Forty-four planets in solar systems beyond our own have been unveiled in one go, dwarfing the usual number of confirmations from extrasolar surveys, which is typically a dozen or less. The findings will improve our models of solar systems and may help researchers investigate exoplanet atmospheres. Novel techniques developed to validate the find could hugely accelerate the confirmation of more extrasolar planet candidates.

An international team of astronomers pooled data from U.S. space agency NASA’s Kepler and the European Space Agency (ESA)’s Gaia space telescopes, as well as ground-based telescopes in the U.S. Alongside John Livingston, lead author of the study and a graduate student at the University of Tokyo, the team’s combined resources led to the confirmed existence of these 44 exoplanets and described various details about them.

A portion of the findings yield some surprising characteristics: “For example, four of the planets orbit their host stars in less than 24 hours,” says Livingston. “In other words, a year on each of those planets is shorter than a day here on Earth.” These contribute to a small but growing list of “ultrashort-period” planets, so it could turn out they’re not as unusual as they might seem.

“It was also gratifying to verify so many small planets,” continues Livingston. “Sixteen were in the same size class as Earth, one in particular turning out to be extremely small — about the size of Venus — which was a nice affirmation as it’s close to the limit of what is possible to detect.”

The source observations for this study were made by Kepler, and they would not have happened were it not for a fault in 2013, which prevented accurate control of the space telescope. “Two out of the four control-reaction wheels failed, which meant Kepler couldn’t perform its original mission to stare at one specific patch of the sky,” explains Professor Motohide Tamura of the University of Tokyo. “This led to its contingent mission, ‘K2’ — our observations came from campaign 10 of this mission. We’re lucky Kepler continues to function as well as it does.”



The 44 confirmed planets and their approximate size class, orbits and surface temperatures. Credit: John Livingston University Of Tokyo

The planets observed by K2 are known as transiting planets because their orbits bring them in front of their host stars, slightly reducing their brightness. However, other astrophysical phenomena can cause similar signals, so follow-up observations and detailed statistical analyses were performed to confirm the planetary nature of these signals. As part of his doctoral work, Livingston traveled to Kitt Peak observatory in the U.S. state of Arizona to obtain data from a special type of camera, known as a speckle interferometer installed on a large telescope there. These observations, along with follow-up observations from a telescope in the state of Texas, were necessary to characterize the host stars and rule out false positives. The combination of detailed analyses of data from these ground-based telescopes, K2 and Gaia enabled the precise determination of the planets’ sizes and temperatures. The team’s findings include 27 additional candidates that are likely to be real planets, which will be the subject of future research.

Scientists hope to understand what kinds of planets might be out there, but can only draw valid conclusions if there are enough planets for robust statistical analysis. The addition of a large number of new planets, therefore, leads directly to a better theoretical understanding of solar-system formation. The planets also provide good targets for detailed individual studies to yield measurements of planetary composition, interior structure and atmospheres — in particular, the 18 planets in several multiplanet systems. “The investigation of other solar systems can help us understand how planets and even our own solar system formed,” says Livingston. “The study of other worlds has much to teach us about our own.”

Publication: John H. Livingston, et al., “44 Validated Planets from K2 Campaign 10,” AJ, 2018; doi:10.3847/1538-3881/aaccde