On The Death of Planets

It’s been a long time since I’ve posted here!  I am in the thick of writing my thesis and getting a job lined up for after graduation.  Still, sometimes I can sneak away and write on my own time for half an hour.  This precludes me making big, well-researched posts like the one on different schools of origin-of-life research or the astrobiological gems of the solar system I’ve been planning.  But I have time to talk briefly about something I’ve been thinking about lately.

In my post “Space and Time – Part II” I sketched out my rough calculations about our place in star and biosphere order, coming to the conclusion that our sun is in around the last fifth of all stars that will ever exist and that our biosphere is somewhere between halfway and 30% of the way through the total complement of biospheres our universe will ever have.  This, however, did not address our position in ABSOLUTE time within 15 billion years of the start of an apparently open ended universe – only our position in the order of stars and planets that will ever exist.

Our sun is large, larger than something like 80% of all stars that exist.  This has interesting implications.  The bigger a star is, the brighter it is.  Brightness increases far faster than mass – for stars in the mass range near the sun, a star twice as massive is 16 times as bright, brightness going up with the fourth power of mass.  This means that star lifetime goes down with the cube of star mass.  A star half as big as the sun will glow stably for 8 times as long.  This, combined with the fact that most stars are small, means that the vast majority of star-years that will ever happen in the universe happen around tiny stars.  The smallest stars may burn for five trillion years, the epoch of star formation we are living through the latter days of constituting the barest tiny fraction of their early history.

This has not escaped the notice of professional astronomers.  An analysis much like what I put forward in “Space and Time – Part II” was put forward in a paper by Loeb, Batista, & Sloan in the latter half of 2016, entitled “Relative likelihood for life as a function of cosmic time“.  Their numbers are a little different due to fitting different datasets but the broad conclusion about the impending end of star formation over the future history of the universe is the same.  What these authors did that I did not do, however, was to integrate the total number of star-years occurring over the history of the universe as the huge burst of star formation that is winding down now finishes and the large stars die, followed by a slower and slower rate of death of smaller and smaller stars.  According to their data, if you go by total star years that will ever happen in the universe we are in something like the first thousandth of available time with the vast majority of star-years occurring in the far distant future around dim red dwarfs.  See here for a bit in the popular press about it.  They conclude that this means that either we are exceedingly early in the universe or small stars are unsuitable for biospheres, and that the average star mass at which we find ourselves at a typical time comes to something like 0.9 solar masses.

This analysis, however, leaves out something extremely important.  This is not surprising, because what it leaves out has nothing to do with stars and everything to do with planets.  Namely, it ignores something I think is of fundamental importance to the study of astrobiology:  geology and atmospheric science, and the fact that planets can die.

What does it mean for a planet to die?  We can take our own Earth as an example.  This planet has been in a state of pretty good homeostasis for the history of the solar system so far.  We have never lost our atmosphere or hydrosphere, and we have never popped into a runaway greenhouse mode like Venus – the surface has been clement since some time deep into the Hadean all the way through to today. This is largely due to something called the carbonate-silicate cycle.  CO2, a greenhouse gas that warms the planet, is belched out of the interior of the planet through volcanoes.  On Venus, once CO2 is in the atmosphere it stays there, never to be returned to rock.  That is not the case here.  Here, there are oceans.  CO2 dissolves in water and reacts with it, interconverting with the following formula:

CO2 + H2O CH2O3

The product of this reaction is carbonic acid, which reacts with dissolved minerals to form carbonate rock which sequesters carbon out of the atmosphere back into the geosphere.  This is paired with another reaction, catalyzed by the protons released by acids in water solutions:

SiO3 + 2H+ SiO2 + H2O

In this reaction, silicate rock thrust up to the surface by geological activity reacts with acids to form silica which again returns to the geosphere.  Both of these reactions proceed overall in the forward direction at the conditions found on Earth’s surface, with CO2 becoming carbonate rock and silicate rock becoming silica.  But deep inside the Earth at high pressures and temperatures, these reactions tend to run in the opposite direction, generating the carbon dioxide and silicate rock that are pushed to the surface.  This forms the longest timescale piece of the global carbon cycle.  On geological timescales this maintains rough equilibrium of Earth’s surface temperature, as the removal of CO2 into carbonate rock runs faster at high temperatures producing a negative feedback loop that alters atmospheric composition to prevent Earth from becoming too hot or cold.

