This article has been reviewed according to Science X's editorial process and policies. Editors have highlighted the following attributes while ensuring the content's credibility: Saturn's moon Enceladus sports a thick shell of ice surrounding a liquid water ocean. As though scraped by an enormous claw, four parallel cracks slash across its south pole.
Each about 500 meters (1,600 feet) deep, 2 kilometers (1.2 miles) across and 130 kilometers (81 miles) long, the fissures spew water vapor and other materials from the subsurface ocean directly into space. But the origin of these "tiger stripes" is mysterious. Most prior research has explored the possibility that Enceladus's tiger stripes were created by processes primarily involving the ice shell itself, such as tectonic fracturing and cooling.
Abdulah and colleagues show that waves in the ocean beneath the ice could play a deciding role in their formation. Their paper is published in the journal AGU Advances. The researchers took inspiration from ocean waves on Earth, which can propagate from the seafloor to the surface, focus at a point, break and dissipate.
Using mathematical analysis and computational simulations, the research team investigated how waves in Enceladus's subsurface ocean might interact with the inner surface of the ice shell. They incorporated a key feature of the moon: because of its irregular orbit around Saturn, the moon's entire ice shell wobbles relative to its ocean. In the new picture of tiger stripe formation, one initial fissure already existed in the ice shell.
As the shell wobbled, the motion of the fissure's uneven underside topography against the liquid ocean below excited waves, which traveled tens of kilometers through the ocean to the seafloor. The waves then ricocheted back up and broke against an adjacent part of the ice shell, imparting energy as heat that began to melt the ice from beneath. The analysis suggests that this melting could kick-start a process that would eventually carve out additional parallel fissures about 35 kilometers (22 miles) apart—matching the observed spacing of Enceladus's existing tiger stripes.
If this proposed mechanism is correct, it would set constraints that reveal additional characteristics of the subsurface ocean, including how its density changes with depth. Additional modeling and a possible future mission to Enceladus could help refine and test the mechanism and its implications. Abdulah et al, An Oceanic Mechanism for Geyser Formation on Enceladus, AGU Advances (2026).
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