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Ring around white dwarf
Link to print quality picture
Picture by Mark A. Garlick

Strict Embargo : Do not publish or broadcast before
Friday 00.01 hours 22nd December 2006 UK time

Metal Ring Round White Dwarf Solves Missing Planets Puzzle

Astrophysicists at the University of Warwick have found an unusual ring of metal-rich gas orbiting very close around a white dwarf star. The presence of the ring helps solve a problem for astronomers who, up till now, have been puzzled by the apparent absence of planets around white dwarf stars. Their research is published today in the Friday December 22nd edition of the journal Science. Click on the picture above for a print quality high resolution artist's impression of the White Dwarf and its ring.

The research team led by Dr Boris Gänsicke and Professor Tom Marsh from the University of Warwick's Department of Physics found this unusual gas disc around a relatively young white dwarf star called SDSS1228+1040. It is located in the constellation Virgo and it is around 463 light years distant from our solar system. The star became a white dwarf around 100 million years ago, and is still fairly hot with a surface temperature around 22000 degrees.

The team observed double-peaked emission lines superimposed on the white dwarf's starlight caused by iron, magnesium and calcium from material in the vicinity of the star. This indicated that they were dealing with a disc of metal-gas orbiting close around the star (around 1.2 solar radii or roughly half a million miles). The observations also show that we are looking nearly edge-on to the ring around the white dwarf.

The likely origin of the disc is an asteroid, of at least 50 kilometres in size, which approached close enough to the star to be broken up by tides generated from the gravitational forces of the white dwarf. Those disrupted remains then entered a close orbit around the star and is evaporated by the radiation from the white dwarf.

White dwarfs begin as a star similar to our sun (or a star up to 8 times bigger than our sun). Late in the star's life it swells into a red giant probably destroying any inner planets at orbits such as those of Mercury and Venus and pushing out other planets and asteroids to a more distant orbit than before.
Here is a link to some simple diagrams explaining this:

In the evolution of what is today a white dwarf, the progenitor of SDSS1228+1040 will have destroyed all planetary material out to a distance of 1000 solar radii (roughly 500 million miles), but asteroids still exist today at larger distances. To destabilise an asteroid from an orbit that far out, it needs the gravitational force of a larger object, such as a relatively massive planetesimal, or a genuine planet. While the presence of asteroids around white dwarf has been hypothesized before, the case of SDSS1228+1040 provides the first clear proof of the debris of a planetary disc around a white dwarf, and provides an example of what our own Solar system may look like in around 5 to 8 billion years.

This "metal" disc around SDSS1228+1040 appears to be relatively rare. Before their study, three white dwarfs, out of a study of a few hundred, were suggested to be surrounded by planetary debris material. However, in none of those three cases could a definite proof of an asteroid origin be made due to the lack of information on the geometry and the chemical abundance of the material found in the vicinity of these stars. As part of their study, the Warwick team investigated data for 500 additional white dwarfs without finding conclusive evidence for another system harbouring such a disc. The rarity of such a ring made from a disrupted asteroid tells us that the majority of planetary systems may look quite different from our own Solar system. They may not have asteroid belts at all, or not as far out as it is the case in the Solar system, or they may not have planets at such great distances as Mars or Jupiter. This conclusion is consistent with the current knowledge on extrasolar planets found around others stars similar to the Sun, where the vast majority of the exo-planets are in very close orbits around their host stars.

Notes for editors

1. Dr Gänsicke is available on Monday 18th, Tuesday 19th and Wednesday 20th  December for interview. He is not available on Thursday 21st December

2. Science have told us that copies of the full embargoed Science paper can only be distributed only by Science's AAAS Office of Public Programs on 1-202-326-6440 or

For further information please contact:

Dr Boris Gänsicke, Department of Physics
University of Warwick 02476 574741
Mobile 07901 875177

Or Richard Fern, Press Officer University of Warwick
Tel: 024 76 574255 mobile 07876 217740

Peter Dunn, Press and Media Relations Manager, Communications Office, University of Warwick,
024 76 523708 email:

PR82 PJD 18th December 2006

Page owner: Eleanor Lovell Last revised: Sat, Dec 16, 2006
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