Astronomers using the Gemini North telescope, one half of the International Gemini Observatory operated by NSF’s NOIRLab, have made multiple detections of rock-forming elements in the atmosphere of a Jupiter-sized exoplanet, WASP-76b. The so-called “hot Jupiter” is perilously close to its host star, which is heating the planet’s atmosphere to astounding temperatures and vaporized rock-forming elements such as magnesium, calcium and iron, providing insight into how our own Solar System formed.Credit: International Gemini Observatory/NOIRLab/NSF/AURA/J. da Silva/Spaceengine/M. Zamani. download: Large JPEG
Chemistry of so-called ‘hot Jupiter’ provides new insights into the formation of our Solar System
Astronomers using the Gemini North telescope, one half of the International Gemini Observatory operated by NSF’s NOIRLab, have detected multiple rock-forming elements in the atmosphere of a Jupiter-sized exoplanet, WASP-76b. The planet is so perilously close to its host star that rock-forming elements — such as magnesium, calcium, and nickel — become vaporized and dispersed throughout its scorching atmosphere. This intriguing chemical profile provides new insights into the formation of planetary systems, including our own.
WASP-76b is a strange world. Located 634 light-years from Earth in the direction of the constellation of Pisces, the Jupiter-like exoplanet orbits its host star at an exceptionally close distance — approximately 12 times closer than Mercury is to the Sun — which heats its atmosphere to a searing 2000°C. Such extreme temperatures have “puffed up” the planet, increasing its volume to nearly six times that of Jupiter.
At such extreme temperatures, mineral- and rock-forming elements, which would otherwise remain hidden in the atmosphere of a colder gas-giant planet, can reveal themselves.
Using the Gemini North telescope, one half of the International Gemini Observatory operated by NSF’s NOIRLab, an international team of astronomers has detected 11 of these rock-forming elements in the atmosphere of WASP-76b. The presence and relative amounts of these elements can provide key insights into exactly how giant gas planets form — something that remains uncertain even in our own Solar System. The results are published in the journal Nature.
Since its discovery in 2013 during the Wide Angle Search for Planets (WASP) program, many astronomers have studied the enigmatic WASP-76b. These studies have led to the identification of various elements present in the hot exoplanet’s atmosphere. Notably, in a study published in March 2020, a team concluded that there could be iron rain on the planet.
Aware of these existing studies, Stefan Pelletier, a PhD student with the Trottier Institute for Research on Exoplanets at the Université de Montréal and lead author on the paper, was inspired to explore the mysteries of this strange exoplanet and the chemistry of its searing atmosphere.
In 2020 and 2021, using Gemini North’s MAROON-X (a new instrument specially designed to detect and study exoplanets), Pelletier and his team observed the planet as it passed in front of its host star on three separate occasions. These new observations uncovered a number of rock-forming elements in the atmosphere of WASP-76b, including sodium, potassium, lithium, nickel, manganese, chromium, magnesium, vanadium, barium, calcium, and, as previously detected, iron.
Due to the extreme temperatures of WASP-76b’s atmosphere, the elements detected by the researchers, which would normally form rocks here on Earth, are instead vaporized and thus present in the atmosphere in their gaseous forms. While these elements contribute to the composition of gas giants in our Solar System, those planets are too cold for the elements to vaporize into the atmosphere making them virtually undetectable.
“Truly rare are the times when an exoplanet hundreds of light-years away can teach us something that would otherwise likely be impossible to know about our own Solar System,” said Pelletier. “That is the case with this study.”
The abundance of many of these elements closely match the abundances found in both our Sun and the exoplanet’s host star. This may be no coincidence and provides additional evidence that gas-giant planets, like Jupiter and Saturn, form in a manner more akin to star formation — coalescing out of the gas and dust of a protoplanetary disk — rather than the gradual accretion and collision of dust, rocks, and planetesimals, which go on to form rocky planets, like Mercury, Venus, and Earth.
Another notable result of the study is the first-ever unambiguous detection of vanadium oxide (V2O5) on an exoplanet. “This molecule is of high interest to astronomers because it can have a great impact on the atmospheric structure of hot giant planets,” says Pelletier. “This molecule plays a similar role to ozone being extremely efficient at heating Earth’s upper atmosphere.”
Pelletier and his team are motivated to learn more about WASP-76b and other ultra-hot planets. They also hope other researchers will leverage what they learned from this giant exoplanet and apply it to better our understanding of our own Solar System planets and how they came to be.
“Available to astronomers across the globe, the International Gemini Observatory continues to deliver new insights that push our understanding of the physical and chemical structure of other worlds. Through such observational programs we are developing a clearer picture of the wider universe and our own place in it,” said NSF Gemini Observatory program director Martin Still.
“Generations of researchers have used Jupiter, Saturn, Uranus, and Neptune measured abundances for hydrogen and helium to benchmark formation theories of gaseous planets,” says Université de Montréal professor Björn Benneke, a co-author on the study. “Likewise, the measurements of heavier elements such as calcium or magnesium on WASP-76b will help further understanding the formation of gaseous planets.”
Notes
NSF’s NOIRLab, the US center for ground-based optical-infrared astronomy, operates the International Gemini Observatory (a facility of NSF, NRC–Canada, ANID–Chile, MCTIC–Brazil, MINCyT–Argentina, and KASI–Republic of Korea), Kitt Peak National Observatory (KPNO), Cerro Tololo Inter-American Observatory (CTIO), the Community Science and Data Center (CSDC), and Vera C. Rubin Observatory (operated in cooperation with the Department of Energy’s SLAC National Accelerator Laboratory). It is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with NSF and is headquartered in Tucson, Arizona. The astronomical community is honored to have the opportunity to conduct astronomical research on Iolkam Du’ag (Kitt Peak) in Arizona, on Maunakea in Hawai‘i, and on Cerro Tololo and Cerro Pachón in Chile. We recognize and acknowledge the very significant cultural role and reverence that these sites have to the Tohono O’odham Nation, to the Native Hawaiian community, and to the local communities in Chile, respectively.
Links
Contacts:
Stefan Pelletier
Université de Montréal, Montréal, Canada
Email:stefan.pelletier@umontreal.ca
Charles Blue
Public Information Officer
NSF’s NOIRLab
Tel: +1 202 236 6324
Email:charles.blue@noirlab.edu
Josie Fenske
NSF’s NOIRLab
Email: josie.fenske@noirlab.edu