This will NOT always be the case.  Our biosphere has an expiration date.  In our case, it comes from the steadily brightening sun.  All stars brighten during their stable lifetimes – they roughly speaking double in brightness over their time in the main sequence, before going through more drastic gyrations at the end of their life.  Our sun was about 70% as bright as it is now at the dawn of the solar system, and will wind up significantly brighter than it is now before it turns the corner and shoots off into the red giant state 5+ billion years from now.  Depending on whose climate models you use, the homeostatic mechanisms that apportion carbon between methane CO2 and carbonate rock and maintain roughly even temperatures over geological timescales on Earth will reach their breaking point somewhere between 300 megayears and 2 gigayears from now – the most likely timeframe seems to be about 1.2 gigayears (see Lenton & Bloh 2001, Biotic feedback extends the life span of the biosphere).

At this time, the energy pouring in from the sun will exceed the level at which even with zero carbon in the air we could avoid our oceans starting to evaporate excessively.  Water is an even better greenhouse gas than CO2, and once enough gets into the upper atmosphere it’s all over.  A runaway feedback loop will commence in which more of the oceans evaporate, trapping more heat and evaporating more water, until all the water on Earth has become a steam atmosphere upwards of a hundred times as thick as today and quite warm all the way up to the edge of space.  Over time, the water in the upper atmosphere will be split by ultraviolet radiation and the hydrogen will escape to space, the oxygen staying behind to oxidize surface rocks and creating sulfuric acid from the sulfur exhalations of volcanoes.  The CO2 pouring out of volcanoes will have no liquid water to dissolve into and will stick around thickening as the water slowly depletes until the Earth is a twin of Venus, having gone through the exact same process its sister planet went through long ago.  Maybe a few microbes could survive, lofted up into the clouds and never plunging into the sterilizing depths; maybe not.

This is the ultimate fate of any large terrestrial planet like Earth around a star large enough to brighten rapidly.  It was certainly the fate of Venus.  Venus may have started out like Earth is today and gone through this process early in the solar system’s history or it may have always been in the runaway greenhouse state, its greater solar radiation preventing the condensation of oceans from its hot birth.  We simply can’t know with the evidence at hand, especially given that the planet’s history more than 500 megayears ago is obscured by massive lava flows that covered most of its surface then.

This is not, however, the only way a planet can die.  One needs only look at Mars to see another way.  We know that Mars used to be warm and at least intermittently wet, with an active hydrosphere and conditions that were surprisingly Earthlike.  This was back when it was getting less than a third the sunlight the Earth gets today.  But Mars is small.  Its interior is closer to its surface, and it had less primordial heat of formation.  It cooled off, its volcanic outgassing that built the atmosphere fell through the floor, its low gravity lead to high rates of atmosphere loss, and it lost its internal geological-convection-driven geodynamo and magnetic field.  Fresh nutrient minerals stopped being delivered to the surface as the atmosphere and hydrosphere were sputtered away and the planet froze over.  There are reasons that if there is any life on Mars today it is deep underground and any surface biosphere that could’ve existed in the past died long ago.  This would eventually happen to ANY  terrestrial planet, even if it were around a star that would last for five trillion years.  I am completely unprepared to determine how long a planet like Earth would last if it weren’t for the brightening sun, but it sure isn’t that long.

The biggest rocky planets that seem to exist, according to the Kepler data, look to perhaps be 1.5 Earth radii and thus about 3.3 Earth masses.  This is an upper limit based on densities of known exoplanets – almost no planets larger than 1.5 Earth radii have densities like that of rock whereas many below do.  We have no idea what the atmospheres of 1.4 Earth radius planets are like – they could be temperate places with rain or crazy 500 atmosphere hells for all we know.  But these planets would create about 3.3x the radiogenic heat of Earth with 2.25x the surface area, for a surface area to volume ratio of about 2/3 that of Earth and 1/3 that of Mars.  Eventually they too will run down, the geosphere grinding to a halt and the atmosphere hydrosphere and any biosphere slowly trickling away.  A small red dwarf may last five trillion years, but for the vast majority of that history any terrestrial planets will be dry, vaccum blasted dead husks of their former selves (barring rare catastrophic collisions between planets that might reset some clocks here and there).

