Kiwi physicists help solve the Sun's “solar wind” secret

Publicly released:
New Zealand; International
'This conceptual image shows Parker Solar Probe about to enter the solar corona. Credit NASAJohns Hopkins APLBen Smith.jpg'
'This conceptual image shows Parker Solar Probe about to enter the solar corona. Credit NASAJohns Hopkins APLBen Smith.jpg'

Strangely, the Sun heats up the farther you move away from its surface - skyrocketing from 6,000 to a million degrees Celsius just a few hundred kilometres out. It's something so hot it generates a “solar wind” that whips out into space and can even reach us Earthlings. An international team, led by NZ scientists, has made a breakthrough in learning how magnetic fields play a part in heating up this wind using six-dimensional supercomputer simulations. They suggest the effect of a “helicity barrier” links two theories that were previously seen as incompatible: one based on heating caused by turbulence, and another based on heating caused by a type of magnetic wave.

Media release

From: University of Otago

Scientists solve solar secret

The further we move away from a heat source, the cooler the air gets. Bizarrely, the same can’t be said for the Sun, but University of Otago scientists may have just explained a key part of why.

Study lead Dr Jonathan Squire, of the Department of Physics, says the surface of the Sun starts at 6000 degC, but over a short distance of only a few hundred kilometres, it suddenly heats up to more than a million degrees, becoming its atmosphere, or corona.

“This is so hot that the gas escapes the Sun’s gravity as ‘solar wind’, and flies into space, smashing into Earth and other planets.

“We know from measurements and theory that the sudden temperature jump is related to magnetic fields which thread out of the Sun’s surface. But, exactly how these work to heat the gas is not well understood – this is known as the Coronal Heating Problem.

“Astrophysicists have several different ideas about how the magnetic-field energy could be converted into heat to explain the heating, but most have difficulty explaining some aspect of observations,” he says.

Dr Squire and co-author Dr Romain Meyrand have been working with scientists at Princeton University and the University of Oxford and found two previous theories can be merged into one to solve a key piece of the ‘problem’. The group’s findings have been published today in Nature Astronomy.

The popular theories are based on heating caused by turbulence, and heating caused by a type of magnetic wave called ion cyclotron waves.

“Both, however, have some problem – turbulence struggles to explain why hydrogen, helium and oxygen in the gas become as hot as they do, while electrons remain surprisingly cold; while the magnetic waves theory could explain this feature, there doesn’t seem to be enough of the waves coming off the Sun’s surface to heat up the gas,” Dr Meyrand says.

The group used six-dimensional supercomputer simulations of the coronal gas to show how these two theories are actually part of the same process, linked together by an intriguing effect called the ‘helicity barrier’.

This interesting occurrence was discovered in an earlier Otago study, led by Dr Meyrand.

“If we imagine plasma heating as occurring a bit like water flowing down a hill, with electrons heated right at the bottom, then the helicity barrier acts like a dam, stopping the flow and diverting its energy into ion cyclotron waves. In this way, the helicity barrier links the two theories and resolves each of their individual problems,” he explains.

For this latest study, the group stirred the magnetic field lines in simulations and found the turbulence created the waves, which then caused the heating.

“As this happens, the structures and eddies that form end up looking extremely similar to cutting-edge measurements from NASA’s Parker Solar Probe spacecraft, which has recently become the first man-made object to actually fly into the corona.

“This gives us confidence that we are accurately capturing key physics in the corona, which – coupled with the theoretical findings about the heating mechanisms – is a promising path to understanding the coronal heating problem,” Dr Meyrand says.

Understanding more about the Sun’s atmosphere and the subsequent solar wind is important because of the profound impacts they have on Earth, Dr Squire explains.

Effects which result from solar wind’s interaction with the Earth’s magnetic field is called ‘space weather’, which causes everything from Aurora to satellite-destroying radiation and geomagnetic currents which damage the power grid.

“All of this is sourced, fundamentally, by the corona and its heating by magnetic fields, so as well as being interesting for our general understanding of the solar system, the solar-corona’s dynamics can have profound impacts on Earth.

“Perhaps, with a better understanding of its basic physics, we will be able to build better models to predict space weather in the future, thus allowing the implementation of protection strategies that could head off – literally – billions of dollars of damage.”

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conference:
Nature Astronomy
Research:Paper
Organisation/s: University of Otago, Princeton University, US and Oxford University, UK
Funder: We thank B. Dorland, B. Chandran and A. Mallet for illuminating discussions. J.S. and R.M acknowledge support from the Royal Society Te Apārangi, New Zealand, through Marsden Fund grant number UOO1727 and Rutherford Discovery Fellowship RDF-U001804. M.W.K. and E.Q. were supported by the Department of Energy through the NSF/DOE Partnership in Basic Plasma Science and Engineering, award numbers DE-SC0019046 and DE-SC0019047, with additional support for E.Q. from a Simons Investigator Award from the Simons Foundation. L.A. acknowledges the support of the Institute for Advanced Study, and the work of A.A.S. was supported in part by UK EPSRC grant number EP/R034737/1. This research was part of the Frontera computing project at the Texas Advanced Computing Center, which is made possible by National Science Foundation award number OAC-1818253. Further computational support was provided by the New Zealand eScience Infrastructure (NeSI) high-performance computing facilities, funded jointly by NeSI’s collaborator institutions and the NZ MBIE, and through the PICSciE-OIT TIGRESS High Performance Computing Center and Visualization Laboratory at Princeton University. The funders had no role in study design, data collection and analysis, decision to publish or preparation of the manuscript.
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