FYFD

Tag: planetary science

  • Stabilizing Jupiter’s Polar Storms

    Stabilizing Jupiter’s Polar Storms

    Four years ago, Juno discovered an octagon of eight cyclones at Jupiter’s northern pole and a similar five cyclone structure at its southern pole. Since then, both polygons have remained intact. What keeps the storm systems so stable is still an open question, but a recent observational study using Juno measurements found that an anticyclonic ring sits between the central and outer cyclones. In line with a previous theoretical study, this ring structure helps shield and stabilize the storm system.

    The underlying convective mechanisms of the storm remain a mystery, though, as the current study is limited in resolution to a scale of about 200 kilometers. (Image credit: NASA/JPL-Caltech/SwRI/ASI/INAF/JIRAM; research credit: A. Ingersoll et al.; via Gizmodo)

  • Martian Glaciers

    Martian Glaciers

    On Earth, glaciers slide on lubricating layers of water, leaving complex landscapes like fjords and drumlins in their wake. Mars — though once home to enormous ice masses — lacks those geological features. Scientists assumed, therefore, that Martian ice stayed frozen and unmoving. But a new study demonstrates that is not the case.

    Researchers used computational modeling to simulate two identical glaciers: one under Earth-like conditions and one under the lower gravity of Mars. They found that Martian glaciers did indeed move, but Mars’s lower gravity, combined with better water drainage beneath the ice, meant that they moved exceedingly slowly. Martian glaciers did erode the landscape but into different features than on Earth. Instead of forming moraines and drumlins, a large Martian glacier would instead carve channels and eskar ridges, geological features found on Mars today. (Image credit: NASA/JPL-CalTech/Uni. of Arizona; research credit: A. Grau Galofre et al.; via AGU; submitted by Kam-Yung Soh)

  • Jupiter’s Frosted Clouds

    Jupiter’s Frosted Clouds

    This 3D rendering of Jupiter's cloud tops is based on flyby data from the JunoCam instrument. It's not a true physical image of the cloud tops, though scientists are working on a calibration for that. Instead, the elevations shown here are based on the intensity of visible light registered by the instrument. This measure correlates with cloud height, but there are exceptions.
    This 3D rendering of Jupiter’s cloud tops is based on flyby data from the JunoCam instrument. It’s not a true physical image of the cloud tops, though scientists are working on a calibration for that. Instead, the elevations shown here are based on the intensity of visible light registered by the instrument. This measure correlates with cloud height, but there are exceptions.

    New 3D renderings of Jovian clouds show textured swirls akin to a cupcake’s sculpted frosting. The images are based on flyby data from the JunoCam instrument. Because illumination of the clouds is generally brightest for the highest clouds, the team has rendered elevation based on brightest. While this is somewhat physical, it’s not exactly what Jupiter looks like. For that, Juno scientists are working on a calibration that will translate these initial renderings into a truer physical model. Nevertheless, the results are stunning, especially the flyover video embedded over here! (Image credit: 3D renders – NASA / JPL-Caltech / SwRI / MSSS / G. Eichstädt, image pair – G. Eichstädt et al.; via phys.org; submitted by Kam-Yung Soh)

    Cross your eyes to see this image pair as a 3D image of Jupiter's cloud tops.
    Cross your eyes to see this image pair as a 3D image of Jupiter’s cloud tops. The brighter regions will appear closer than the darker ones.
  • Predicting Alien Ice

    Predicting Alien Ice

    Europa is an ocean world trapped beneath an ice shell tens of kilometers thick. To better understand what we might find in those oceans, researchers turn to analogs here on Earth, looking at Antarctica’s ice shelves. Beneath those shelves, ice forms via two mechanisms: the first, congelation ice, freezes directly onto the existing ice-water interface. The second, frazil ice, forms crystals in supercooled water columns, which drift upward in buoyant currents and settle on the ice shelf like upside-down snow (pictured above).

    Based on Europa’s conditions, the researchers conclude that congelation ice would gradually thicken the ice shell as the moon’s interior cools. But in areas where the shell is thinned by local rifts and Jovian tidal forces, frazil ice is likely to form. (Image credit: H. Glazer; research credit: N. Wolfenbarger et al.; via Physics World)

  • Neptune’s Seasonal Changes

    Neptune’s Seasonal Changes

    Ice giant Neptune orbits our sun once every 165 years, meaning that each season on the planet lasts about 41 years here on Earth. Currently, the side of Neptune facing us is entering early summer, but a recent survey of atmospheric measurements show that Neptune’s stratosphere is experiencing some unexpected changes. Between 2003 and 2018, the team found that global stratospheric temperatures actually decreased by 8 degrees Celsius. Even more dramatically, Neptune’s southern pole warmed by a full 11 degrees Celsius between 2018 and 2020. Both results hint that atmospheric patterns on the planet may be far more complex than current models assume. (Image credit: NASA/JPL; research credit: M. Roman et al.; via Physics World)