Incidentally, terrestrial moons of gas giants may get around this if they are tidally heated through gravitational resonances with other moons, heating themselves internally by stealing the energy of rotation of the central planet.  However, it remains an open question if rocky as opposed to icy moons of terrestrial planet mass are even an option around gas giants – the total mass of moon systems of gas giants in our outer solar system are universally about 1/10,000 that of the mass of the central planet and have a lot of ice mass in addition to rock mass, so large rocky moons big enough to maintain atmospheres at liquid water temperatures may be pretty rare.  But places like Europa where low-energy and low-biomass biospheres are an option might last a very long time.

Anyways, if you assume that planets with biospheres die with a lifetime of say ten billion years, you no longer need to postulate a narrow range of valid star masses for us to be a typical observer.  Our absolute time becomes typical again, 5 billion years into the lifetime of a biosphere, even though our world might last a shorter time than average due to the brightening large sun.  We do wind up in the upper 10-20% of star masses hosting a biosphere that lasts this long, but this is significantly less extreme than the one in a thousand value we started with.

For all we know smaller stars could also still be nonviable for big biospheres bringing our true position in the stellar mass distribution for big biospheres closer to average.  Below something like two thirds of a solar mass you start getting into orbital regimes where a planet warm enough to have liquid water on a rock surface is close enough to the parent star that it tidally locks and we honestly don’t know if that’s a showstopper or not.  Or there could be something about planets that form close to stars in absolute distance terms (rather than radiation received terms) that makes them different and unsuitable.  Or maybe you actually need to tune the running down of a geosphere putting out less greenhouse gases over time with the brightening of a star, such that you do have a narrow population of stars that brighten at the same timescales that planets run down and the two effects balance.  More information is desperately needed, which we are only just barely starting to get by observation of exoplanets.  I look forward to the possibility of getting atmospheric information from spectra of exoplanets that transit their parent stars to help clear this up.

Energy, Metabolism, and Photosynthesis

Originally I sat down to write about the large-scale history of Earth, and line up the big developments that our biosphere has undergone in the last 4 billion years.  But after writing about the reason that Earth is unique in our solar system (photosynthesis being an option here), I guess I needed to explore photosynthesis and other forms of metabolism on Earth in a little more detail and before I knew it I’d written more than 3000 words about it.  So, here we are, taking a deep dive into photosynthesis and energy metabolism.

Again, fans of the ‘rare earth hypothesis’ will tend to take a look at everything along the history of Earth and argue that if anything had happened differently, we wouldn’t have the big happy biosphere we have today.  This only holds water, however, if there was no other way to have what happened happen.  It also only really holds water if there is only one instance of the major transitions in Earth’s biosphere – if something happened multiple times on Earth you can argue that it is likely to happen anywhere there is life, while if something only happened once here it is at least possible that we are here because of a very rare event that doesn’t often happen, and necessarily see that unusual event.  Here, I will try to dissect energy metabolism across the set of living things on Earth and argue that at least coupling light to it is probably likely to happen anywhere there is light falling onto a biosphere.

I would like to refer all my readers to a wonderful recent book on photosynthesis, from which I derived more than half of my understanding of it:  “Oxygen, a Four Billion Year History” by Donald Canfield.  It is an amazing walk through the current state of the art of research on both the history/origins of photosynthesis, and the history of molecular oxygen in Earth’s atmospheric and geological chemistry.  I would also like to refer everyone to another recent book that touches on energy metabolism and the origin of life by Dr. Nick Lane, entitled “The Vital Question: Energy, Evolition, and the Origins of Complex Life”.  The first third of the book is a thorough look at a particular strand of origin of life research I find compelling in many of its details, and the latter two thirds explores the origin and attributes of Eukatyotes from a perspective I am rather less of a fan of but think makes some important points, and will get to later.

Redox Metabolism

I am going to make a bold claim:  all metabolism on Earth depends ultimately on redox gradients, and photosynthesis is just a way to generate these internally in a cell from light.

Redox reactions – named for oxidation and its opposite, reduction – are chemical reactions that involve the movement of electrons from one substance to another during the reaction.  A substance that loses electrons in a reaction is said to be oxidized (so named long ago because oxygen is a fantastic oxidizing agent that will suck electrons away from almost anything) and something that gains electrons is said to be reduced (a horrible piece of nomenclature – blame 18th century chemists who didn’t understand electrons and only thought about redox reactions in terms of gaining or losing oxygen).  When hydrogen burns in oxygen, the result is water.  The OH bond in water is asymmetrical – oxygen pulls on the shared electrons in the bond much harder and gains a partial negative charge.  The oxygen is reduced, as it has gained some electron density from the hydrogen, and the hydrogen has been oxidized as it has lost some of its electron density.  This definition can be extended to any substance, even ionic substances like iron which can exist in two redox states – Fe2+ is more reduced than Fe3+ because it has one more electron.

