April 27, 2016 ![Illustration of Cosmic-Ray “Air Showers”](/sites/lmf/files/styles/scaled_425h/public/2021-02/cosmic-rays.jpg?itok=HM1ij2n8)*An illustration of “air showers” that result when ultra-high-energy cosmic rays strike the top of the Earth’s atmosphere and collide with air nuclei, producing other particles that lose most of their energy before reaching the ground. Most cosmic rays are protons or helium nuclei from the sun, but the origins of the highest-energy cosmic rays, often nuclei from heavier elements like carbon and iron, are uncertain. Many scientists believe they are produced during supernova explosions, but recent studies indicate they might be sent on their way by activity near black holes at the center of the Milky Way and other galaxies. Credit: Asimmetrie/INFN, via CERN* [(Download Image)](/file-download/download/public/10436 "cosmic-rays.jpg") # Shedding Laser Light on Mysterious Cosmic Rays [ Opens in a new window ](https://www.facebook.com/sharer/sharer.php?u=https://lmf.llnl.gov/markdownify/node/1761&title=Shedding%20Laser%20Light%20on%20Mysterious%20Cosmic%20Rays "Share to Facebook") [ Opens in a new window ](https://twitter.com/intent/tweet?text=Shedding%20Laser%20Light%20on%20Mysterious%20Cosmic%20Rays+https://lmf.llnl.gov/markdownify/node/1761 "Share to X") [ ](mailto:?subject=Shedding%20Laser%20Light%20on%20Mysterious%20Cosmic%20Rays&body=https://lmf.llnl.gov/markdownify/node/1761 "Share by email") [ Opens in a new window ](https://www.linkedin.com/sharing/share-offsite/?url=https://lmf.llnl.gov/markdownify/node/1761 "Share to LinkedIn") [ ](javascript:window.print() "Print") [ Opens in a new window ](https://www.facebook.com/sharer/sharer.php?u=https://lmf.llnl.gov/markdownify/node/1761&title=Shedding%20Laser%20Light%20on%20Mysterious%20Cosmic%20Rays "Share to Facebook") [ Opens in a new window ](https://twitter.com/intent/tweet?text=Shedding%20Laser%20Light%20on%20Mysterious%20Cosmic%20Rays+https://lmf.llnl.gov/markdownify/node/1761 "Share to X") [ ](mailto:?subject=Shedding%20Laser%20Light%20on%20Mysterious%20Cosmic%20Rays&body=https://lmf.llnl.gov/markdownify/node/1761 "Share by email") [ Opens in a new window ](https://www.linkedin.com/sharing/share-offsite/?url=https://lmf.llnl.gov/markdownify/node/1761 "Share to LinkedIn") [ ](javascript:window.print() "Print") By Charlie Osolin The Earth is under constant bombardment by subatomic particles called cosmic rays, including some, known as ultra-high-energy cosmic rays, that pack much more punch than the world’s most powerful particle accelerators. Fortunately, Earth’s atmosphere protects us by dissipating most of that energy before it reaches the ground. But where do these ultrafast cosmic rays come from, and how are they accelerated to such high energies—one quadrillion (1015) electron volts and more? Scientists have been searching the heavens for answers to those questions for many decades, yet much about the origin and nature of ultra-high-energy cosmic rays remains a mystery. Now an international team of researchers is trying a different approach. Instead of looking deep into the universe with telescopes, or trying to capture the debris from atmospheric cosmic-ray collisions with particle detectors, they’re trying to duplicate the actual conditions that could contribute to cosmic-ray acceleration right here on Earth, in the NIF Target Chamber. In a NIF Discovery Science campaign conducted by the Astrophysical Collisionless Shock Experiments with Lasers (ACSEL) collaboration, the researchers are carrying out a series of experiments aimed at understanding the possible role of collisionless shocks and related intergalactic magnetic fields in cosmic-ray acceleration. ![Technician Prepares Proton Radiography Imaging Diagnostic](https://lmf.llnl.gov/sites/lmf/files/styles/large/public/grant.jpg?itok=MVhb7XmV "Technician Prepares Proton Radiography Imaging Diagnostic") Target Diagnostics Facility technician Glen Grant mounts a large-aperture proton radiography imaging diagnostic on the snout of a diagnostic instrument manipulator for a March 29 Discovery Science collisionless shock experiment. The