Читать книгу Astrobiology - Charles S. Cockell - Страница 92

The possibilities for alternative solvents to liquid water have been discussed for a long time by the astrobiology community. Although water is an abundant solvent in the Universe, other solvents might be plausible in planetary environments with different physical and chemical environments to Earth. Unfortunately, few of these alternatives have been empirically investigated in any depth. Without detection of a life form using them, it is difficult to carry out convincing biological experiments to show that they could be used. Additionally, our knowledge of how the origin of life occurred is not sufficiently complete to be able to test alternative solvents in the laboratory as possible solvents for the origin of life. Nevertheless, some physical properties of alternative solvents might make them candidates.

It has been shown that many enzymes can be active in non-polar solvents such as benzene and that about 20% of the human DNA encodes membrane proteins that require the non-polar environments inside cell membranes to operate. Although these observations do not provide any direct evidence for the possibility of non-aqueous solvents being potentially successful media for complete biochemistry, they show that even some terrestrial biochemistry operates in non-aqueous environments.

Ammonia has been one of the most discussed alternatives to water. Although the chemistries it would be involved in would be different, analog reaction sequences can be envisaged. In Figure 4.20, the central role of the N atom in the formation of new CC bonds in a putative liquid ammonia-based chemistry is illustrated.

Figure 4.20 Chemistry in alien solvents. Different functional groups, but analogous mechanisms, could be used to form carbon–carbon bonds in different solvents. Here this concept is illustrated for forming a new CC bond in water (left) and liquid ammonia (right).

Source: Reproduced with permission of Steve Benner.

Comparing the physical properties of ammonia to those of water yields insights into their possible comparative advantages and disadvantages. Ammonia is less viscous than water (compare 1 centipoise (cP) for water at room temperature to 0.265 cP for ammonia) and so molecules diffuse through it more quickly. We could therefore even speculate that it would make a better solvent for the rapid transport and diffusion of metabolites in a cell. Ammonia has some intriguing capacities that are not seen in water. For example, it readily dissolves metals, resulting in a solution of solvated electrons. As electron transfer is a fundamental part of energy acquisition in known life, maybe the solvent would be highly efficacious for electron transport.

However, ammonia has a lower heat of vaporization (1369 kJ kg⁻¹) than water (2257 kJ kg⁻¹) and so may be less able to maintain a liquid state under rapid environmental temperature changes, depending on the environmental conditions. The greatest difference to water is that ammonia is liquid at lower temperatures and has a smaller liquid temperature range at atmospheric pressure (−78 to −34 °C). In contrast, one could argue that this view is Earth-centric and that in a cold planetary environment, its low-temperature liquid state would provide a solvent for life. The temperature of its liquid range can be increased by increasing the pressure, such that at about 2 MPa (20 atm), the boiling point is increased to around 50 °C.

Ammonia presents other potential challenges for life, most notably the high pH of ammonia solutions. Ammonia solutions of 1% or greater have pH values greater than 11, and biochemistries would require adaptation to these conditions, although organisms with adaptations to high pH are known. In solution, ammonia dissociates into NH₄⁺ and NH₂⁻ ions, the latter binding to protons and thus being annihilative to molecules.

In summary, we can find, like water, both advantages and disadvantages to ammonia as a potential solvent for life. Of solvents that have been investigated, it probably comes closest to water in its versatility. It is universally abundant. Saturn's moon Titan is thought to host a subsurface ocean that may contain ammonia, perhaps at around 30%. It is likely to exist in a variety of extraterrestrial environments where low temperatures favor its persistence. The limitations in our knowledge about its potential as a biological solvent primarily relate to a lack of both chemical and biological evidence that a life form could be constructed in this solvent.

Finally, there are some other suggestions for solvents. Hydrofluoric acid has been discussed as an alternative. The wide temperature range at which it remains liquid makes it a possible candidate, with fluorine replacing oxygen in many molecular structures. However, the low cosmic abundance of fluorine and high reactivity with organic carbon molecules make it limited.

Yet another suggested solvent is methane. Methane is found in abundance on Saturn's moon Titan, where the surface temperature is 94 K. The liquid forms lakes and rivers in a geological analogy to liquid water on Earth. This sheer abundance has invited ideas about the evolution of life within this liquid. As it is non-polar, one intriguing idea is that cells would form inside-out membranes, where the non-polar tails would point into the methane, and charged “methane-phobic” groups would point inwards. As we know that even in terrestrial life trans-membrane proteins operate best in non-polar environments, it could even be that cells and their associated enzymes and proteins assembled in a solvent like methane would be able to escape damaging hydrolysis reactions associated with water. As with other solvents, since we lack an example of life within this alternative liquid, it is difficult to empirically assess its potential. Indeed, ultimately the best way to test such a hypothesis would be to look for life on Titan using spacecraft.

Various other substances have been discussed and some of their properties are shown in Table 4.1. These alternative solvents raise the question of what we require in a solvent for it to be useful in life. Although for any given liquids we can find characteristics that are compatible with the biology we know, to act as a plausible solvent, a liquid must offer several characteristics, including the ability to mediate the diversity of chemical reactions needed for a replicating, evolving chemical system. Investigating these attributes can become tautological in the sense that the carbon-containing chemistry that we know in terrestrial life has evolved in water. To take this entire structure and ask whether it will work in other solvents is almost certainly likely to result in the conclusion that water is best. The simple point is that we just don't know to what extent a reproducing, evolving entity can be built in alternative solvents and what corresponding modifications in its core chemistry compared to terrestrial life would permit it to evolve in such solvents.

Table 4.1 A range of possible solvents for life, their temperature ranges, heats of vaporization, viscosity, and dipole moments.

Solvent	Molecular weight	Liquid range (K at atmospheric pressure)	Heat of vaporization (kJ kg−1)	Viscosity (cP)	Dipole moment (debye)
H2O	18	273.1–373.1	2257	1.00	1.85
NH3	17	195.4–239.8	1369	0.265	1.47
HF	20	190.0–292.7	374.1	0.256	1.91
H2SO4	98	283.5–611.1	56.0	48.4	2.72
CH4	16	90.7–111.7	480.6	0.184	None

We also tend to consider either the core elements used in life's chemistry or its solvent in isolation. However, perhaps altering both would result in a viable system of life. The reactive nature of silicon (when not in silicates) might be mitigated by a silicon chemistry that evolved in cold environments, such as in a liquid nitrogen. Could a silicon-based life form evolve in liquid nitrogen? Although such ideas are intriguing, altering both the fundamental chemistry and the solvent of life takes us even further into unknown chemical territory at the current time. However, these concepts remind us to keep an open mind.