The most obvious way that metabolism depends on redox reactions is the fact that all carbon in biomass ultimately comes from CO2.  This is a highly oxidized and inert form of carbon, and it must be reduced and some oxygens pulled off of it before it can do the interesting chemistry of life.  In all of life, there are six known molecular pathways through which carbon is stripped out of CO2 and built into biomolecules.  In all of them, both cellular energy and highly reduced ‘carrier’ molecules react with CO2 to reduce it.  The energy applied massively increases the reaction rate, and the reduced carrier molecules strip away the oxygens as water and reduce the carbon so it can bond with other carbons and hydrogen.  These reducing carriers either need to be reduced themselves by reducing agents in the environment that the organism eats, in the case of chemolithotrophic bacteria that live far away from sunlight, or they need to be reduced by photosynthesis forcing electrons from another substance out in the word onto it by the energy of photosynthesis.

There is one carbon fixation pathway that is special that I will talk about more in later blog posts.  This is sometimes called the acetyl-coenzyme A pathway, and sometimes the Wood-Ljungdahl pathway.  It is the pathway by which methanogenic archaea and acetogenic bacteria react hydrogen gas from geological or biological sources with CO2 to build biomass.  Of all six known pathways, it is the only one found in both the archaebacteria and the eubacteria – the two deepest branches on the tree of life that split off the last universal common ancestor, ‘LUCA’.  This alone should be a clue that it is important.  But secondly, it is the only carbon fixation pathway that is on the whole spontaneous and does not require an external input of energy – its early stages require an input of energy, but its later stages actually generate more energy than is consumed.  This is because hydrogen gas is such a strong reducing agent – most substances when reacting with it will pull electrons away from it.  As such, fixing carbon using hydrogen gas has been called, “a free lunch you are paid to eat,” by certain origin of life researchers.  It is actually energetically favorable for CO2 and hydrogen gas to interact to build biomass.  This pathway may have a key role to play in the origin of life, which I will discuss another time.

Secondly, life gets energy to DO things from redox gradients, not just build things.  Redox gradients are perfect for life to insert itself into as a middleman to get energy out of.  Temperature gradients, for example, are pretty much a nonstarter – a cell is usually at most microns wide, and there are no natural temperature gradients that matter that are that sharp in the natural world.  Redox gradients can get inside a cell – you can have an oxidized molecule and a reduced molecule right next to each other inside an organism, and it can require a catalyst to get them to react.  The energy released by that reaction is, by and large, harnessed by a mechanism called chemiosmosis.  Cells make sure that the reaction that pulls an electron away from a reducing agent and the reaction that adds one to an oxidizing agent happen in different places on the cell, usually on a cell membrane.  They then pass electrons between these places through what’s called an electron transport chain, a series of membrane-bound proteins carrying metal ions and other reactive redox reaction centers that the electron  must pass along in order to complete the energetically favorable redox reaction.

The electron transport chain of animal mitochondria, in which food is oxidized by oxygen to pump protons out of the mitochondrial inner membrane.  These protons leak back across their concentration gradient, driving the production of ATP via the ATP synthase.  There are many other quite diverse electron transport chains across biology.

The electron moving from protein to protein to complete the reaction is coupled to and forces the pumping of protons – hydrogen ions – through the membrane from the inside of a cell to the outside.  As these reactions proceed a proton gradient (and thus a pH gradient) is built up across the membrane.  This gradient is then allowed to dissipate through something called the membrane ATP synthase – a huge rotary complex that couples the dissipation of the proton gradient to the production of ATP, a highly energetic molecule that most processes that use energy in biology get their energy from.  Why this roundabout coupling?  Because ATP is a highly energetic molecule and many redox reactions do not release enough energy to cause a whole molecule of ATP to be produced.  But by pumping protons across a membrane and building a gradient, the effects of multiple redox reactions can be accumulated and saved up until enough energy has been stored to produce one molecule of ATP.

