Ancient stars shed light on the prehistory of the Milky Way

The results are published in the Astrophysical Journal Letters.

Shortly after the Big Bang the universe was dominated by the mysterious dark matter along with hydrogen and helium. As the dark matter and gasses clumped together under their own gravity, they formed the first stars.

In the scorching interior of these stars, hydrogen and helium melted together and formed the first heavier elements like carbon, nitrogen and oxygen, and after a 'short' while (a few hundred million years) all of the known elements were in place. However, these early stars only contained a thousandth of the heavy-elements seen in the Sun today.

Every time a massive star burns out and dies in a violent explosion known as a supernova, it releases clouds of gas and newly formed elements out into space, where the gas clouds contract again and finally collapse and form new stars. In this way, the new generations of stars become richer and richer in heavy elements.

Fossils from the galaxy's childhood

It is therefore surprising to find stars from the early universe that are relatively rich in the very heaviest elements. But they exist and even right in our own galaxy, the Milky Way.

"In the outer parts of the Milky Way there are old 'stellar fossils' from our own galaxy's childhood. These old stars lie in a halo above and below the galaxy's flat disc. In a small percentage- approx. 1-2 percent of these primitive stars, you find abnormal quantities of the heaviest elements relative to iron and other 'normal' heavy elements," explains Terese Hansen, who is an astrophysicist in the research group Astrophysics and Planetary Science at the Niels Bohr Institute at the University of Copenhagen.

The research group at the Niels Bohr Institute had studied these ancient stars with ESO's giant telescopes in Chile over several years. To get a handle on the origin of the heavy elements, they followed 17 of these 'abnormal' stars for another four years with the Nordic Optical Telescope on La Palma.

Terese Hansen used her master's thesis to analyse the observations. "After slaving away on these very difficult observations for a few years I suddenly realised that three of the stars had clear orbital motions that we could define, while the rest didn't budge out of place and this was an important clue to explaining what kind of mechanism must have created the elements in the stars," explains Terese Hansen, who calculated the velocities along with researchers from the Niels Bohr Institute and Michigan State University, USA.

Gold plated gas clouds

She explains that there are two theories that can explain the early stars' overdose of heavy elements. One theory is that these stars are all close binary star systems where one star has exploded as a supernovae and has coated its companion star with a thin layer of freshly made gold, platinum, uranium and so on.

The other theory is that early supernovae (exploding giant stars) could shoot the heavy elements out in jets in different directions, so these elements would be built into some of the diffuse gas clouds that formed some of the stars we see today in the galaxy's halo.

"My observations of the motions of the stars showed that the great majority of the 17 heavy-element rich stars are in fact single. Only three (20 percent) belong to binary star systems -- this is completely normal, 20 percent of all stars belong to binary star systems. So the theory of the gold-plated neighbouring star cannot be the general explanation. The reason why some of the old stars became abnormally rich in heavy elements must therefore be that exploding supernovae sent jets out into space. In the supernova explosion the heavy elements like gold, platinum and uranium are formed and when the jets hit the surrounding gas clouds, they will be enriched with the elements and form stars that are incredibly rich in heavy elements," says Terese Hansen, who immediately after her groundbreaking results was offered a PhD grant by one of the leading European research groups in astrophysics at the University of Heidelberg.