The team used an ice-sealed metastable reservoir to generate eruptions from within the experimental setup. As the liquid boiled, it produced internally generated overpressure that drove material from the subsurface reservoir. At about 4.5 mbar, the eruptions evolved systematically: energetic ballistic fountains gave way to episodic flows, and the discharged material eventually formed coherent mud-flow structures. This sequence contrasts with the commonly assumed rapid quenching of metastable liquid eruptions exposed to near-vacuum planetary environments.

The experiment exposed an interaction between ballistic transport and deposition around the vent. Airborne droplets and fragments redistributed liquid mud around the eruption site, while material landing nearby accumulated into proximal deposits. Those deposits then coalesced into sustained flows despite continued cooling and freezing. The observations show that an eruption at low pressure need not stop as soon as its material begins losing heat; mud could pass through distinct ballistic and effusive stages and still reach a surface-emplaced flow stage.

Numerical modeling complemented the pressure-controlled experiment by examining transport under Martian gravity. The model indicated that erupted mud would remain largely unfrozen during ballistic transport in Martian gravitational conditions. It therefore supports the physical plausibility of a sequence in which material does not freeze rapidly during flight. The experiment directly reproduced the eruption behavior under Martian-like pressure, whereas the gravity-dependent result came from modeling rather than an eruption observed on Mars.

The combined results provide experimental and modeled constraints on sedimentary volcanism under low-pressure conditions. In the laboratory process, boiling supplied the overpressure needed to initiate and continue eruption, while ballistic redistribution helped produce accumulations that developed into coherent flows. The study does not demonstrate that eruptions occur on Mars, establish their expected scale or frequency there, or reproduce the full range of planetary surface conditions. Instead, it shows that rapid boiling, cooling and freezing can coexist with continued eruptive transport and surface emplacement, offering a broader physical framework for metastable liquid eruptions across the Solar System.

Subject of Research: Experimental and modeled low-pressure sedimentary volcanism under Martian-like conditions

Article Title: Effusive sedimentary volcanism experimentally reproduced under Martian-like conditions

Article References: Krýza, O., Brož, P., Adler, J., Sylvest, M., & Patel, M. (2026). Effusive sedimentary volcanism experimentally reproduced under Martian-like conditions. Communications Earth & Environment. https://doi.org/10.1038/s43247-026-04155-x

Image Credits: AI Generated

DOI: 10.1038/s43247-026-04155-x

Keywords: Mars, sedimentary volcanism, low-pressure experiments, effusive eruptions, boiling overpressure, mud flows, ballistic transport, cryovolcanism, planetary science, Effusive, sedimentary, volcanism