The only energy metabolism on Earth that doesn’t use membrane-bound redox manipulating proteins is fermentation – a whole slew of processes that take large biomolecules and rearrange their atoms into slightly lower energy states.  But even that rearrangement is an intramolecular redox reaction – the bonds are rearranged in such a way to slightly reduce oxygen further, slightly oxidize hydrogen further.  Through some clever chemistry a tiny amount of the energy provided by their rearrangement – say from sugar into CO2, alcohols, and acids – is captured but it’s very small compared to the energy you get from bigger electron transfers between different substances.  But ultimately, all carbon fixation from CO2 into biomass derives from either reducing CO2 using a reducing agent out in the environment and energy from a collapsing a redox disequilibrium, or photosynthesis.  As such, organisms that ferment biomolecules all ultimately depend on other living things for their energy.  They also all show evidence of descending from precursors that used redox reactions pumping protons for energy.  As such, chemiosmotic energy production appears to be ancestral to all life, likely via chemolithotrophy, consuming chemical redox gradients be it between CO2 and H2 or other slight disequlibria within Earth’s geosphere.


As I mentioned in my last post, “The Solar System:  Why Earth?” photosynthesis is the reason that Earth is what it is today.  It drives the vast majority of metabolic activity on the planet and has chemically transformed the atmosphere and geosphere.  The story of Earth since this set of metabolic pathways was invented is, arguably, mostly the story of photosynthesis and its interaction with the geosphere and the evolutionary pressures it created for all life on Earth.  As the source of almost all biomass on Earth and the force that built the planet we have, I think it deserves a really deep look.

Light is a very interesting biological energy source.  There are multiple reasons that all photosynthesis makes use of what we call ‘visible light’.  One, there’s a LOT of it here – at our sun’s temperature, the vast majority of the radiation it emits is in this band of wavelengths, and our atmosphere is really only strongly transparent to two bands of frequencies, the visible and the radio.  Two, the energies that visible light photons have really are special.  Longer wavelengths, like infrared or microwaves or radio, can transfer energy and heat things up but individual photons do not have enough energy to move electrons around inside the organic molecules that living things are composed of.  They do often contain enough energy to vibrate or rotate bonds, but the electrons stay stuck exactly where they are and no chemical reactions are driven since photons and electrons interact for the most part in a binary way, transferring the exact amount of energy embodied in the photon.  Shorter wavelength photons, like ultraviolet light or X-rays, are so energetic that they can completely blow apart organic molecules or break bonds turning biomolecules into highly reactive poisons.

Visible light, on the other hand, has just the range of energies that can kick electrons around within organic molecules without completely breaking them, forcing the molecules into excited states or different shapes.  Strong enough to shuffle electrons, weak enough to not shatter the molecules completely.  This is especially interesting given what I said above about the metabolism of all life ultimately deriving from redox gradients – the movement of electrons from one substance to another during chemical reactions.

Photosynthesis has originated at least twice in Earth’s biosphere.  Or, more technically, phototrophy has – there is a distinction to be made between organisms that use sunlight to produce energy to DO things (phototrophs) or MAKE things (photosynthesizers).  All cells that photosynthesize are phototrophs, as they must be able to extract energy from sunlight, but only a subset of phototrophs are able to take that energy and embody it in long-lived organic biomolecules rather than just run their energy-using processes off it while they get their organic molecules from elsewhere.  Only one of these two origins of phototrophy has been elaborated into photosynthesis, in multiple inventive ways (one of these being oxygen-producing photosynthesis).  It is photosynthesis that has then gone on and remade the world.

Bacteriorhodopsin, via the Protein Databank (and Wikipedia).  Retinal pigment caged inside in purple.

The simplest form of phototrophy on Earth is the plethora of microbes carrying a molecule called bacteriorhodopsin (or a whole bunch of evolved derivatives of it) – a membrane-bound protein clutching a little purple dye molecule called retinal (note the name: it’s the same dye that in our own eyes is clutched by different proteins with a similar shape but probably a separate evolutionary origin).  When a photon of the proper frequency range hits this molecule (mostly green, leaving purple behind to see) it can excite it and flip the molecular structure of one particular bond 180 degrees and change its shape, in the process forcing a proton across the membrane from the inside to the outside of the prokaryotic cell.  This proton can then be brought back through the membrane by the ATP synthase or other channels that couple the breakdown of the proton gradient to other activities.

Light flips a particular bond in retinal from ‘trans’ to ‘cis’ arrangement, causing the pumping of one proton per photon across the cell membrane through the bacteriorhodopsin protein.  Image by Darekk2, from Wikipedia.

