The movement of this plasma in the convection zone – the upper part of the solar interior – produces huge electrical currents and strong magnetic fields. The Sun is composed almost entirely of plasma, which is highly ionised gas that carries an electrical charge. Scientists looked to the Sun’s properties to explain this disparity. The extreme heat of the Sun’s corona is one of the most vexing problems in astrophysics. Edlén and Grotrian’s finding that the Sun’s corona is so much hotter than the photosphere – despite being further from the Sun’s core, its ultimate source of energy – has led to much head-scratching in the scientific community. Over many decades of study, the photosphere’s temperature has been consistently estimated at around 6,000☌. Estimating the photosphere’s heat has always been relatively straightforward: we just need to measure the light that reaches us from the Sun, and compare it to spectrum models that predict the temperature of the light’s source. This represents temperatures up to 1,000 times hotter than the photosphere beneath it, which is the surface of the Sun that we can see from Earth. The coronal heating problem has been established since the late 1930s, when the Swedish spectroscopist Bengt Edlén and the German astrophysicist Walter Grotrian first observed phenomena in the Sun’s corona that could only be present if its temperature was a few million degrees celsius. Our recent study has finally achieved this, validating Alfvén’s 80 year-old theory and taking us a step closer to harnessing this high-energy phenomenon here on Earth. The theory had been tentatively accepted – but we still needed proof, in the form of empirical observation, that these waves existed. He theorized that magnetized waves of plasma could carry huge amounts of energy along the Sun’s magnetic field from its interior to the corona, bypassing the photosphere before exploding with heat in the Sun’s upper atmosphere. Seeking to unify the corona and heliosphere.In 1942, the Swedish scientist Hannes Alfvén proposed an explanation. Observations of the middle corona provide strong new constraints on models These new data uniquely demonstrate how EUV Reveals the full kinematic profile of the initiation of several coronal massĮjections, filling a crucial observational gap that has hindered understanding Strongly influenced by inflows from above, not only by photospheric motion, aįactor largely overlooked in current models of coronal evolution. These data emphasize that low-coronal phenomena can be Originate from complex dynamics manifesting in the middle corona that do not Our observations highlight that solar wind structures in the heliosphere Rather than collisional excitation, consistent with recent model predictions. OurĪnalysis shows that the dominant emission mechanism here is resonant scattering New observations from the GOES Solar Ultraviolet Imager in AugustĪnd September 2018 provide the first comprehensive look at this region'sĬharacteristics and long-term evolution in extreme ultraviolet (EUV). Poorly understood due to the difficulty of observing this faint region (1.5-3 Physical regimes of the lower and outer solar corona. Seaton and 8 other authors Download PDF Abstract: The "middle corona" is a critical transition between the highly disparate Download a PDF of the paper titled The Sun's Dynamic Extended Corona Observed in Extreme Ultraviolet, by Daniel B.
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