experiment generated magnetic fields through the formation of plasma instabilities (known as filamentary Weibel instabilities) which trap ions in the plasma and form shocks. This type of collisionless shock may be contributing to cosmic ray acceleration. In collisionless shocks, the charged particles in a plasma (a medium consisting of freely moving ions and free electrons) pass by largely without colliding with each other; such shocks occur in many astrophysical phenomena including supernova remnants, gamma-ray bursts, and jets from active galactic nuclei. NIF is the only facility capable of creating plasmas with sufficiently high density (greater than 1020 particles per cubic centimeter), high flow velocity (greater than 1,000 kilometers per second), and high temperature (greater than 1,000 electron volts) to conduct these experiments. In the scaled NIF experiments, the collisional mean free path—the average distance traveled by a particle between collisions with other particles—is much larger than the experimental volume, yet the collisionless shocks created are similar to the astrophysical conditions observed in space. The two most recent ACSEL experiments, conducted on NIF on March 29, studied high-speed collisionless shock formation by firing more than 125 NIF beams at targets composed of two plastic foils facing each other. The associated magnetic field was backlighted, or probed, by protons from a tiny laser-irradiated sphere known as an "exploding pusher" target filled with a mixture of deuterium and helium-3 (D3He). ![Collisionless Shock Target and Image](https://lmf.llnl.gov/sites/lmf/files/styles/carousel_580_430/public/collissionless_image.jpg?itok=GkEGAImD "Collisionless Shock Target and Image") (Left) The collisionless shock target consists of two opposed plastic foils separated by 10 millimeters, each heated by 250 kilojoules of laser energy. The foils create plasmas that accelerate and collide, while a D3He-filled exploding pusher (at the end of the L-shaped arm below the target) creates a proton source to probe the self-generated magnetic fields in the interaction region. The magnetization effects on the counterpropagating plasmas were imaged with proton pulses delayed by 3.5 and seven nanoseconds after the main laser pulse and detected by the large-aperture proton imager. (Right) An image of the targets captured by the upper static x-ray imager (SXI) showing the emissions from the two heated plastic foils and the exploding pusher proton backlighter. This series of experiments was the first to use the D3He-filled exploding pusher, which was developed in collaboration with the Massachusetts Institute of Technology (MIT) Plasma Science and Fusion Center, as the proton backlighter for a physics experiment on NIF. The signature of the Weibel instabilities would be filamentary structures caused by the magnetic nature of flow interactions and shock formation; processing of the data gathered by the proton radiography imager is now under way. Participating in the ACSEL campaign are Osaka University, LLNL, Oxford University, Princeton University, MIT, the SLAC National Accelerator Laboratory, the University of Chicago, Michigan University, Los Alamos National Laboratory, and UC San Diego. For more information on the ACSEL campaign, see [ "International Team Conducts First Collisionless Shock Experiment on NIF.](https://lasers-prod.llnl.gov/international-team-conducts-first-collisionless-shock-experiment-nif)" ![Collisionless Shock Team](https://lmf.llnl.gov/sites/lmf/files/styles/scaled_425h/public/collisionlless_shock_team.jpg?itok=yJhcTB9E "Collisionless Shock Team") Members of the ACSEL collaboration who participated in the March 29 experiments (from left): Dmitri Ryutov (LLNL), Hans Rinderknecht (LLNL), Samuel Totorica (Stanford University), Brandon Lahmann (MIT), Hye-Sook Park (LLNL), Chikang Li (MIT), Bruno Van Wonterghem (LLNL), Dan Kalantar (LLNL), Youichi Sakawa (Osaka University), Bob Burr (LLNL), Channing Huntington (LLNL), Steve Ross (LLNL), Drew Higginson (LLNL), George Swadling (LLNL), and Brad Pollock (LLNL). 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