This false-color satellite image of Malaspina Glacier (Sít’ Tlein) is a riot of color. Composed of coastal/aerosol, near infrared, and shortwave infrared bands from Landsat 9, the colors highlight features otherwise hard to identify. Watery features appear in reds, oranges, and yellows; vegetation is green and rock appears in blue. The glacier covers more than 4000 square kilometers, an area larger than the state of Rhode Island. The dark lines atop the glacier are moraines, where rock, soil, and other debris has been scraped up along the glacier’s edge. Over time, changes in the glacier’s velocity cause the moraines to fold and shear, creating the zigzag pattern seen here. (Image credit: W. Liang; via NASA Earth Observatory)
Tag: planetary science
Exoplanet Heating
WASP-96B is a tidally-locked exoplanet between the size of Saturn and Jupiter. This hot, massive planet lies close to its star, orbiting in less than three-and-a-half Earth days. A recent study shows that planets like these can have very different weather, depending on what depth their atmosphere absorbs heat at.
Using numerical simulations, researchers took a detailed look at the possible atmospheric dynamics on this planet. When the atmosphere absorbed heat at a shallow depth — near the outer layers of the planet — a coupled vortex pair formed (left, below). These vortices promenaded westward and completed a circuit around the planet every 11-15 days.
Shallow heating on a hot Jupiter produces a pair of coupled vortices (left), but deeper heating in the atmosphere generates four more-chaotic vortices (right). In contrast, deeper heating produced a more-chaotic pattern of four vortices (right, above) that each lasted 3 to 15 days before disappearing, replaced by a new vortex. This atmosphere, they found, was very turbulent, with smaller-scale vortices as well.
Since each weather pattern is visually distinct and carries its own brightness signature, the authors predict that additional observations of WASP-96b with the current generation of telescopes will show which type of heating dominates on the exoplanet. (Image and research credit: J. Skinner et al.; via APS Physics)
Snapshots from a simulation of a deep-heated hot Jupiter. Each image shows the planet on a different consecutive day. 
Dust Storms
Hot, dry berg winds swept down from the Namibian highlands and sent these plumes of dust flying out to the Atlantic coast. Another plume — white instead of brown — marks salt dust from the Etosha Pan salt flat. The dust and salt become aerosol particles in the atmosphere — seeds for raindrops to form. Coastal towns sometimes need construction equipment to deal with the drifting sand from these storms, but these storms are small compared to Saharan dust storms. Those storms are so large that their dust influences the weather on the other side of the Atlantic. (Image credit: W. Liang; via NASA Earth Observatory)
Field of Dunes
Barchan dunes collide in this astronaut image of Brazil’s southern coastline. Barchan (pronounced “bar-kahn”) dunes are crescent-shaped; their tips point downwind into their direction of travel. When many barchan dunes overlap, they coalesce into a dune field like the one seen here. A dune’s speed depends on many factors, including the wind speed, dune size, and its proximity to other dunes. In experiments, dunes have even chased one another and changed speeds to avoid collision. (Image credit: NASA; via NASA Earth Observatory)
Changing Climes on Mars
China’s Zhurong rover explored Utopia Planitia on Mars from May 2021 to December 2022. During that expedition, the rover uncovered evidence of a major shift in climate that took place some 400,000 years ago. Originally, the area was covered in crescent-shaped barchan dunes formed by winds from the northeast. But after Mars exited its last ice age — courtesy of a shift in its rotational axis — the winds shifted around 70 degrees, coming from the northwest. Those shifted winds eroded the barchan dunes and caused new transverse ridges to form atop them. (Image credit: NASA/JPL-Caltech/UArizona; research credit: J. Liu et al.; via Gizmodo)
Uranus’s Polar Cyclone
Uranus is an oddity among the planets of our solar system. Where other planets spin around an axis roughly in line with their orbital axis, Uranus spins on its side, placing its poles in line with the sun. On Earth, the polar regions are naturally colder the equator, but that doesn’t hold true for Uranus. Yet new observations of the ice giant show that it, like the other planets with atmospheres in our solar system, has a polar cyclone.
Those observations are thanks to improvements in radio astronomy over the past couple decades. Uranus’s odd orbital geometry means that each of its poles are hidden from Earth for 42 years at a time; the current northern-hemisphere spring marks our first view of Uranus’s northern pole since 1965. In the recent observations, researchers saw a bright spot on the pole, surrounded by a faint darker ring. The team modeled the temperature and gas composition necessary to match their observations and found that those patterns were consistent with a cyclone sitting at the northern pole. (Image credit: NASA/JPL-Caltech/VLA; research credit: A. Akins et al.; via Physics Today)
Jovian Swirls
Jupiter, our solar system’s stormiest planet, shares many similarities with Earth. But where Earth’s strongest storms are cyclones centered on low-pressure regions, Jupiter’s longest and strongest storms are anti-cyclones, driven by areas of high pressure. They’re often massive — larger than the entire Earth — and persist for weeks, months, or years. This processed image comes from the JunoCam instrument and shows some of the incredible cloud structure in Jupiter’s atmosphere. Jupiter’s highest altitude clouds tend to be the lightest, while darker clouds remain lower. (Image credit: NASA/JPL-Caltech/SwRI/MSSS/K. Gill; via APOD)
Fast-Moving Martian Rivers
For the first time, scientists have found evidence of deep, fast-flowing ancient rivers on Mars. After examining images taken recently by the Perseverance rover in Jezero Crater, fluvial experts have spotted familiar signs of turbulent river flow. The mosaic above shows an area nicknamed “Shrinkle Haven,” where curved bands of rock mark the landscape. Although scientists are confident that a powerful river deposited these rocks, they’re still debating whether that river was a meandering one like the Mississippi or a braided river like the Platte.
Nicknamed “Pinestand,” this hill’s sedimentary layers were likely formed by a deep, fast-moving river. In another area, known as “Pinestand,” scientists spotted hills as high as 20 meters tall with clear sedimentary layers. Like Shrinkle Haven’s rock bands, formations like this are most often associated with a large, fast-flowing river. (Image credits: NASA/JPL-Caltech/ASU/MSSS; via Gizmodo; see also NASA JPL)
“Elements”
Photographer Mikko Lagerstedt specializes in Nordic landscapes, like the windswept snow seen here. I love the way he’s captured the snow that gets picked up and blown by the wind. Notice the hazy layer of snow hovering over the foreground. This snow is saltating, just as sand does in the desert. When flakes get picked up by the wind, they follow a ballistic trajectory, much like a cannonball in a high-school physics class. As the snow crashes back down, its impact knocks up more flakes, and the process continues. Repeat enough times, and you’ll see this hazy layer of blowing snow blanketing a snowscape. (Image credit: M. Lagerstedt; via Colossal)
Founts of Enceladus
In its exploration of Saturn, Cassini discovered that the moon Enceladus is home to icy eruptions. Beneath its shell of ice, Enceladus has a global ocean of salty liquid water. The average thickness of the ice is 20 kilometers, putting the ocean seemingly out of reach — except at the moon’s southern pole, where icy plumes of ocean water jet out.
Here, where the ice is thinnest, the tidal forces Enceladus experiences from Saturn and its fellow moon Dione break through the ice. As the cracks open and close, liquid from the ocean sprays out, freezing into plumes that Cassini measured. Plans are underway for new missions that prioritize further sampling of Enceladus’ ocean. For now, we can only imagine what hides in its interior ocean. (Image credit: NASA/JPL-Caltech/SSI; for more, see M. Manga and M. Rudolph)
