Figure 1. Artist's rendering of what HD 131488's inner planetary system might look like as two large rocky bodies collide. Inset illustrates the location of HD 131488's dust belts (top) and comparable regions to our own Solar System (bottom). HD 131488's hot inner dust belt has similar separations from its host star as the terrestrial planet zone (TPZ) around our Sun while the star's cool dust belt has similar separations from its host star as the Kuiper Belt region in our Solar System. Also shown for our Solar System are the orbits of Jupiter, Saturn, Uranus, and Neptune. Image Credit: Lynette Cook for Gemini Observatory/AURA
Figure 2. Mid-infrared spectroscopy of a sample of stars known to host warm dust in their terrestrial planet zones. The three spectra at the top of the plot illustrate the features of olivine and pyroxene dust species whereas the bottom three spectra illustrate the features of silica dust species. These species of dust are commonly found in comets and asteroids in our own Solar System. The solid middle curve shows the Gemini-South T-ReCS spectrum of HD 131488 which exhibits a dust spectral feature that is significantly different from the others shown. Comparison spectra were taken from the Spitzer-IRS archive
Using the Gemini South telescope in Chile, astronomers at UCLA have found dusty evidence for the formation of young, rocky planets around a star some 500 light years distant. But these potential extrasolar worlds are alien in an even more intriguing way… In the aftermath of collisions between planetary embryos around this star the researchers discovered that the dusty debris bears no resemblance to the planetary building blocks of our own Solar System.
"Until now, warm dust found around other stars has been very similar in composition to asteroidal or cometary material in our Solar System,” said Dr. Carl Melis, who led the research while a graduate student at UCLA. “This newly discovered dusty star is a compelling exception.” Melis reported these findings today at the 215th American Astronomical Society meeting in Washington, DC.
The star, known as HD 131488, appears to be surrounded by warm dust in a region called the terrestrial planet zone, where the star heats the dust to temperatures similar to those found on Earth. "What makes HD 131488 truly unique is the unidentified dust species released from the colliding bodies as well as the presence of cold dust far away from the star,” said UCLA professor of physics and astronomy Dr. Benjamin Zuckerman, who is a co-author of the research which is pending publication. “These two characteristics make HD 131488 unlike any other star with evidence for massive quantities of dust in its terrestrial planet zone."
Infrared imaging and spectroscopy of the HD 131488 system using an instrument called T-ReCS on the Gemini South telescope in Chile provided the data used by the team in analyzing the warm inner dust. "Typically, dust debris around other stars, or our own Sun, is of the olivine, pyroxene, or silica variety, minerals commonly found on Earth," said Melis. “The material orbiting HD 131488 is not one of these dust types. We have yet to identify what species it is - it really appears to be a completely alien type of dust.”
The amount of cold and warm dust around HD 131488 is comparable to the amount of cool material seen around other dusty main sequence stars (the majority of a star's life where it is stable like our Sun is spent on the main-sequence). Melis and his team argue that the most plausible explanation for the unusually large quantity of warm dust is a recent collision of two rocky planetary mass bodies. Such a collision would provide an appropriate source of dust particles that are needed to explain the observations.
While the mysteriously composed warm dust is located at a distance from HD 131488 that is comparable to the Earth–Sun separation, the team also found cooler dust about 45 times further out. This outer dusty region is analogous to the Kuiper Belt in our own Solar System where many minor planets orbit the Sun just beyond the orbit of Neptune.
"The hot dust almost certainly came from a recent catastrophic collision between two large rocky bodies in HD 131488's inner planetary system," Melis said. "The cooler dust, however, is unlikely to have been produced in a catastrophic collision and is probably left over from planet formation that took place farther away from HD 131488."
"Although dusty telltales of planetary formation processes in the outer regions surrounding young stars have often been seen with infrared-sensitive space telescopes, for some reason stars that have large amounts of orbiting warm dust do not also show evidence for the presence of cold dust. HD 131488 dramatically breaks this pattern," said Zuckerman.
HD 131488 joins five other stars with masses a few times larger than the Sun and with evidence of dust in their terrestrial planet zone. According to Melis, "Of the thousands of intermediate mass stars that could have been detected with such large quantities of terrestrial planet zone dust, only these five were. Interestingly, all five of these stars have ages in the range of 10-30 million years. This finding indicates that the epoch of final catastrophic mass accretion for terrestrial planets, the likes of which could have resulted in the formation of the Earth-Moon system in our own Solar System, occurs in this narrow age range for stars somewhat more massive than the Sun." Similar statistics for stars of solar mass are not yet available for comparison.
The team will continue to study HD 131488 to try and uncover the nature of its strange dust composition and search for additional stars with evidence for rocky planet formation.
HD 131488 is located in the direction of the constellation Centaurus and is three times more massive and 33 times more luminous than our own Sun. The star is part of a major southern hemisphere star forming region known as the Upper-Centaurus-Lupus association whose members are believed to be about 10 million years old. By contrast, the Sun and Earth are about 4.6 billion years old.
These results are based on infrared observations made with the Gemini South telescope, the Infrared Astronomical Satellite (IRAS) space-based infrared observatory (which made the original observations that eventually let to the team’s discovery of infrared excess around HD 131488), the NASA Infrared Telescope Facility (IRTF), and the Keck II telescope and optical observations from the Keck I telescope, the Siding Spring Observatory (SSO) 2.3-meter telescope, and the Tycho space-based imager/astrometer that flew aboard the ESA Hipparcos mission.
In addition to Melis and Zuckerman, co-authors include Inseok Song, a professor in the University of Georgia's Department of Physics and Astronomy; Joseph Rhee, a UCLA postdoctoral scholar in astronomy; M.S. Bessell of the Australian National University's Research School of Astronomy and Astrophysics; and Simon Murphy a graduate student at the Australian National University's Research School of Astronomy and Astrophysics.
Contacts:
Carl Melis
University of California San Diego
(858) 449-0437 (Cell)
Peter Michaud
Gemini Observatory, Hilo Hawai‘i
(808) 936-6643 (Cell)
The Gemini Observatory is an international collaboration with two identical 8-meter telescopes. The Frederick C. Gillett Gemini Telescope is located at Mauna Kea, Hawai'i (Gemini North) and the other telescope at Cerro Pachón in central Chile (Gemini South), and hence provide full coverage of both hemispheres of the sky. Both telescopes incorporate new technologies that allow large, relatively thin mirrors under active control to collect and focus both optical and infrared radiation from space.
The Gemini Observatory provides the astronomical communities in each partner country with state-of-the-art astronomical facilities that allocate observing time in proportion to each country's contribution. In addition to financial support, each country also contributes significant scientific and technical resources. The national research agencies that form the Gemini partnership include: the US National Science Foundation (NSF), the UK Science and Technology Facilities Council (STFC), the Canadian National Research Council (NRC), the Chilean Comisión Nacional de Investigación Cientifica y Tecnológica (CONICYT), the Australian Research Council (ARC), the Argentinean Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET) and the Brazilian Conselho Nacional de Desenvolvimento Científico e Tecnológico CNPq).
