Bringing the Stars Down to Earth

Thus by studying these isotopes in nuclear laboratories here on Earth — a far more peaceful testing ground than the interior of a star — the team realised they could shed light on the death throes of these stars. “This work started when we realized that a strongly suppressed, and hence previously ignored and experimentally unknown, transition between the ground states of neon-20 and fluorine-20 was a key piece of information needed to determine the electron capture rate in intermediate-mass stars,” says Professor Karlheinz Langanke, Research Director of GSI and FAIR.

Electron capture here demonstrated with Carbon-11, plays an important role in the fate of intermediate-mass stars. Image credit: JLab

By studying the decay rate of fluorine-20 and combining this with theoretical calculations, the team were able to tease out a value for the electron capture rate. Electron capture is a process in which an electron is drawn into an atomic nucleus. This results in the transformation of a proton to a neutron and a neutrino — the latter of which is ejected. As elements are characterised by the number of protons in their nucleus, the end result is the transformation of one element to another. This usually means the transformation of an unstable isotope to a more stable one.

The team's measurements — taken in the Accelerator Laboratory of the University of Jyväskylä — revealed a strong transition between the ground states of neon-20 and fluorine-20. This leads to electron capture in neon-20 occurring in much lighter densities than physicists had previously believed was possible. For intermediete-mass stars, this means that process is much more likely to occur and thus lead to a thermonuclear explosion rather than collapse into a neutron star.

“It is amazing to find out that a single transition can have such a strong impact on the evolution of a big object like a star,” remarks Dag Fahlin Strömberg, who was responsible for large parts of project’s simulations.

The team’s results have wider implications for the abundance and evolution of certain chemical elements in the galaxy because thermonuclear explosions eject far more material into their surroundings than gravitational collapse does. This ejected material is rich in titanium-50, chromium-54, and iron-60, meaning that the unusual titanium and chromium isotopic ratios found in some meteorites, and the discovery of iron-60 in deep-sea sediments could be produced by intermediate-mass stars. Should this be the case, it means that intermediate stars may have exploded in our galactic neighbourhood in both its relatively recent history — the last few million years — and its distant past — billions of years ago.

Should the team’s research be correct, a thermonuclear explosion seems the most likely end fate of mosy intermediete-mass stars. This would result in a Type Ia supernova leaving behind a unique type of white dwarf, known as an oxygen-neon-iron white dwarf. Thus, confirming the team’s conclusion relies on the detection of these white dwarfs. Their subsequent study should then grant insight into the mechanism that triggers the explosion.

Whilst waiting for those developments, the team has no intentions of resting on their laurels, however. There is still the question of what role convection within the star plays in the explosion to tackle. Also, current and planned nuclear accelerators here on Earth are set to investigate various isotopes and their properties in order to better understand their roles in these cosmic events.