It is thought that this 'wave heating' can raise the temperature of the corona to about 1.5 million kelvin, its temperature in its quiescent phase. The first mechanism is heating from the solar interior carried to the surface by waves in the hot gas. The discovery that nanoflares play an important and perhaps dominant role in coronal heating paves the way to understanding how the sun affects Earth, our place in the universe.The mechanisms that heat the corona are poorly understood, but are thought to be of two kinds. The X-ray and UV also affect the propagation of radio signals and thereby adversely affect communication and navigation systems. Changes in the upper atmosphere can affect the orbits of satellites and space debris by slowing them down, an effect known as 'drag.' It is important to know the changing orbits so that maneuvers can be made to avoid space collisions. X-ray and UV get absorbed by Earth's upper atmosphere, which heats up and expands. Nanoflares are responsible for changes in the X-ray and ultraviolet (UV) radiation that happen as an active region evolves. The observations also confirm 'there is some nanoflare activity everywhere' in the sun's active regions, says Klimchuk. The Hinode observations and the scientists' analysis verify that nanoflares are occurring on the sun and that they explain much and perhaps most coronal heating. 'For the first time, we have detected this 10 million degree plasma, which can only be produced by the impulsive energy bursts of nanoflares.' 'What we see is 1 million degree K plasma that has received its energy from the heat flowing down from the superhot plasma,' says Klimchuk. Thus, a coronal loop is a collection of 5-10 million degree K faint strands and 1 million degree K bright strands. This dense plasma expands up into the strand. Because it is so dense at the base, the temperature only reaches about 1 million degrees K. This heats up the dense plasma at the loop’s base. Heat flows from up in the strand, where it's hot, down to the base of the coronal loop, where it's not as hot. The density remains low, however, so the emission, or brightness, remains faint. Klimchuk surmises that when a nanoflare suddenly releases its energy, the plasma in the low-temperature, low-density strands becomes very hot-around 10 million degrees K-very quickly. 'Then we make predictions about how much emission we should see from plasma of different temperatures.' 'We simulate a burst of heating and see how the corona responds,' says Klimchuk. Klimchuk and colleagues constructed a theoretical model to explain how plasma evolves within these coronal tubes and what causes temperatures to skyrocket. The corona is mostly bright at about 1 million degrees K. Where there's high density, there's a lot of brightness. Where there's low density, there isn't much brightness. The brightness of the observed X-ray and ultraviolet emission is strongly dependent on the density of the coronal plasma. 'Coronal loops are bundles of unresolved strands that are heated by storms of nanoflares.'Ĭoronal heating is a dynamic process. 'These temperatures can only be produced by impulsive energy bursts,' says Klimchuk, who presented the findings on August 6 at the International Astronomical Union General Assembly meeting in Rio de Janeiro, Brazil. The XRT measured plasma at 10 million degrees K, and the EIS measured plasma at 5 million degrees K. Observations from the NASA-funded X-Ray Telescope (XRT) and Extreme-ultraviolet Imaging Spectrometer (EIS) instruments aboard Hinode reveal that ultra-hot plasma is widespread in solar active regions. But no direct evidence of the nanoflares existed until now. Newer models based on nanoflares can explain the observed density. However, observations showed that coronal loops have much higher density than the steady heating model predicts. The steady heating model indicates that a coronal loop of a given length and temperature should have a specific density. Scientists previously thought steady heating explained the corona's million degree temperatures. Coronal loops are the fundamental building blocks of the thin, translucent gas known as the sun's corona. 'They occur within tiny strands that are bundled together to form a magnetic tube called a coronal loop,' says Klimchuk. Nanoflares are small, sudden bursts of heat and energy. New observations made with instruments aboard Japan's Hinode satellite reveal the culprit to be nanoflares. The mystery of why temperatures in the solar corona, the sun's outer atmosphere, soar to several million degrees Kelvin (K) -much hotter than temperatures nearer the sun's surface-has puzzled scientists for decades.

Gas of sun corona