Bacteriorhodopsin really just gives a cell that carries it energy, not the ability to fix carbon in and of itself.  It is also rather inefficient, with every photon captured only pumping one proton and thus wasting a lot of the available energy.  But it’s simple and inexpensive.  All you need for it is the metabolic pathway required to build the retinal pigment (not much protein per cell all things considered) and the single bacteriorhodopsin gene that represents the pump itself.  This phototrophy pathway has been horizontally transferred all over the eubacteria and archaea by these microbes swapping genes around (and a few times into the Eukaryotes where it is usually substantially altered to do something completely different) to the point it’s pretty hard to figure out where and when it originated within the eubacteria or archaea.

The second, substantially more complex form of phototrophy looks a bit more like the redox-driven metabolisms I previously spoke about and is ultimately a way of transforming the highly organized energy of visible light into a redox gradient internal to the cell.  Everything with this second form of phototrophy uses some variation on the theme of chlorophyll or bacteriochlorophyll as important pigments, caged up in a massive membrane-bound protein complex called a photosystem.

An incomplete Photosystem II structure from cyanobacteria.  Proteins as ribbons, pigments as green ball-and-sticks wedged between them.  Illustration by Curtis Neveu, from Wikipedia.

You can tell just from looking at this that it’s a much much more complicated system, with dozens of proteins involved (not all pictured and not all part of the photosystem) and multiple types of pigments embedded in it.  What happens in these photosystems is special:  they are where the energy of light is turned into an internal redox gradient.  Light hits one of the pigments in the photosystem, or one of some dispersed ‘antenna’ pigments elsewhere in the membrane of the cell.  These pigments become electrically excited, and are capable of transferring this excitation back and forth between themselves, until the pigment at the active center of the photosystem is excited.  At the active center, this electronically excited pigment transfers an electron to another molecule, losing that electron.  When this happens, suddenly you have one molecule with an overabundance of electrons (a very strong reducing agent) and one with a deficit of electrons (a very strong oxidizing agent).  It is very energetically favorable for those molecules to react and release this energy like any other favorable redox reaction.  But the structure of the photosystem catalyzes the creation of that gradient from the excited pigment, not its dissipation by letting them react.  To dissipate the new redox gradient between these two molecules, the electrons have to go through a Rube Goldberg apparatus that wrings as much energy as possible from them in the process.

Some phototrophic organisms (green nonsulfur bacteria, most purple nonsulfur bacteria, etc) basically just run the electrons from one photosystem through a circular electron transport chain, running them from the photosystem through membrane protein complexes until the end of the chain dumps the now lower-energy electron back into the oxidized pigment, restoring it to its original state but having pumped several protons across the membrane in the process.  This, again, just extracts energy from the light and puts it into the form of a proton gradient that the rotary ATP synthase or other processes can dissipate to let the cell do its business but does it much more efficiently than bacteriorhodopsin can at the expense of complexity.

Other organisms actually take the redox gradient created within a photosystem and use it to fix CO2 into biomolecules, performing photosynthesis.  These organisms (the green sulfur bacteria, the purple sulfur bacteria, some purple and green nonsulfur bacteria, etc) take the electron rich reducing agent generated in the photosystem and through the various carbon fixation pathways use it to reduce the carbon in CO2 into biomass (average formula: CH2O).  This, however, leaves the extremely strong oxidizing agent in the photosystem un-neutralized.  It has to be neutralized or else the cycle cannot repeat – for every carbon that is reduced using light energy, something else has to be oxidized by the photosystem using light energy. A whole slew of substances are possible – hydrogen sulfide can be oxidized to elemental sulfur as in the various sulfur bacteria, ferrous iron (green Fe2+) can be oxidized to ferric iron (red Fe3+, rust), or water can be oxidized into oxygen.  Ultimately, photosynthesis is thus a process for ripping electrons from something in the environment, thus oxidizing it, and using the electrons to reduce CO2 into biomass.

Oxygen-producing photosynthesis appears to have only appeared from photosystem-type photosynthesis once, in the cyanobacteria.  But today it is by far the most common kind.  This has very little to do with the fact that it makes oxygen in and of itself.  Dissolved ferrous iron, hydrogen sulfide, and water are all perfectly good electron donors for photosynthesis.  But oxygenic photosynthesis both sidesteps factors that limit all other forms of photosynthesis and simultaneously forces these other forms to the sidelines.

