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One free scan finds every outdated or missing driver and matches the right update for your exact hardware.Free scan · exact hardware matchNASA calls the strange reversal a magnetic switchback: a temporary kink in the solar-wind magnetic field that can turn the field almost completely backward, toward the Sun. Parker Solar Probe found these events repeatedly close to the Sun, where the wind is still being formed and energized.
The discovery matters because switchbacks may carry enough Alfvén-wave energy to help explain how the solar wind is heated and accelerated before it fills the heliosphere.
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What Parker Solar Probe detected
Parker’s FIELDS instrument measured rapid reversals in the magnetic field carried by the solar wind. NASA’s Dec. 4, 2019 results release said the events were common inside Mercury’s orbit and lasted from a few seconds to several minutes. During an event, the field can whip around until its direction points almost directly back at the Sun instead of outward.
These are not permanent changes to the Sun’s global magnetic field. They are short-lived structures embedded in the outward-flowing plasma. Parker encountered them at roughly 15 million miles from the Sun during its early passes, sampling a highly organized and variable flow rather than the relatively smooth stream usually measured near Earth.
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Why measuring them near the Sun changes the picture
By the time solar wind reaches Earth, interactions and expansion can blur the details of its origin. Parker travels inside Mercury’s orbit and measures the field and particles much closer to the corona, where the structures are created or first amplified.
That location lets scientists ask whether a reversal begins in the solar atmosphere, develops as the wind expands, or results from both processes. It also provides a direct test of how magnetic fluctuations transfer energy into the fast and slow solar-wind streams.
What could create a switchback?
NASA has not adopted one settled explanation. Its 2021 overview lists several active possibilities, and an April 2020 analysis examined interchange reconnection in detail.
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Interchange reconnection
In this model, an open magnetic field line extending into space meets a closed loop anchored at both ends on the Sun. Magnetic reconnection exchanges their connections and launches an outward-moving, S-shaped kink in the field. The idea was first proposed in 1996 using results from the Ulysses mission, but NASA presents it as a possible mechanism rather than a final answer.
Turbulent growth in the expanding wind
Small magnetic and velocity fluctuations can grow and steepen as the solar wind expands away from the Sun. In this view, at least some switchbacks are produced within the outflow rather than being created directly at the coronal surface.
Shear between fast and slow streams
Adjacent streams moving at different speeds can generate strong shear. NASA lists this interaction as another route to the bends and reversals Parker observes.
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A hybrid process
Reconnection may create the initial structure, after which turbulence in the expanding wind enlarges or sustains it. This combined picture could explain why a feature born near the Sun remains detectable farther out.
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| Explanation | Where the structure starts | Required process | What scientists would test | Status |
|---|---|---|---|---|
| Interchange reconnection | Solar atmosphere, where open and closed field lines meet | Magnetic reconnection creates an S-shaped outward kink | Whether reconnection signatures and the predicted field geometry match Parker measurements at different distances | Proposed mechanism, not a confirmed verdict |
| Turbulent amplification | Expanding solar wind | Fluctuations grow and steepen as the wind travels outward | How switchback frequency, size and shape change with distance | Active NASA hypothesis |
| Fast–slow stream shear | Interfaces between streams moving at different speeds | Velocity and magnetic shear distort the field | Whether events correlate with stream boundaries and particular wind speeds | Active NASA hypothesis |
| Hybrid reconnection plus turbulence | Begins near the Sun and evolves in the wind | Reconnection seeds the structure; expansion and turbulence amplify it | Whether a two-stage model explains both the initial geometry and later persistence | Active NASA hypothesis |
The key unresolved test is not simply which mechanism can bend a field line. It is which process reproduces the observed distance dependence, association with different wind streams and energy budget at the same time.
Do switchbacks heat and accelerate the solar wind?
Evidence increasingly points to an important energy role. Switchbacks are associated with Alfvén-wave fluctuations—coupled motions of magnetic field and plasma that can transport energy outward. Coordinated Parker Solar Probe and Solar Orbiter measurements summarized by NASA on Aug. 30, 2024 found enough energy in these fluctuations to account for heating and acceleration in faster solar-wind streams.
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NASA’s 2021 comparison gives the scale of the flows: fast solar wind travels about 430 miles per second, while slow solar wind travels about 220 miles per second. The measurements do not mean every switchback supplies all of a stream’s energy. They show that the population of fluctuations has an energy budget large enough to make a substantial contribution to the heating and acceleration problem.
That problem has persisted for decades. The corona is much hotter than the Sun’s visible surface, yet the solar wind continues to gain speed as it moves outward. Identifying where magnetic energy is stored, redirected and dissipated is central to explaining that behavior.
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The solar wind fills the heliosphere and interacts with planetary magnetic fields. Changes in its speed, density and magnetic orientation can drive disturbances in Earth’s magnetosphere. Better knowledge of how magnetic structure and energy move outward should improve physical models of the solar wind and the space-weather conditions it can produce.
Parker’s measurements are especially valuable because they connect remote observations of the corona with direct measurements of the plasma that later reaches the planets. That connection helps scientists determine which features survive the journey and which are transformed along the way.
Do not confuse switchbacks with Parker’s later “U-turn” observation
NASA’s Dec. 11, 2025 article described a related but different event. During Parker’s Dec. 24, 2024 pass, at only 3.8 million miles from the solar surface, the spacecraft’s WISPR camera imaged a coronal mass ejection and elongated inflows—blobs of solar material pulled back toward the Sun after magnetic field lines tore and re-formed.
That observation shows material falling sunward during coronal-mass-ejection reconfiguration. A switchback is an in-situ reversal in the magnetic field carried by the solar wind. Both involve changing magnetic geometry, but the 2025 inflow is not evidence that switchbacks themselves are blobs returning to the Sun.
What remains unknown
- Whether most switchbacks are born by interchange reconnection, turbulence, stream shear or a combination.
- How their size, frequency and orientation evolve as the solar wind travels away from the Sun.
- How much of the energy in Alfvénic fluctuations is converted into heat versus bulk flow speed.
- Why some solar-wind streams preserve strong switchback signatures while others appear smoother.
NASA associate administrator for science Thomas Zurbuchen said the first Parker data revealed the Sun “in new and surprising ways.” The continuing measurements are designed to turn that surprise into a physical account of how the heliosphere is powered.
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