  • Extreme Weather

    Extreme Weather

    Many of the exoplanets we’ve observed so far are extreme environments. WASP-121b is known as a hot Jupiter, a gas giant so close to its star that it orbits in just 30 hours. The exoplanet is tidally-locked to its star, meaning that one side always faces toward the star and the other faces away. This constant sunlight makes the daytime side of the planet hot enough to vaporize metals. A recent study combined observations of the exoplanet with numerical simulations to model both the daytime and nighttime atmosphere of the exoplanet. The results are pretty wild. The authors found evidence of 18,000 km/h winds that blow hot gases from the dayside to the nightside, where temperatures cool enough for some metals — primarily corundum — to rain out of the atmosphere. Given the trace amounts of other elements available in the atmosphere, the authors posit that the nightside of the planet may have rainfall of liquid rubies and sapphires. (Image credit: NASA/ESA; research credit: T. Mikal-Evans et al.; via Physics World)

  • Featured Video Play Icon

    Martian Flyover

    Fly over a Martian crater in this incredibly detailed 8K video built from Mars Reconnaissance Orbiter imagery. Like Earth’s deserts, Mars is largely shaped by wind, and we get some fantastic views of sand ripples in this flyover. For reference, the vertical scale covered in the video image is roughly 1 kilometer. It’s pretty astounding to see this kind of detail from a spacecraft 250 kilometers away! (Video and image credit: S. Doran/NASA; via Colossal)

  • Inside a Super-Earth

    Inside a Super-Earth

    When studying exoplanets, scientists often judge habitability by the possibility of liquid water on the planet’s surface. But there is more to Earth’s habitability than water. The liquid iron dynamo within our planet is critical for life here because it generates magnetic fields that protect the planet from harmful solar radiation. It’s been difficult to predict what the interiors of a bigger and more massive planet like a super-Earth would look like, but a recent study changes that.

    Researchers at the National Ignition Facility used its high-powered lasers to subject liquid iron to conditions similar to those expected in a super-Earth’s core, including pressures as high as ~1000 GPa. That’s more than 3 times higher than pressures at the boundary where Earth’s liquid iron meets its solid core. Based on their findings, the team concluded that super-Earths likely have a similar interior structure to our planet, with a solid iron-heavy core surrounded by churning liquid iron capable of generating a protective magnetosphere. (Image credit: NASA; research credit: R. Kraus et al.; via Science)

  • Jovian Circulation

    Jovian Circulation

    Jupiter‘s atmosphere remains quite mysterious, due to our limited ability to measure the depths of the gas giant’s clouds. But measurements from the Juno spacecraft are continuing to shape researchers’ understanding of our massive neighbor. By tracking ammonia distributions in Jupiter’s belts and zones, a team has found a series of circulation cells similar to the Ferrel cells of Earth’s midlatitudes.

    Unlike the stronger Hadley cells and polar cells, Earth’s Ferrel cells are relatively weak. They’re driven by turbulence and the motion of the circulation cells to the north and south. The Northern and Southern hemispheres each have one Ferrel cell. In contrast, Jupiter — with its larger size and higher rotation rate — boasts eight Ferrel-like cells in each hemisphere! (Image and research credit: K. Duer et al.; via Universe Today; submitted by Kam-Yung Soh)

  • Probing Saturn’s Interior

    Probing Saturn’s Interior

    Saturn’s rings are one of the most iconic sights in our solar system, and scientists are using them to learn more about the planet they surround. Until recently, scientists believed that gas giants like Saturn and Jupiter have dense, rocky cores buried beneath their gassy atmospheres. But a new study of Saturn’s rings suggests that Saturn’s core is far larger and more fluid than assumed.

    When the interior of Saturn wobbles, it causes gravitational shifts that affect the material making up its rings. By studying disturbances in the ring system — a technique known as ring seismology — researchers can deduce what motions took place inside the planet to cause the changes in the rings.

    Using data from the Cassini spacecraft, the authors determined that Saturn’s core likely spreads to nearly 60% of its radius, and, rather than being dense and rocky, the core is a relatively fluid mixture of ice, rock, and metallic fluids. The core diffuses gradually into the gaseous atmosphere, and it’s stably stratified against convection, so its wobbles are quite small for the planet’s size. (Image credit: rings – NASA; illustration – Caltech/R. Hurt; research credit: C. Mankovich and J. Fuller; via Gizmodo)

    Illustration of Saturn's interior showing a large, wobbly core composed of a mixture of ice, rock and metallic fluid.