University College London, agrees. “It seems there are a lot more holes in the Earth’s magnetic sieve than we thought,” he says. “If we want to develop the ability to predict space-weather effects, then it is important to know the full range of ways that energy, mass and momentum can get into the system.”

Arridge, a researcher on the interaction between the solar wind and the outer planets of the solar system, believes this line of research could also help us understand Jupiter and Saturn. “The exact role of KHWs in the magnetospheres of the giant planets is a hot topic,” he reveals. Understanding the Earth’s KHW mechanisms will help us understand Jupiter and Saturn’s magnetic environments and vice versa.”

The research is published in Journal of Geophysical Research.

About the author

Colin Stuart  is a science writer and astronomer based in London

  • Read directly via the source

Journal of Geophysical Research
Space Physics


The first in situ observation of Kelvin-Helmholtz waves at high-latitude magnetopause during strongly dawnward interplanetary magnetic field conditions

We report the first in situ observation of high-latitude magnetopause (near the northern duskward cusp) Kelvin-Helmholtz waves (KHW) by Cluster on January 12, 2003, under strongly dawnward interplanetary magnetic field (IMF) conditions. The fluctuations unstable to Kelvin-Helmholtz instability (KHI) are found to propagate mostly tailward, i.e., along the direction almost 90° to both the magnetosheath and geomagnetic fields, which lowers the threshold of the KHI. The magnetic configuration across the boundary layer near the northern duskward cusp region during dawnward IMF is similar to that in the low-latitude boundary layer under northward IMF, in that (1) both magnetosheath and magnetospheric fields across the local boundary layer constitute the lowest magnetic shear and (2) the tailward propagation of the KHW is perpendicular to both fields. Approximately 3-hour-long periods of the KHW during dawnward IMF are followed by the rapid expansion of the dayside magnetosphere associated with the passage of an IMF discontinuity that characterizes an abrupt change in IMF cone angle, ϕ = acos B x B , from ∼90° to ∼10°. Cluster, which was on its outbound trajectory, continued observing the boundary waves at the northern evening-side magnetopause during sunward IMF conditions following the passage of the IMF discontinuity. By comparing the signatures of boundary fluctuations before and after the IMF discontinuity, we report that the frequencies of the most unstable KH modes increased after the discontinuity passed. This result demonstrates that differences in IMF orientations (especially in ϕ) are associated with the properties of KHW at the high-latitude magnetopause due to variations in thickness of the boundary layer, and/or width of the KH-unstable band on the surface of the dayside magnetopause.

Colin Stuart (2012).
Earth’s magnetic shield behaves like a sieve




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