Scientists can predict when and where there will be aurora, but with less confidence than they can predict the regular weather. Some increased activity in the solar wind happens during every equinox. These regular fluctuations are known as magnetic storms. Magnetic storms can lead to auroras being seen in the midlatitudes during the time around the spring and autumnal equinoxes. Auroras have been visible as far south as the Yucatan Peninsula in Mexico.

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Remote sensing spacecraft also monitor the sun for indications of impulsive eruptions that eject material toward Earth, or regions where continuous high-speed streams of material are escaping and heading Earthward. In either case, the travel time to Earth for such material leaving the sun is 1 to 3 days. This allows good forecasts to be made on these look-ahead time scales, based on events and conditions observed on the sun. The Base– The solid, no-gap base is given a 3mm layer of foam insulation, with reflective aluminum foil on each side. Again helping it to add some additional insulation. MusicianAurora Aksnes is known mononymously as Aurora. She is a Norwegian musician,-songwriter, and producer. The accompanying pictures are by members of the Royal Photographic Society (RPS), Grahame Soden ARPS and Richard Ellis ARPS.

This level of auroral activity, index Kp=2, will occur often enough that you will probably see the aurora if you travel to these regions when the nights are dark and stay for three days to a week, assuming that the skies are clear. If the auroral activity level is higher than 2, you will still observe the stronger motions and color changes, etc., that are seen farther equatorward. Customers migrating to Aurora see lower latency and practical elimination of replica lag (e.g, from 12 minutes to 20ms). In the ionosphere, the ions of the solar wind collide with atoms of oxygen and nitrogen from Earth’s atmosphere. The energy released during these collisions causes a colorful glowing halo around the poles—an aurora. Most auroras happen about 97-1,000 kilometers (60-620 miles) above Earth’s surface. The Royal Photographic Society are experts in photography and have brought together the best advice on photography for the auroras below.

Streams of charged particles that produce the aurora come from the corona, the outermost layer of the sun's atmosphere. The corona is exceedingly hot, measuring more than one million degrees. The high temperature causes hydrogen atoms to split into protons and electrons. The resulting gas of charged particles is called plasma, which is electrically conductive. The solar plasma is so hot that it breaks free of the sun's gravitational force and blows away from the surface in all directions. The movement of this plasma is called solar wind. The intensity of the solar wind and the magnetic field carried by it change constantly. When the solar wind blows stronger, we see more active and brighter aurora on Earth. Cameras have different sensitivities to colors than the human eye, therefore there is often more red aurora in photos than you can see with the unaided eye. Just like sunlight, which appears to be white, is a blend of the colors of the rainbow, the aurora is also a mixture of colors. The overall impression is a greenish-whitish glow. Since there is more oxygen at high altitudes, the red aurora tends to be on top of the regular green aurora. Very intense aurora often has a purple rim at the bottom. The purple results from a mixture of blue and red emissions from nitrogen molecules. With regular MySQL, there are lots of writes going on as shown in the figure below (see §3.1 in the paper for a description of all the individual parts).