December 8, 2010
Astronomers Find Sparkling Zirconium Star
A team of astronomers led by graduate student Naslim and her supervisor Dr Simon Jeffery from Armagh Observatory in Northern Ireland has found what at first sight appears to be the most zirconium-rich star ever discovered. Zirconium, the material used by jewelers to make false diamonds, glitters in clouds above the star's surface. The scientists publish their results in the journal Monthly Notices of the Royal Astronomical Society.
The team made the discovery while looking for chemical clues that explain why a small group of stars reaching the end of their lives, known as helium-rich hot subdwarfs, have much less hydrogen on their surfaces than other similar stars. Using data obtained with the Anglo-Australian Telescope at the Siding Spring Observatory in New South Wales, the team looked at the evolved star LS IV-14 116, 2000 light years from the Sun in the direction of the border between the constellations of Capricornus and Aquarius.
As expected, the spectrum of LS IV-14 116 had the usual lines arising from more common elements, but other strong lines were less easy to identify. A careful study showed four of these lines were due to a form of zirconium that only exists at temperatures above 20 000 degrees Celsius and that had never previously been found in an astronomical spectrum.
Team member Prof. Alan Hibbert, from Queen's University Belfast, computed a model of the zirconium atom to predict the expected line strengths. With this information, the team measured the zirconium abundance in LS IV -14 116 to be ten thousand times as high as in the Sun (meaning that one atom in every two hundred thousand is zirconium rather than one in two billion). Further work showed the remaining unidentified lines to come from strontium, germanium and yttrium and these elements are found to be between one thousand and ten thousand times more abundant than normal.
In their paper the Armagh team argues that the unusual abundances in LS IV-14 116 are caused by the formation of cloud layers in the star's atmosphere "“ the only part of a star that can be seen directly. High concentrations of certain elements, mainly metals heavier than calcium, build up in these clouds but the same elements are scarce in layers above and below, meaning that their overall abundance is near normal. Dr Natalie Behara, now at the Universit© Libre de Bruxelles, calculated models of the star's atmosphere. This may well have a dramatic appearance, with many thin cloud layers, each due to a different metal.
The team also suggests that the star is shrinking from being a bright cool giant to a faint hot subdwarf. As the star shrinks, different elements sink down or float up in the atmosphere to a region where they become highly visible, making the apparent composition very sensitive to the star's recent history.
Most stars like the Sun have about ten zirconium atoms for every million silicon atoms. LS IV-14 116 has two million zirconium atoms for every one million silicon atoms. It is estimated that the zirconium layer seen in LS IV-14 116 would weigh about four billion tons or 4,000 times the world's annual production of zirconium.
Describing the new results, Dr Simon Jeffery said "It was very exciting to discover these completely new chemical signatures in our data. The peculiar abundances measured in this star, and hopefully in others, offer a new tool to explore a stage of stellar evolution which is extremely difficult to observe directly." Naslim reports "The huge excess of zirconium was a complete surprise. We had no reason to think this star was more peculiar than any other faint blue star discovered so far."
The results of the study will appear in 'An extremely peculiar hot subdwarf with a ten-thousand fold excess of zirconium, yttrium and strontium', Naslim N. et al, Monthly Notices of the Royal Astronomical Society, in press.
Image Caption: An artist's impression of LS IV "“ 14 116. The white clouds are rich in zirconium and lie above the blue surface of the star. Image: Natalie Behara
On the Net:
- A preprint of the paper can be seen at http://arxiv.org/abs/1010.5146