NASA Missions Make Unprecedented Map of Sun’s Magnetic Field

The chromosphere remains the most mysterious of the Sun’s atmospheric layers. Sandwiched between the bright surface and the ethereal solar corona, the Sun’s outer atmosphere, the chromosphere is a place of rapid change, where temperature rises and magnetic fields begin to dominate the Sun’s behavior.

The chromosphere lies between the photosphere, or bright surface of the Sun that emits visible light, and the super-heated corona, or outer atmosphere of the Sun at the source of solar eruptions. The chromosphere is a key link between these two regions and a missing variable determining the Sun’s magnetic structure. Photo: NASA’s Goddard Space Flight Center

Now, for the first time, a triad of NASA missions have peered into the chromosphere to return multi-height measurements of its magnetic field.

The observations – captured by two satellites and the Chromospheric Layer Spectropolarimeter 2, or CLASP2 mission, aboard a small suborbital rocket – help reveal how magnetic fields on the Sun’s surface give rise to the brilliant eruptions in its outer atmosphere.

A major goal of heliophysics – the science of the Sun’s influence on space, including planetary atmospheres – is to predict space weather, which often begins on the Sun but can rapidly spread through space to cause disruptions near Earth.

Driving these solar eruptions is the Sun’s magnetic field, the invisible lines of force stretching from the solar surface to space well past Earth.

This magnetic field is difficult to see – it can only be observed indirectly, by light from the plasma, or super-heated gas, that traces out its lines like car headlights traveling a distant highway. Yet how those magnetic lines arrange themselves – whether slack and straight or tight and tangled – makes all the difference between a quiet Sun and a solar eruption.

Ideally, researchers could read out the magnetic field lines in the corona, where solar eruptions take place, but the plasma is way too sparse for accurate readings. (The corona is far less than a billionth as dense as air at sea level.)

Instead, scientists measure the more densely packed photosphere – the Sun’s visible surface – two layers below. They then use mathematical models to propagate that field upwards into the corona. This approach skips measuring the chromosphere, which lies between the two, instead, hoping to simulate its behavior.

Unfortunately the chromosphere has turned out to be a wildcard, where magnetic field lines rearrange in ways that are hard to anticipate. The models struggle to capture this complexity.

“The chromosphere is a hot, hot mess,” said Laurel Rachmeler, former NASA project scientist for CLASP2. “We make simplifying assumptions of the physics in the photosphere, and separate assumptions in the corona. But in the chromosphere, most of those assumptions break down.”

Institutions in the U.S., Japan, Spain and France worked together to develop a novel approach to measure the chromosphere’s magnetic field despite its messiness.

Modifying an instrument that flew in 2015, they mounted their solar observatory on a sounding rocket, so named for the nautical term “to sound” meaning to measure.

Sounding rockets launch into space for brief, few-minute observations before falling back to Earth. More affordable and quicker to build and fly than larger satellite missions, they’re also an ideal stage to test out new ideas and innovative techniques.

Launching from the White Sands Missile Range in New Mexico, the rocket shot to an altitude of 170 miles (274 kilometers) for a view of the Sun from above Earth’s atmosphere, which otherwise blocks certain wavelengths of light. They set their sights on a plage, the edge of an “active region” on the Sun where the magnetic field strength was strong, ideal for their sensors.

As CLASP2 peered at the Sun, NASA’s Interface Region Imaging Spectrograph or IRIS and the JAXA/NASA Hinode satellite, both watching the Sun from Earth orbit, adjusted their telescopes to look at the same location. In coordination, the three missions focused on the same part of the Sun, but peered to different depths.

Hinode focused on the photosphere, looking for spectral lines from neutral iron formed there. CLASP2 targeted three different heights within the chromosphere, locking onto spectral lines from ionized magnesium and manganese.

Meanwhile, IRIS measured the magnesium lines in higher resolution, to calibrate the CLASP2 data. Together, the missions monitored four different layers within and surrounding the chromosphere.

Eventually the results were in: The first multi-height map of the chromosphere’s magnetic field.

The most striking aspect of the data was just how varied the chromosphere turned out to be. Both along the portion of the Sun they studied and at different heights within it, the magnetic field varied significantly.

The team hopes to use this technique for multi-height magnetic measurements to map the entire chromosphere’s magnetic field. Not only would this help with our ability to predict space weather, it will tells us key information about the atmosphere around our star. (NASA)

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