Led by nuclear astrophysicist Kelly Chipps of the U.S. Department of Energy’s Oak Ridge National Laboratory (ORNL), scientists working in the lab have produced a signature nuclear reaction that occurs on the surface of a neutron star gobbling mass from a companion star. Their achievement improves understanding of stellar processes generating diverse nuclear isotopes.

“Neutron stars are really fascinating from the points of view of both nuclear physics and astrophysics,” said Chipps, who led the study, which was published in Physical Review Letters. “A deeper understanding of their dynamics may help reveal the cosmic recipes of elements in everything from people to planets.”

Chipps heads the Jet Experiments in Nuclear Structure and Astrophysics, or JENSA, which has collaborators from nine institutions in three countries. The team uses a unique gas jet target system, which produces the world’s highest-density helium jet for accelerator experiments, to understand nuclear reactions that proceed with the same physics on Earth as in outer space.

The process of nucleosynthesis creates new atomic nuclei. One element can turn into another when protons or neutrons are captured, exchanged or expelled.

A neutron star has an immense gravitational pull that can capture hydrogen and helium from a nearby star. The material amasses on the neutron star surface until it ignites in repeated explosions that create new chemical elements.

Many nuclear reactions powering the explosions remain unstudied. Now, JENSA collaborators have produced one of these signature nuclear reactions in a lab at Michigan State University. It directly constrains the theoretical model typically used to predict element formation and improves understanding of the stellar dynamics that generate isotopes.

The JENSA system was built at ORNL, operated for the experiment at National Superconducting Cyclotron Laboratory, and afterwards moved to FRIB for use in future experiments. JENSA provides a target of lightweight gas that is dense, pure and localized within a couple millimeters. JENSA will also provide the primary target for the Separator for Capture Reactions, or SECAR, a detector system at FRIB that allows experimental nuclear astrophysicists to directly measure the reactions that power exploding stars. Co-author Michael Smith of ORNL and Chipps are members of SECAR’s project team.

For the current experiment, the scientists struck a target of alpha particles (helium-4 nuclei) with a beam of argon-34. (The number after an isotope indicates its total number of protons and neutrons.) The result of that fusion produced calcium-38 nuclei, which have 20 protons and 18 neutrons. Because those nuclei were excited, they ejected protons and ended up as potassium-37 nuclei.

High-resolution charged-particle detectors surrounding the gas jet precisely measured energies and angles of the proton reaction products. The measurement took advantage of detectors and electronics developed at ORNL under the leadership of nuclear physicist Steven Pain. Accounting for the conservation of energy and momentum, the physicists back-calculated to discover the dynamics of the reaction.

“Not only do we know how many reactions occurred, but also we know the specific energy that the final potassium-37 nucleus ended up in, which is one of the components predicted by the theoretical model,” Chipps said.

The lab experiment improves understanding of nuclear reactions that occur when material falls onto the surface of an important subset of neutron stars. These stars are born when a massive star runs out of fuel and collapses into a sphere about as wide as a city such as Atlanta, Georgia. Then gravity squeezes fundamental particles as close together as they can get, creating the densest matter we can directly observe. One teaspoon of neutron star would weigh as much as a mountain. Neutron-packed stars rotate faster than blender blades and make the universe’s strongest magnets. They have solid crusts surrounding liquid cores containing material shaped like spaghetti or lasagna noodles, earning them the nickname “nuclear pasta.”

“Because neutron stars are so weird, they are a useful naturally occurring laboratory to test how neutron matter behaves under extreme conditions,” Chipps said.

Achieving that understanding takes teamwork. Astronomers observe the star and collect data. Theoreticians try to understand physics inside the star. Nuclear physicists measure nuclear reactions in the lab and test them against models and simulations. That analysis reduces large uncertainties resulting from a dearth of experimental data. “When you put all of those things together, you really start to understand what’s happening,” Chipps said.

“Because the neutron star is superdense, its huge gravity can pull hydrogen and helium over from a companion star. As this material falls to the surface, the density and temperature grow so high that a thermonuclear explosion can occur that can propagate across the surface,” Chipps said. Thermonuclear runaway transforms nuclei into heavier elements. “The reaction sequence can produce dozens of elements.”

Surface explosions do not destroy the neutron star, which goes right back to what it was doing before: feeding off its companion and exploding. Repeated explosions pull crust material into the mix, creating a bizarre composition in which heavy elements formed during previous explosions react with lightweight hydrogen and helium.

Theoretical models predict which elements form. Scientists typically analyze the reaction that the JENSA team measured using a statistical theoretical model called the Hauser-Feshbach formalism, which assumes that a continuum of excited energy levels of a nucleus can participate in a reaction. Other models instead assume that only a single energy level participates.

“We’re testing the transition between the statistical model being valid or invalid,” Chipps said. “We want to understand where that transition happens. Because Hauser-Feshbach is a statistical formalism—it relies on having a large number of energy levels so effects over each individual level are averaged out—we’re looking for where that assumption starts to break down. For nuclei like magnesium-22 and argon-34, there’s an expectation that the nucleus doesn’t have enough levels for this averaging approach to be valid. We wanted to test that.”

A question remained about whether the statistical model was valid for such reactions taking place in stars rather than earthly laboratories. “Our result has shown that the statistical model is valid for this particular reaction, and that removes a tremendous uncertainty from our understanding of neutron stars,” Chipps said. “It means that we now have a better grasp of how those nuclear reactions are proceeding.”

Next, the researchers will try to improve the statistical model by further testing its limits. A past paper explored atomic mass 22, a magnesium nucleus, and found the model incorrect by almost a factor of 10. The current ORNL-led paper, probing 12 atomic mass units above this, found that the model correctly predicted reaction rates.

“Somewhere between [atomic] mass 20 and 30, this transition between where the statistical model is valid and where it’s not valid is taking place,” Chipps said. “The next thing is to look for reactions in the middle of that range to see where this transition is occurring.” Chipps and her JENSA collaborators have begun that endeavor.

The title of the paper is “First direct measurement of the ³⁴Ar(α,p)³⁷K reaction cross section for mixed hydrogen and helium burning in accreting neutron stars.”

DOE’s Office of Science, the National Science Foundation and ORNL’s Laboratory Directed Research and Development program supported the work.

UT-Battelle manages ORNL for the Department of Energy’s Office of Science, the single largest supporter of basic research in the physical sciences in the United States. The Office of Science is working to address some of the most pressing challenges of our time. For more information, please visit energy.gov/science.

By Dawn Levy, Oak Ridge National Laboratory

Read the original article on the ORNL website: Element creation in the lab deepens understanding of neutron stars

Michigan State University (MSU) operates the Facility for Rare Isotope Beams (FRIB) as a user facility for the U.S. Department of Energy Office of Science (DOE-SC), supporting the mission of the DOE-SC Office of Nuclear Physics. Hosting what is designed to be the most powerful heavy-ion accelerator, FRIB enables scientists to make discoveries about the properties of rare isotopes in order to better understand the physics of nuclei, nuclear astrophysics, fundamental interactions, and applications for society, including in medicine, homeland security, and industry.

The U.S. Department of Energy Office of Science is the single largest supporter of basic research in the physical sciences in the United States and is working to address some of today’s most pressing challenges. For more information, visit energy.gov/science.