If you are fixing carbon using sulfur producing photosynthesis, you need hydrogen sulfide – two H2S molecules for every CO2 molecule you turn into biomass.  If you are using ferrous iron, you need four Fe2+ ions for every CO2 you fix.  These molecules are produced geologically, iron leaching out of rocks as they are weathered by water and hydrogen sulfide belching out of volcanoes and coming up from underground in certain types of hydrothermal vents.  But the rate at which carbon can be fixed by a biosphere running on these forms of photosynthesis is constrained by the rate at which these substances are produced geologically.  There’s a cap, and these substances are the limiting factor.  Oxygen producing photosynthesis, on the other hand, uses water itself as the chemical source of electrons, two H2O for every CO2.  It’s hard to think up a more common substance in biology.  In one stroke, the evolution of oxygenic photosynthesis removed a primary chemical limiting factor for biomass production and turned the limiting factor into mineral nutrients, atmospheric CO2 levels, or light energy itself, depending on the ecosystem.

On top of this, once oxygenic photosynthesis became common enough the oxygen byproduct of biomass production started rapidly oxidizing the geosphere and atmosphere with massive side effects.  In the presence of absolutely TINY levels of atmospheric oxygen, ferrous iron immediately turns into ferric iron oxide – rust – and falls out of solution, eliminating one major source of nonoxygenic biomass production from the biosphere.  Huge bands of iron oxide from the ancient ocean floors show this process from what is known as the ‘great oxidation’ 2.3 billion years ago when atmospheric oxygen levels first rose from nothing to just barely something.  Oxygen also oxidizes hydrogen sulfide into water and sulfate salts – and living things accelerate this process, building electron transport chains to get energy for themselves using oxygen as the oxidizing agent and hydrogen sulfide as the reducing agent.  This practically eliminates it from the biosphere except in the places where it is generated (which often have no available light).  In short, oxygen rapidly oxidizes all the reduced substances that can be used by other forms of photosynthesis as electron sources, so not only does oxygenic photosynthesis remove limiting factors on biomass production, but it crowds out the competition.  These other forms of photosynthesis most assuredly exist today, but they are marginal, making tiny fractions of the biomass of the planet in special environments.

Oxygenic photosynthesis is a funny hack of the photosystem-based photosynthesis pathway.   Oxygen is a VERY strong oxidizing agent, much stronger than sulfur or Fe3+, and it takes a lot more energy to rip the electrons out of water to make it than it takes to rip them out of hydrogen sulfide or ferrous iron.  Given the efficiency that photosystems have, there’s not enough energy captured from a single visible light photon to do it even though there is enough energy to do so to these nonoxygenic substrates.  In cyanobacteria, the one place that oxygenic photosynthesis emerged, the two different uses for photosystems were combined.  In essence, an energy-producing photosystem and a sulfur-producing photosystem were tied together by a short electron transport chain in between them in the same cell.  The energy producing photosystem stacks its energy on top of the energy captured by the sulfur producing photosystem, allowing the combined pathway to use the energy of two photons rather than one to rip apart water and allow this ubiquitous but tough substrate to be used.  This also necessitated the evolution of the part of the oxygenic photosystem II that splits water, the oxygen-evolving complex – there’s some weird chemistry that happens there that is unlike what happens when hydrogen sulfide is involved and there is quite a bit of argument over how it came to be.

This is weird.  No other phototrophic microbes have both the energy-producing and the photosynthesizing photosystem in the same cell – two very similar but still divergent protein complexes – but instead only have one or the other.  It’s hard but not impossible to imagine horizontal gene transfer moving around that many dozens of genes in a coherent way.  One popular hypothesis surrounding the origin of oxygenic photosynthesis suggests that an ancestral photosynthesizing microbe actually had both the circular electron transport chain photosystem and the sulfur / iron / etc oxidizing photosystem which had been duplicated within its genome and diverged, and would switch between them depending on the environment and what it needed.  In this situation the lineage leading to the cyanobacteria chained them together, while in all other known lineages of phototrophic/photosynthetic bacteria one or the other photosystem would have been lost (loss being close to irreversible for such a big complicated system and likely to happen to something if it’s ever not needed by a lineage for a long enough while).  This hypothesis is, however, unconfirmed, and the details of the origin of oxygenic photosynthesis are not well understood other than that it appears to have come from a lineage that was capable of both using light for energy and using light to make biomass using hydrogen sulfide.  The question is still open as to how this happened.


