Scientists at Northumbria University have begun to unlock the mystery of why the outer edge of the Sun is much hotter than its surface for the first time. A team led by Northumbria's Dr Richard Morton, and including researchers from the University of Sheffield and Queen's University Belfast, have used cutting-edge solar-imaging technology to observe the Sun's chromosphere – a region of the Sun's atmosphere sandwiched between its surface (photosphere) and outer layer (corona) – to an unprecedented level of detail.
Now, for the first time, the team has examined the MHD waves using a UK-designed dedicated solar-imaging telescope known as Rapid Oscillations in the Solar Atmosphere, or ROSA, to observe the chromosphere with a high degree of clarity. The powerful tool enabled some of the highest resolution images of the chromosphere to be obtained, allowing the scientists to study the speed and power of the waves and then estimate the amount of energy that they transport.
Their calculations confirm that the MHD waves could be responsible for transporting energy from below the solar surface, out through the chromosphere, into the corona and leading to heating of the outer layers in excess of a million degrees.
"The Sun is our closest star and provides a unique opportunity to study the properties of stars in detail," said Morton. "ars generate heat through thermonuclear reactions in their core and the temperature decreases towards the star's surface. However, a significant number of stars have higher temperatures at the outer edges of their atmospheres than they do on their surface.
"Our observations have permitted us to estimate the amount of energy transported by the magnetic waves, and these estimates reveal that the waves' energy meets the energy requirement for the unexplained temperature increase in the corona."
The team's findings have been published in Nature Communications, an online journal. Journal reference: Nature Communications Provided by Northumbria University.
Image at the top of the page shows magnetic loop structures in the corona of the Sun. The loops highlight the Sun’s magnetic field and are visible because they support the dense, million degree gas typical of the corona. The image is courtesy of the Science Team for NASA’s Solar Dynamic Observatory.
The Daily Galaxy via Northumbia University