"It is all the more astonishing that temperatures of several million degrees suddenly prevail again in the overlying Sun's corona," says Dr. At its surface, it emits its light at a comparatively moderate 6000 degrees Celsius. In an experiment using the molten alkali metal rubidium and pulsed high magnetic fields, a team from the Helmholtz-Zentrum Dresden-Rossendorf (HZDR), a German national lab, has developed a laboratory model and for the first time experimentally confirmed the theoretically predicted behavior of these plasma waves – so-called Alfvén waves – as the researchers report in the journal Physical Review Letters (DOI: 10.1103/PhysRevLett.127.275001).Īt 15 million degrees Celsius, the center of our Sun is unimaginably hot. A "hot" trail to explain this effect leads to a region of the solar atmosphere just below the corona, where sound waves and certain plasma waves travel at the same speed. Why the Sun's corona reaches temperatures of several million degrees Celsius is one of the great mysteries of solar physics. view moreĬredit: Courtesy of NASA/SDO and the AIA, EVE, and HMI science teams. Immediately after the eruption, cascades of magnetic loops form over the eruption area as the magnetic fields attempt to reorganize. The researchers found that the energy fluxes of their mechanisms match those required by all studies to maintain the temperature of the plasma in the solar atmosphere, namely 4,500 W/m 2 in the chromosphere and 300 W/m 2 in the corona.ġ The magnetic field lines are structured like roots and branches.Ģ Plasma, often called the fourth state of matter, here represents an electrically conducting fluid.ģ Spicule: a thin jet of matter that emerges from the chromosphere and enters the corona.Image: A plasma ejection during a solar flare. All these phenomena, which have been ascertained individually but not explained, make up various energy channels produced by the boiling plasma, rather than the single source hitherto postulated. Thin plasma jets near the tree trunks are also produced and are associated with recently discovered spicules. The scientists' calculations also show that as the ejected matter falls back towards the surface it forms tornadoes, which have actually been observed. These waves then transport energy to the upper corona, which is heated by their progressive dissipation. This eruptive process generates 'magnetic' waves along the tree trunks, rather like sound traveling along a plucked string. They also discovered that larger but less numerous eruptive events take place in the neighborhood of the mesospots, although these are not able to heat the upper corona on a larger scale. The researchers' calculations show that, in the chromosphere, heating of the atmosphere results from multiple micro-eruptions in the mangrove roots that carry intense electric current, in pace with the 'bubbles' from the boiling plasma. The scientists also discovered that a structure resembling a mangrove forest appears around the solar mesospots: tangled 'chromospheric roots' dive into the spaces between the granules, surrounding 'magnetic tree trunks' that rise up towards the corona and are associated with the larger-scale magnetic field. As the field emerges from the surface, it takes on a salt-and-pepper appearance, forming concentrations dubbed 'mesospots' that are larger, fewer in number and more persistent, all of which is consistent with observations. This boiling plasma soup generates a dynamo process that amplifies and maintains the magnetic field. The researchers observed that the thin layer under the Sun's surface actually behaves rather like a shallow pan containing boiling plasma, heated from below and forming 'bubbles' associated with granules. Using powerful numerical models run on computers at the Centre de Physique Théorique (CNRS/École Polytechnique) and GENCI at IDRIS-CNRS, the team performed a simulation for several hours, based on a model made up of several layers, one inside the Sun and the others in its atmosphere. The researchers concentrated on the small-scale magnetic field, which, except for the sunspots, has a 'salt-and-pepper' appearance. So what source of energy can heat the atmosphere and maintain it at such high temperatures? For around a century, this question puzzled astrophysicists, all the more so as it relates to the origin of the solar wind that affects Earth.Īlthough there was little doubt that part of the energy from the Sun's interior reached its outer layers, the exact mechanism remained a mystery. Instead, it rises to about 10,000☌ in the chromosphere, and exceeds a million degrees Celsius in the corona. Logically, it should therefore continue to decline in the atmosphere. The Sun's temperature, which reaches around 15 million degrees Celsius in its core, steadily decreases with distance from the core, falling to 6000☌ at its 'surface'.
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