by Amanda Doyle for Astrobiology Magazine
Moffett Field CA (SPX) Sep 07, 2012
Triton was discovered in 1846 by the British astronomer William Lassell, but much about Neptune's largest moon still remains a mystery. A Voyager 2 flyby in 1989 offered a quick peak at the satellite, and revealed a surface composition comprised mainly of water ice.
The moon's surface also had nitrogen, methane, and carbon dioxide. As Triton's density is quite high, it is suspected that it has a large core of silicate rock. It is possible that a liquid ocean could have formed between the rocky core and icy surface shell, and scientists have investigated if this ocean could have survived until now.
Captured from the Kuiper Belt
These orbits are known as prograde, and a rogue object that orbits backwards is said to be in a retrograde orbit. The retrograde orbit of Triton means that it most likely did not form around Neptune.
The early Solar System was a place of dynamic violence, with many bodies changing orbits and crashing into each other. Triton likely originated in the Kuiper Belt, beyond the orbit of Neptune, and was sent hurtling inwards until it was captured by Neptune's gravity. Directly after capture, the moon would have been in a highly elliptical, eccentric orbit.
This type of orbit would have raised large tides on the moon, and the friction of these tides would have caused energy to be lost. The energy loss is converted into heat within the moon, and this heat can melt some of the icy interior and form an ocean beneath the ice shell. The energy loss from tides is also responsible for gradually changing Triton's orbit from an ellipse to a circle.
Heating the interior
Radiogenic heating contributes several times more heat to Triton's interior than tidal heating; however this heat alone is not sufficient to keep the subsurface ocean in a liquid state over 4.5 billion years. However, tidal dissipation causes heat to be concentrated at the bottom of the ice shell, which impedes the growth rate of the ice and effectively acts as a tidal-heated blanket. This tidal dissipation is stronger for larger values of eccentricity, meaning it would have played a major role in heating Triton in the past.
"While the concentration of tidal dissipation near the bottom of ice shells was known for some time, we believe our work is the first to demonstrate that it indeed controls the rate of freezing and sustainability of subsurface oceans," says Saswata Hier-Majumder at the University of Maryland. "Radiogenic heating, in comparison, heats up the shell uniformly, and thus doesn't have as disproportionate an influence as tidal dissipation does."
Sustaining the ocean
As Triton cools, the ice sheet will grow to engulf the underlying ocean. The new research calculates how the thickness of the ice shell can influence the tidal dissipation and thus the crystallization of the subsurface ocean. If the ice shell is thin, then the tidal forces will have a more pronounced effect and increase the heating. If the shell is thick, then the moon becomes more rigid and less tidal heating will occur.
"I think it is extremely likely that a subsurface ammonia-rich ocean exists in Triton," says Hier-Majumder. "[But] there are a number of uncertainties in our knowledge of Triton's interior and past which makes it difficult to predict with absolute certainty."
For instance, the exact size of Triton's rocky core is unknown. If the core turns out to be larger than the value used in the calculations, then there will be more radiogenic heating, with extra heating increasing the size of any existing ocean. The depth of the ocean also may not be constant across the moon, as tidal dissipation concentrates energy near the poles, meaning that an ocean would likely be deeper there.
In addition, recent calculations estimate that icy bodies in the outer Solar System could be comprised of up to 15 percent ammonia. Ammonia-rich volatile material works to lower the temperature at which a solid turns to a liquid, and the presence of such volatiles may also help the persistence of a liquid layer beneath the ice.
Life in the ocean
The ammonia that is likely present in Triton's subsurface ocean might act to lower the freezing point of water, thus making it more suitable for life. The temperature of the ocean is still probably around 176 K (minus 97 C, or minus 143 F), which would slow down biochemical reactions significantly, and impede evolution. However terrestrial enzymes have been found to speed up biochemical reactions down to temperatures of 170 K.
Another more remote possibility is that Triton could host silicon-based life, assuming that silicon can actually be used as a foundation for life instead of carbon. Silanes, which are structural analogues of hydrocarbons, could be used as a building block for life under the right conditions.
The frigid temperatures and the limited abundance of carbon on Triton could be suitable for silicon-based life, but there isn't enough known about the behavior of silanes in such unusual conditions to firmly state that such life could exist.
The research by Jodi Gaeman, Saswata Hier-Majumder, and James Roberts was published in the August issue of the journal Icarus.
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