Scientists have discovered a potential mechanism that could lead to the oceans on icy moons boiling. According to research published in Nature Astronomy, the tidal heating caused by gravitational interactions between the moon and its parent planet can create conditions where the ocean's surface temperature exceeds the freezing point of water.
The researchers suggest that some of these moons are small enough for the low pressure at their icy surfaces to cause the water at the interface to boil. This phenomenon is thought to occur when the interior of the moon melts, creating a low-pressure area under the shell. As the ice expands and contracts, it creates stresses on the ice shell, leading to pressure drops.
These pressure drops can have significant consequences on the stresses experienced by the icy shells of these moons, particularly for smaller bodies where gravity is weaker. In such cases, the water at the interface may boil even at ambient temperatures, creating a unique set of geological features.
Researchers are particularly interested in three small moons: Enceladus, Mimas, and Miranda. Enceladus is known for its geysers, while Mimas has recently developed an ocean. The scientists estimate that Enceladus would only need to melt an ocean about 14 km deep to create conditions where boiling is possible.
However, the implications of this phenomenon are still unclear. Researchers note that the fate of the vapor generated in a subsurface ocean is uncertain and suggest that it could potentially act like liquid magma, forcing its way into fractures in the icy crust. The water should condense while others gases released from the water remain in the gaseous phase.
The study highlights the complex interactions between tidal heating and ice shell stress, leading to conditions where oceans on icy moons can boil. Further research is needed to understand the full implications of this phenomenon and its potential consequences for these unique celestial bodies.
The researchers suggest that some of these moons are small enough for the low pressure at their icy surfaces to cause the water at the interface to boil. This phenomenon is thought to occur when the interior of the moon melts, creating a low-pressure area under the shell. As the ice expands and contracts, it creates stresses on the ice shell, leading to pressure drops.
These pressure drops can have significant consequences on the stresses experienced by the icy shells of these moons, particularly for smaller bodies where gravity is weaker. In such cases, the water at the interface may boil even at ambient temperatures, creating a unique set of geological features.
Researchers are particularly interested in three small moons: Enceladus, Mimas, and Miranda. Enceladus is known for its geysers, while Mimas has recently developed an ocean. The scientists estimate that Enceladus would only need to melt an ocean about 14 km deep to create conditions where boiling is possible.
However, the implications of this phenomenon are still unclear. Researchers note that the fate of the vapor generated in a subsurface ocean is uncertain and suggest that it could potentially act like liquid magma, forcing its way into fractures in the icy crust. The water should condense while others gases released from the water remain in the gaseous phase.
The study highlights the complex interactions between tidal heating and ice shell stress, leading to conditions where oceans on icy moons can boil. Further research is needed to understand the full implications of this phenomenon and its potential consequences for these unique celestial bodies.