WASHINGTON: NASA’s Parker Solar Probe has flown close enough to the sun to detect the fine structure of the solar wind close to where it is generated at the sun’s surface, revealing details that are lost as the wind exits the corona as a uniform blast of charged particles, according to a new study.
Launched in 2018, the Parker Solar Probe was designed to determine what the turbulent solar wind looks like where it’s generated near the sun’s surface, or photosphere, and how the wind’s charged particles — protons, electrons and heavier ions, primarily helium nuclei — are accelerated to escape the sun’s gravity.
The sun-kissing probe also aimed to resolve two conflicting explanations for the origin of the high-energy particles that comprise the solar wind: magnetic reconnection or acceleration by plasma or Alfven waves.
Understanding how and where the solar wind originates will help predict solar storms that, while producing beautiful auroras on Earth, can also wreak havoc with satellites and the electrical grid.
To do this, the sun-kissing probe had to get closer than 25 to 30 solar radii, that is, closer than about 13 million miles.
In 2021, the Parker probe's instruments recorded magnetic field switchbacks in the Alfven waves that seemed to be associated with the regions where the solar wind is generated.
By the time the probe reached about 12 solar radii from the surface of the sun — 5.2 million miles — the data were clear that the probe was passing through jets of material, rather than mere turbulence.
The researchers traced these jets back to the supergranulation cells in the photosphere, where magnetic fields bunch up and funnel into the sun, which they described as “like seeing jets of water emanating from a showerhead through the blast of water hitting you in the face”.
“The big conclusion is that it’s magnetic reconnection within these funnel structures that’s providing the energy source of the fast solar wind,” Bale said, in a paper to be published in the journal Nature. (IANS)
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