{"id":828044,"date":"2026-07-26T22:59:08","date_gmt":"2026-07-26T22:59:08","guid":{"rendered":"https:\/\/www.newsbeep.com\/ca\/828044\/"},"modified":"2026-07-26T22:59:08","modified_gmt":"2026-07-26T22:59:08","slug":"new-findings-complicate-the-search-for-life-beneath-europas-ice","status":"publish","type":"post","link":"https:\/\/www.newsbeep.com\/ca\/828044\/","title":{"rendered":"New findings complicate the search for life beneath Europa\u2019s ice"},"content":{"rendered":"

Water trying to rise from Europa\u2019s ocean<\/a> would likely cool quickly and begin freezing inside cracks.Tiny ice crystals could build into slush and clog those pathways within hours.Shallow water, if detected, may have melted locally instead of coming from the deep ocean.<\/p>\n

Europa\u2019s buried ocean may be one of the solar system\u2019s most promising places to search for habitable conditions. Yet the icy moon\u2019s surface may be far less connected to that ocean than scientists once hoped.<\/p>\n

A Rutgers-led study in Nature Astronomy<\/a> examined whether liquid water can rise from Europa\u2019s deep ocean through cracks in the ice. The simulations suggest that water may cool, form ice crystals and clog its route before reaching shallow depths.<\/p>\n

Europa\u2019s surface features and conceptual model schematics. (CREDIT: Lujendra Ojha et al, Nature Astronomy) A frozen barrier above a restless ocean<\/p>\n

Europa\u2019s global ocean may stay liquid because Jupiter\u2019s gravity repeatedly squeezes and stretches the moon. That motion generates heat beneath the frozen exterior.<\/p>\n

Scientists have proposed that water could move upward through narrow fractures called dykes. On Earth, similar cracks carry molten rock toward the surface. On Europa, the process would involve water and ice instead of magma and stone.<\/p>\n

Those fractures could feed shallow reservoirs called sills. Such pockets would be easier for spacecraft to detect than the ocean below. They also may help form lenticulae, double ridges, chaos terrain, domes and pits.<\/p>\n

\u201cIce and liquid water are fundamentally different than lava and the volcanoes<\/a> that we see here on Earth,\u201d Ojha said. \u201cI think there\u2019s some fundamental physics that\u2019s missing here, and so I wanted to explore that.\u201d<\/p>\n

The team used COMSOL Multiphysics simulations combining fluid flow and heat transfer. The models tested how pure and salty water would behave in cold sections of Europa\u2019s shell.<\/p>\n

Box plot showing the estimated volume of liquid water (log10\u2009m3) required to account for the formation of various surface features on Europa. The red boxes represent estimates assuming elastic support of the overlying ice shell, whereas the blue boxes correspond to estimates under near-isostatic compensation conditions. (CREDIT: Lujendra Ojha et al, Nature Astronomy) Turbulence changes the journey<\/p>\n

Earlier models often treated the flow as orderly. The new analysis found that water would likely move turbulently at about 5 to 20 meters per second.<\/p>\n

That swirling motion pushes warmer water against frozen walls. Heat then escapes quickly into the surrounding ice.<\/p>\n

\u201cThis water that\u2019s going to come up, it\u2019s going to be turbulent,\u201d Ojha said. \u201cIt\u2019s going to be left and right, it\u2019s going to be up and down, it\u2019s going to have a swirling motion. And when that happens, that liquid water<\/a> is going to cool very, very fast as it approaches the surface.\u201d<\/p>\n

The researchers modeled the upper 1 to 2 kilometers of a possible fracture. Surrounding ice there could be about 140 to 200 kelvins, or roughly minus 208 to minus 100 degrees Fahrenheit.<\/p>\n

Even without turbulence, narrow fractures closed quickly. A dyke 0.1 meter wide could freeze shut within two to six hours. Delivering 1 billion cubic meters of water would require a crack about 77 kilometers long under favorable conditions.<\/p>\n

At colder conditions, one fracture would need to stretch more than 200 kilometers. A realistic one-kilometer crack would require roughly 200 to 800 parallel dykes. Supplying 10 billion cubic meters could require thousands.<\/p>\n

Dynamical and thermal constraints on ascent of liquid water on Europa\u2019s dykes. (CREDIT: Lujendra Ojha et al, Nature Astronomy) Wider cracks still face freezing<\/p>\n

A one-meter-wide fracture seemed more promising under conduction-only modeling, remaining open for one week to 23 days. That advantage weakened once turbulence entered the calculation.<\/p>\n

As water loses heat, it can become supercooled, meaning it remains liquid below its normal freezing point.<\/p>\n

In the simulations, water crossing a one-kilometer section cooled by about 1 to 2 kelvins. Longer fractures could allow more cooling.<\/p>\n

Supercooled water can produce frazil ice, small crystals<\/a> that form in turbulent water. The process requires seed crystals, but only a tiny amount may be needed.<\/p>\n

Fragments could come from the walls as a crack opens or as turbulent water scrapes against the ice. A wall-ice layer between 0.13 and 19 micrometers thick could trigger rapid frazil growth.<\/p>\n

Ice crystals can choke the flow<\/p>\n

The crystals can collide, stick together and build a slushy mixture. Cooling could turn about 1% to 3% of the water into frazil ice.<\/p>\n

Seed ice requirement for runaway frazil ice growth and implications for hydraulic clogging in turbulent Europan dykes. (CREDIT: Lujendra Ojha et al, Nature Astronomy) <\/p>\n

Even when only 1% to 5% of crystals striking the wall remained attached, a one-meter-wide fracture could clog within hours.<\/p>\n

\u201cThere\u2019s an icy shell, there\u2019s water underneath, and there\u2019s all this speculation about how that water can come from deep underground and make its way all the way up without freezing en route,\u201d Ojha said. \u201cThat\u2019s really what we think we disproved.\u201d<\/p>\n

Shallow water may form locally<\/p>\n

Localized heating inside the shell could melt ice in place. A sealed fracture might also focus tidal strain, producing heat and perhaps temporary melting nearby.<\/p>\n

That matters because shallow water may not represent the chemistry of the deep ocean. A nearby reservoir could still interest scientists, but it may not provide a direct sample of Europa\u2019s most compelling environment.<\/p>\n

\u201cOur work suggests that Europa\u2019s ice shell may be a stronger barrier between the ocean and the surface than previously assumed,\u201d Ojha said. \u201cThis helps future missions interpret what they find and better understand where to look for signs of habitability.\u201d<\/p>\n

NASA\u2019s Europa Clipper launched in October 2024 and is scheduled to reach Jupiter in April 2030. It will make 49 close flybys. The European Space Agency\u2019s JUICE mission launched in April 2023 and is scheduled to arrive in July 2031.<\/p>\n

Practical implications of the research<\/p>\n

Europa Clipper\u2019s radar<\/a> may test whether the moon contains shallow reservoirs, frozen fractures or groups of parallel dykes. Those observations could show whether water pathways once connected deeper layers to the surface.<\/p>\n

The work also gives mission scientists a warning. Detecting shallow water would not automatically mean that a spacecraft had found material from the global ocean.<\/p>\n

Future measurements of Europa\u2019s ice structure, ocean conductivity and possible salt content could refine the freezing models. They may reveal whether any conditions allow water to travel farther.<\/p>\n

For now, Europa\u2019s ice appears less like a simple lid and more like an active barrier. That makes the search for habitability harder, but it gives future missions sharper questions.<\/p>\n

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