U.S. National Science Foundation-supported researchers published a new paper that explains how atmospheric wind affects eddies, an ocean weather phenomena of spinning ocean currents. “Our theory and findings provide a roadmap for incorporating interactions between winds and ocean eddies into operational and long-term forecasting,” said Hussein Aluie, a co-author on the paper and professor at the University of Rochester.

“Accurate ocean forecasts are essential for navigation and shipping, fisheries management, disaster response, coastal management and climate prediction,” Aluie said. These economic sectors rely on accurate forecasts to plan for potentially dangerous conditions.

Aluie and a team of researchers used satellite imagery and climate models to discover that not only do atmospheric winds dampen eddies, like previously thought, but they can also energize them. Prevailing winds that move longitudinally across the globe, like westerlies and trade winds, slow eddies when they move in the opposite direction but energize them if they spin the same way.

Between the eddies are ocean weather phenomenon called strain, which account for about half of the ocean’s kinetic energy. The team found that strain is also dampened or energized by wind-like eddies.

“The new energy pathways between the atmosphere and the ocean that we discovered can help design better ocean observation systems and improve climate models,” said Shikhar Rai, the study’s first author and a doctoral student at the University of Rochester,

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A research team led by the recipient of a U.S. National Science Foundation Faculty Early Career Development grant used computer simulations to determine that white dwarf stars have greater potential to host habitable planets than previously realized. The team concluded that many more stars in the Milky Way galaxy might be home to planets that could support life.

There are approximately 10 billion white dwarf stars in the Milky Way. Because such stars are colder than others, scientists have thought they likely would not support habitable exoplanets. Led by Aomawa Shields, a University of California, Irvine professor of physics and astronomy, researchers used a supercomputer provided by the NSF National Center for Atmospheric Research in Boulder, Colorado, to simulate conditions on a theoretical rocky planet orbiting a white dwarf. Using data from real exoplanets orbiting the non-white dwarf star Kepler-62, the researchers found that their simulated rocky planet could have liquid water if it closely orbited a white dwarf and had certain rotational characteristics. Their findings were published in The Astrophysical Journal.

“Not much consideration has been given to these stars’ ability to host habitable exoplanets,” says Shields. “Our computer simulations suggest that if rocky planets exist in their orbits, these planets could have more habitable real estate on their surfaces than previously thought.”