Planets Need Heavy-Metal
A comparison of 754 nearby stars like our sun – some with planets and some without – shows definitively that the more iron and other metals there are in a star, the greater the chance it has a companion planet.
|Artist concept of star system, HD70642.
Credit:John Rowe animation
"Astronomers have been saying that only 5 percent of stars have planets, but that’s not a very precise assessment," said Debra Fischer, a research astronomer at the University of California, Berkeley. "We now know that stars which are abundant in heavy metals are five times more likely to harbor orbiting planets than are stars deficient in metals. If you look at the metal-rich stars, 20 percent have planets. That’s stunning."
"The metals are the seeds from which planets form," added colleague Jeff Valenti, an assistant astronomer at the Space Telescope Science Institute (STScI) in Baltimore, Md.
The research team presented their analyses at the International Astronomical Union meeting in Sydney, Australia.
Iron and other elements heavier than helium – what astronomers lump together as "metals" – are created by fusion reactions inside stars and sown into the interstellar medium by spectacular supernova explosions. Thus, while metals were extremely rare in the early history of the Milky Way galaxy, over time, each successive generation of stars became richer in these elements, increasing the chances of forming a planet.
"Stars forming today are much more likely to have planets than early generations of stars," Valenti said. "It’s a planetary baby boom."
As the number of extrasolar planets has grown – about 100 stars are now known to have planets – astronomers have noticed that stars rich in metals are more likely to harbor planets. A correlation between a star’s "metalicity" – a measure of iron abundance in a star’s outer layer that is indicative of the abundance of many other elements, from nickel to silicon – had been suggested previously by astronomers Guillermo Gonzalez and Nuno Santos based on surveys of a few dozen planet-bearing stars.
|Scene from a moon orbiting the extra-solar planet in orbit around the star HD70642.
Credit:David A. Hardy, astroart.org (c) pparc.ac.uk
The new survey of metal abundances by Fischer and Valenti is the first to cover a statistically large sample of 61 stars with planets and 693 stars without planets. Their analysis provides the numbers that prove a correlation between metal abundance and planet formation.
"People have looked already in fair detail at most of the stars with known planets, but they have basically ignored the hundreds of stars that don’t seem to have planets. These under-appreciated stars provide the context for understanding why planets form," said Valenti, who is an expert at determining the chemical composition of stars.
The data show that stars like the sun, whose metal content is considered typical of stars in our neighborhood, have a 5 to 10 percent chance of having planets. Stars with three times more metal than the sun have a 20 percent chance of harboring planets, while those with 1/3 the metal content of the sun have about a 3 percent chance of having planets. The 29 most metal-poor stars in the sample, all with less than 1/3 the sun’s metal abundance, had no planets.
"These data suggest that there is a threshold metalicity, and thus not all stars in our galaxy have the same chance of forming planetary systems," Fischer said. "Whether a star has planetary companions or not is a condition of its birth. Those with a larger initial allotment of metals have an advantage over those without, a trend we’re now able to see clearly with this new data."
The two astronomers determined metal composition by analyzing 1,600 spectra from more than 1,000 stars before narrowing the analysis to 754 stars that had been observed long enough to rule a gas giant planet in or out. Some of these stars have been observed for 15 years by Fischer, Geoffrey Marcy, professor of astronomy at UC Berkeley, and colleague Paul Butler, now at the Carnegie Institution of Washington, in their systematic search for extrasolar planets around nearby stars. All 754 stars were surveyed for more than two years, enough time to determine whether a close-in, Jupiter-size planet is present or not.
Though the surfaces of stars contain many metals, the astronomers focused on five – iron, nickel, titanium, silicon and sodium. After four years of analysis, the astronomers were able to group the stars by metal composition and determine the likelihood that stars of a certain composition have planets. With iron, for example, the stars were ranked relative to the iron content of the sun, which is 0.0032%.
|Our Milky Way galaxy is packed with 400 billion stars and perhaps even more planets.
"This is the most unbiased survey of its kind," Fischer emphasized. "It is unique because all of the metal abundances were determined with the same technique and we analyzed all of the stars on our project with more than two years of data."
Fischer said the new data suggest why metal-rich stars are likely to develop planetary systems as they form. The data are consistent with the hypothesis that heavier elements stick together easier, allowing dust, rocks and eventually planetary cores to form around newly ignited stars. Since the young star and the surrounding disk of dust and gas would have the same composition, the metal composition observed from the star reflects the abundance of raw materials, including heavy metals, available in the disk to build planets. The data indicate a nearly linear relationship between amount of metals and the chance of harboring planets.
"These results tell us why some of the stars in our Milky Way galaxy have planets while others do not," said Marcy. "The heavy metals must clump together to form rocks which themselves clump into the solid cores of planets."
During the next 15 years, American and European scientists hope to launch more than half a dozen missions to search our corner of the Milky Way galaxy for terrestrial planets.
To search for Earth-like planets around stars beyond our solar system, the space-borne telescope Kepler Mission is scheduled for launch in 2006. Kepler will simultaneously observe 100,000 stars in our galactic neighborhood, looking for Earth-sized or larger planets within the "habitable zone" around each star – the not-too-hot, not-too-cold zone where liquid water could exist on a planet.
One NASA estimate says Kepler should discover 50 terrestrial planets if most of those found are about Earth’s size, 185 planets if most are 30 percent larger than Earth, and 640 if most are 2.2 times Earth’s size. In addition, Kepler is expected to find almost 900 giant planets close to their stars and about 30 giants orbiting at Jupiter-like distances from their parent stars.
After Kepler, NASA is considering a 2009 launch for the Space Interferometry Mission (SIM). SIM’s primary mission will be to measure distances to stars with 100 times greater precision than currently is possible. This will improve estimates of the size of the universe, and help determine the true brightness of stars, allowing us to learn more about their chemical compositions and evolutions. SIM also will look for Earth-sized planets in the habitable zones around some 200 stars.
SIM will be an interferometer, which means it will combine interacting light waves from three telescopes. This interaction, called interference, makes the individual telescopes act as though they were a single, larger telescope with greater light-gathering ability.
Future missions will search for many more planets. ESA’s Herschel mission, for instance, will take detailed pictures of stars that might harbor dusty remnants of entire solar systems. As these images become available, astronomers will be able to predict the sizes and orbits of giant planets within the distant solar system.
The research by Fischer and Valenti is supported by the National Aeronautics and Space Administration, the National Science Foundation, the Particle Physics and Astronomy Research Council (PPARC) in the United Kingdom, the Anglo-Australian Observatory, Sun Microsystems, the Keck Observatory and the University of California’s Lick Observatories.