A new study led by NASA with contributions from the University of Maryland reveals that the distant planet HAT-P-26b has a primitive atmosphere composed almost entirely of hydrogen and helium. Located about 437 light years away from Earth, HAT-P-26b orbits a star roughly twice as old as the sun. The analysis is one of the most detailed studies to date of a "warm Neptune," a planet that is Neptune-sized and orbits close to its star.
By combining observations from NASA's Hubble and Spitzer space telescopes, the researchers determined that HAT-P-26b's atmosphere is relatively clear of clouds and has a strong water signature, although the planet is not a water world. The study, published in the May 12, 2017 issue of the journal Science, also provides the best measurement to date of water on an exoplanet of this size.
"Not too long ago, it was exciting just to find an exoplanet," said Drake Deming, a professor of astronomy at UMD and a co-author of the study. "But now, as technology and methods become more refined, we are building a whole new understanding of the wide diversity of planetary systems beyond our own. It's a very exciting time to be in this field."
The discovery of such a primordial atmosphere on this Neptune-sized planet has implications for how scientists think about the birth and development of planetary systems. Compared to Neptune and Uranus, the planets in our solar system with about the same mass, HAT-P-26b likely formed either closer to its host star or later in the development of its planetary system--or a combination of both.
"Astronomers have just begun to investigate the atmospheres of these distant Neptune-mass planets, and almost right away, we found an example that goes against the trend in our solar system," said Hannah Wakeford, a postdoctoral researcher at NASA's Goddard Space Flight Center in Greenbelt, Maryland, and lead author of the study. "This kind of unexpected result is why I really love exploring the atmospheres of alien planets."
To study HAT-P-26b's atmosphere, the researchers used data from transits-- occasions when the planet passed in front of its host star. During a transit, a fraction of the starlight gets filtered through the planet's atmosphere, which absorbs some wavelengths of light but not others. By looking at how the signatures of the starlight change as a result of this filtering, researchers can work backward to figure out the chemical composition of the atmosphere.
In this case, the team pooled data from four transits measured by Hubble and two seen by Spitzer. Together, these observations covered a wide range of wavelengths from yellow light through the near-infrared region.
"To have so much information about a warm Neptune is still rare, so analyzing these data sets simultaneously is an achievement in and of itself," said co-author Tiffany Kataria of the Jet Propulsion Laboratory in Pasadena, California.
Because the study provided a precise measurement of water, the researchers were able to use the water signature to estimate HAT-P-26b's metallicity--an indication of how rich the planet is in all elements heavier than hydrogen and helium. Astronomers calculate metallicity to provide clues about how a planet formed.
To compare planets by their metallicities, scientists use the sun as a point of reference--almost like describing how much caffeine a beverage has by comparing it to a cup of coffee. Jupiter has a metallicity about 2 to 5 times that of the sun. For Saturn, it's about 10 times as much as the sun. These relatively low values mean that the two gas giants are made almost entirely of hydrogen and helium.
The ice giants Neptune and Uranus are smaller than the gas giants but richer in the heavier elements, with metallicities of about 100 times that of the sun. So, for the four outer planets in our solar system, the trend is that the metallicities are lower for the bigger planets.
Scientists think this happened because, as the solar system was taking shape, Neptune and Uranus formed in a region toward the outskirts of the enormous disk of dust, gas and debris that swirled around the immature sun. Summing up the complicated process of planetary formation in a nutshell: Neptune and Uranus would have been bombarded with a lot of icy debris that was rich in heavier elements. Jupiter and Saturn, which formed in a warmer part of the disk, would have encountered less of the icy debris.
Two planets beyond our solar system also fit this trend. One is the Neptune-mass planet HAT-P-11b. The other is WASP-43b, a gas giant twice as massive as Jupiter.
But Wakeford and her colleagues found that HAT-P-26b bucks the trend. They determined its metallicity is only about 4.8 times that of the sun, much closer to the value for Jupiter than for Neptune.
"This analysis shows that there is a lot more diversity in the atmospheres of these exoplanets than we were expecting, which is providing insight into how planets can form and evolve differently than in our solar system," said David K. Sing of the University of Exeter and the second author of the paper. "I would say that has been a theme in the studies of exoplanets: Researchers keep finding surprising diversity."
The research paper, "HAT-P-26b: A Neptune-mass Exoplanet with a Well-constrained Heavy Element Abundance," Hannah Wakeford, David Sing, Tiffany Kataria, Drake Deming, Nikolay Nikolov, Eric Lopez, Pascal Tremblin, David Amundsen, Nikole Lewis, Avi Mandell, Jonathan Fortney, Heather Knutson, Björn Benneke and Tom Evans, was published May 12, 2017 in the journal Science.
This work was supported by the European Space Agency, NASA (Award Nos. NAS 5-26555 and HST-GO-14260) and the European Research Council (Award Nos. 336792, 313014, and 247060-PEPS). The content of this article does not necessarily reflect the views of these organizations.
This release is adapted from text provided by NASA's Goddard Space Flight Center.
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