Aurora effect is known as the aurora borealis or the northern lights. The former term was coined by Galileo in 1619, from the Roman goddess of the dawn and the Greek name for the north wind. The southern counterpart, the aurora australis or the southern lights, has features almost identical to the aurora borealis and changes simultaneously with changes in the northern auroral zone. The Aurora Australis is visible from high southern latitudes in Antarctica, Chile, Argentina, New Zealand, and Australia. A geomagnetic storm causes the auroral ovals (north and south) to expand, and bring the aurora to lower latitudes. The
Aurora the same as that employed in plasma fusion laboratories throughout the world, and appears well able to account in principle for most – if not all – detailed properties of the electrons responsible for the brightest forms of auroras, above, below and within the acceleration region. [[Image:Aurora Borealis.jpg|thumb|left|The aurora borealis as viewed from the International Space Station|ISS [[Expedition 6]] team, [[Lake Manicouagan]] is visible to the bottom left]] Other mechanisms have also been proposed, in particular, [[Alfvén waves]], wave modes involving the magnetic field first noted by [[Hannes Alfvén]] (1942), which have been observed in the laboratory and in space.