Ultrafast substorm aurorae result from magnetic reconnection events, which occur far out in the magnetotail.
Photo by ESA/AOES Medialab
From time to time, sudden releases of energy in Earth’s magnetosphere lead to major disturbances that result in bright auroral displays over the planet’s polar regions. These aurorae are caused by a phenomenon known as a geomagnetic substorm. The precise cause of these substorms has been debated for decades, but new computer simulations, allied to analysis of data from the European Space Agency’s (ESA) Cluster spacecraft, are now filling in many of the missing pieces in the puzzle.
Earth’s magnetic field is continuously buffeted by clouds of energetic, electrically charged particles — mainly electrons and protons — that are carried in the solar wind or released during huge explosions on the Sun, known as coronal mass ejections. The magnetic bubble that surrounds Earth — the magnetosphere — generally protects the planet from these particles, but the shield is sometimes breached, enabling particles and energy to accumulate in the magnetotail. This stored energy is subsequently released as the result of a sudden rearrangement of the magnetic-field lines. Electrified particles then race along the field lines and enter the atmosphere above the magnetic poles, creating bright rings of light in the form of colorful aurorae.
Although this basic process has been recognized for many years, there has been no scientific consensus about where the geomagnetic substorms are initiated. One question concerned whether they are caused by a sudden disruption of electric current about 40,000 miles (64,000 kilometers) from the planet, or by a process called magnetic reconnection that occurs much farther down the magnetotail, at a distance of around 78,000 to 124,000 miles (125,000 to 200,000 km).
Although recent research appears to favor the magnetic reconnection mechanism, a major problem with this theory involves the rapid onset of aurorae after the sudden realignment of the magnetic-field lines.
According to established theory, the energy from the reconnection event is carried by Alfvén waves — a type of magnetic wave that propels the charged particles in the plasma toward and away from Earth. However, these Alfvén waves travel quite slowly, reaching Earth after a travel time of about 250 seconds. They cannot account for some observations of substorm events, which indicate that aurorae intensify less than 1 minute after the onset of reconnection — much earlier than expected. This discrepancy led to the suggestion that another, faster, type of wave — known as a kinetic Alfvén wave (KAW) — might also be generated during a substorm.
Unlike ordinary Alfvén waves, which move both ions and electrons toward Earth at 300 to 600 miles per second (500 to 1,000 km/s), kinetic Alfvén waves influence only electrons. This enables them to travel much faster through the plasma, at speeds of several thousand kilometers per second.
In an effort to investigate these questions, Michael Shay, a professor at the Bartol Research Institute in the Department of Physics and Astronomy at the University of Delaware, began a series of simulations on a Cray XE6, one of the most powerful computers in the world. Located at the National Energy Research Scientific Computing Center, the HOPPER supercomputer crunched away at solving fluid equations that simulated the behavior of individual particles energized by reconnection.
“We ran a very simple system and simulated how the reconnection event released energy in the plasma sheet of charged particles,” said Shay. “We were looking for a faster mechanism for propagating the signal from the explosion than the Alfvén waves that were already widely recognized.”
The simulations confirmed that KAWs could be generated by reconnection and then propagate rapidly away from the site of the explosion, reaching Earth in less than 1 minute. They also confirmed that KAWs carry enough energy to intensify aurorae.
Further verification of this result came from Jonathan Eastwood, a research fellow at the Blackett Laboratory, Imperial College London, United Kingdom, who began to trawl through data sent back by the four Cluster spacecraft during their decade-long exploration of near-Earth space. Eastwood was sifting through the data returned by the Fluxgate Magnetometer (FGM) and the Electric Fields and Waves (EFW) instrument on each spacecraft in a search for measurements that coincided with magnetic reconnection events in the magnetotail.
“I found 18 events which occurred at the time the four spacecraft were flying through the tail region,” said Eastwood. “The fast signal predicted by Michael Shay showed up in the Cluster data, supporting the theory that kinetic Alfvén waves generated by reconnection were rapidly energizing the auroras.”
“It’s rather like what happens in a thunderstorm,” he added. “The fast-moving lightning flash arrives first, followed some time later by the slower sound waves of the thunderclap. The Cluster data also supported the theory that reconnection occurs far from Earth, some 125,000 to 200,000 kilometers [78,000 to 124,000 miles] down the tail.”
“We have shown that kinetic Alfvén waves are no longer simply a theoretical conjecture, but an entirely plausible source for generating auroras,” said Shay.
“This research is a striking example of how Cluster data are now being used by theoreticians around the world to back up their simulations and transform scientists’ understanding of the complex processes that take place in near-Earth space,” said Arnaud Masson, ESA deputy project scientist for the Cluster mission.