On August 11, NASA plans to launch Earth’s first spacecraft to venture inside the orbits of Venus and Mercury to touch the very edge of the sun’s fiery corona.
“This is a piece of heliophysics science we all really wanted for a long time, since the 1950s,” said Stuart Bale, a UC Berkeley professor of physics, former director of the campus’s Space Sciences Laboratory and one of four principal investigators for the instruments aboard the mission. “For me personally, I’ve been working on the probe since it was approved in 2010, but I really spent a large part of my career getting ready for it.”
The solar probe will travel faster than any spacecraft in history, at its peak reaching 430,000 miles per hour, and will be only four-and-a-half solar diameters, or 3.8 million miles, above the solar surface at its closet approach to the sun around 2024. The probe is equipped with a heat shield to protect its sensors from the sun’s heat, which could reach 2,500 degrees Fahrenheit, nearly hot enough to melt steel.
At this distance, the solar probe will be within a region where electrons and ionized atoms – mostly hydrogen ions, or protons, and helium ions, called alpha particles – are accelerated and shot out toward the planets at high speed.
When these ions, called the solar wind, hit Earth, they interact with Earth’s magnetic fields and generate the northern and southern lights as well as storms in the outermost atmosphere that interfere with radio communications and satellite operations. Accelerated to higher speeds, so-called “solar energetic” particles can pose a hazard to astronauts.
Scientists still do not know how the solar wind ions are accelerated, or why the ions and electrons in the corona are so much hotter, about 1.7 million degrees Fahrenheit, than the surface of the sun, which is a relatively cool 10,000 degrees Fahrenheit. The Parker Solar Probe could answer those questions, and help scientists on Earth forecast the large eruptions from the sun that pose the greatest peril to our spacecraft and communications systems.
Follow the magnetic fields
FIELDS, a suite of instruments built at UC Berkeley’s Space Sciences Laboratory, is one of four instrument packages aboard the probe. With the help of a six-foot boom projecting in the direction the spacecraft is moving, it will measure the electric and magnetic fields in the corona, which will tell scientists the total energy streaming outward from the sun.
These measurements will test one theory of how the sun heats the corona: by jiggling the magnetic field lines. The strong magnetic field of the sun stretches out far into space, but the magnetic field lines are anchored in surface regions that constantly move around because of convection below, like boiling water. The constant movement of the base of the magnetic field lines creates waves that travel outward along the lines, just as jiggling the end of a long rope sends waves to the other end. Somehow, these so-called Alfvén waves accelerate particles to high speeds and fling them into space.
“If the wave-driven model is correct, then I think our measurements will be the fundamental measurements on the mission,” Bale said.
The other popular theory is that tiny flares called nanoflares all over the surface of the sun produce magnetic fields that cross, reconnect and fling disconnected loops of magnetic field into space, accelerating ions along with it. This was first proposed in 1987 by Eugene Parker, after whom the solar probe is named. Now 91, Parker predicted the existence of and named the solar wind in the 1950s.
Radio antennas on the FIELDS package will look for radio waves created by nanoflares, which have yet to be detected, while another package of instruments, SWEAP (Solar Wind Electrons Alphas and Protons), will record the speed of solar wind electrons, protons and alpha particles as they whiz by the probe. Correlating nanoflare or microflare activity with the flux of particles streaming from the sun could confirm the magnetic reconnection theory. SWEAP is led by the University of Michigan and the Smithsonian Astrophysical Observatory in Cambridge, Massachusetts, though much of the instrument was designed and built at the Space Sciences Laboratory at UC Berkeley.
Two other instrument packages will be aboard the probe. WISPR, the Wide-Field Imager for Parker Solar Probe, was built at the Naval Research Laboratory and will capture visible-light images of the sun’s corona directly in front of the orbiting probe. ISʘIS (pronounced E-sis) – short for Integrated Science Investigation of the Sun, and including ʘ, the symbol for the Sun, in its acronym – is led by Princeton University and will measure the energy and identity of energized electrons and ions, including ions heavier that hydrogen and helium, in order to find out how they are sometimes accelerated to nearly light speed close to the sun.
Together, these instruments should be able to record the speed-up of the solar wind from subsonic to supersonic and the birth of the highest-energy solar particles.
“Plasma physics is really hard to study in the laboratory,” said Bale, who focuses on the role of magnetic fields and ionized plasma in space, in particular around stars like the sun. “Sticking a spacecraft right in the hot plasma makes an ideal laboratory.”
Looping around Venus
This probe is the chance of a lifetime for Bale. Though his team will deploy booms and test instrument functions one day after launch, most of the instruments will then be turned off and won’t begin taking real measurements of the corona until the probe reaches its first close approach to the sun in November.
After a loop around Venus to slow down, the probe will get the closest any spacecraft has ever been to the sun, a distance from the center of the sun equal to 36 times the sun’s radius (36 solar radii). Venus orbits at 155 solar radii and Mercury at 83 solar radii.
Over the next six years, the probe will loop around Venus six more times, gradually working its way to approximately 9.8 solar radii from the center of the sun. There, it will be well within the corona, at the outer edge of which particles exceed the speed of sound – the Alfvén speed, which is about 200 miles per second – and no longer call the sun home.
“The goal of the mission is to get inside that transition region, so we get into the real corona where the flow is subAlfvénic,” Bale said. “We think that boundary is at about 15 solar radii, so we probably won’t start hitting it until 2021.”
Once inside the corona, the probe may see the jiggling magnetic field lines, or Alfvén waves, bouncing back and forth between the sun’s surface and the edge of the corona, a turbulent cascade that may be the feedback loop that accelerates particles to the high speeds seen in the solar wind.
“In early December, I am counting on having that first pass of data at 35 solar radii, and I am sure it will be revolutionary. There will be great new stuff in there, from what we know about previous missions,” Bale said.
Over its seven-year mission lifetime, the probe will dip into the sun’s inner atmosphere 24 times. As part of NASA’s outreach efforts, more than 1.1 million people submitted their names to be recorded on a memory card that will accompany the spacecraft around the sun.
The probe is scheduled for launch in the early hours of Monday, Aug. 11, from Cape Canaveral Air Force Station in Florida, aboard a United Launch Alliance Delta IV Heavy rocket with an upper stage to boost it out of Earth orbit toward Venus.
Since the mission was approved in 2010, some 40 to 50 people at Berkeley’s Space Sciences Laboratory have worked on the solar probe. Through the formal end of the mission in 2026, and including subsequent data analysis, UC Berkeley will have received about $100 million out of a total of $1.5 billion spend on the mission.