No one really knows the time at which oxygenic photosynthesis first appeared.  People like to point to the ‘great oxidation’ about 2.3 billion years ago, but that just represents the time at which the main geological sinks that sucked up biogenic oxygen filled up and oxygen became a measurable force in the atmosphere.  Volcanic or biogenic methane exhalations, as well as the oxidation of crustal minerals and the enormous pool of dissolved iron in the oceans would have kept the air completely anoxic for quite some time before the rate of production of oxygen could overwhelm the rate of it being sequestered away in sediments as oxides or turned back into CO2.  The slowing of Earth’s geology as the interior of the planet cooled down leading to less volcanism or changes in the mineral nutrients available to drive different forms of metabolism as a result of this could have been confounding factors, changing when this tipping point was reached.

There is ample evidence of photosynthesis going on all over Earth long before the great oxidation, but it can be difficult to tell oxygenic and nonoxygenic photosynthesis apart unless you can get preserved chemicals from the cells themselves out of fossil microbial mats.  The older banded iron oxide formations from ancient seafloor may have been produced by non-oxygenic photosynthesis turning ferrous iron to rust, without the help of oxygen, or at the same time that oxygenic photosynthesis was also oxidizing iron indirectly.  Molecular biomarkers from preserved microbial mats have suggested cyanobacteria were definitely around by 2.7 billion years ago, and in 2014 evidence came to light in the form of various metal oxides in the rock record that certain shallow marine settings covered in microbial mats were getting oxidized before the ocean basins as a whole up to 3 billion years ago (see Planavsky et al., 2014: http://www.nature.com/ngeo/journal/v7/n4/full/ngeo2122.html).  Fossilized microbial mats consistent with an origin from photosynthesis of some sort are seen far before even then, though.

Stromatolites are bulbous formations of photosynthesizing bacteria, trapped sediment, and crystallized minerals excreted by the bacteria.  They only appear when grazing animals are completely absent, and are exceedingly rare today but show up all through the rock record of early Earth.  The oldest unequivocal evidence for photosynthesis of any type was, until recently, 3.5 gigayear old fossil stromatolites seen in Australia (the oldest pieces of the Earth’s crust that survive to this day can be found in Australia, Northern Canada, and Greenland).  But just this August, previously unseen rock strata revealed in Greenland by retreating ice have been found to contain a new deposit bearing what are believed to be the oldest known stromatolites in the world, at 3.7 gigayears old (see Nutman et al., 2016, ‘Rapid emergence of life shown by discovery of 3,700 million year old microbial structures’ at http://www.nature.com/nature/journal/v537/n7621/full/nature19355.html) (popular press: https://www.washingtonpost.com/news/speaking-of-science/wp/2016/08/31/3-7-billion-year-old-fossils-may-be-the-oldest-signs-of-life-on-earth/).

Oldest known stromatolites, layered microbial fossils created by photosynthetic microbial mats growing towards light and trapping sediment.  Figure 1 reproduced from Nutman et al., 2016.

As photosynthesis is a very complicated process, oxygenic or non, it’s striking that these structures were well established by 3.7 gigayears ago.  The entire solar system is about 4.6 gigayears old, and there’s precious little rock on Earth that has survived the cycles of plate tectonics and geologic recycling back to 3.7 gigayears ago.  This is an absolute MINIMUM age for a well established, photosynthetic, high-biomass biosphere that was transforming a lot of matter and energy, as it would be very difficult to find evidence if this was happening earlier.  Life got going FAST, and it is the preservation of evidence of it that is the factor that keeps limiting our knowledge of its age.  I would bet money on photosynthesis being found to be significantly older than this latest discovery – the earliest known date DID just slip back by 200 megayears after all, and there are equivocal traces of biogenic carbon in the tiny grains of older rocks that have been preserved that not everyone believes going all the way back to 4.3 gigayears ago (!).

In short, photosynthesis in general goes back all the way to the edge of our ability to look for it in some of the oldest coherent, non-ground-up rocks that we can look for microbial structures in and we have probably not yet found its true age.  The origin of oxygenic photosynthesis is fuzzier.  It could be a relative latecomer stitched together by horizontal gene transfer, or it could have come from one of the first microbes to use photosystems, with most other photosynthetic or phototrophic microbes losing the full set of pieces that were stitched together to create that pathway.


So, is photosynthesis and later oxygenic photosynthesis a weird unlikely event, or something that you’d expect in any biosphere?  The fact that there are two separate origins of phototrophy, getting energy from light, argues to me that such a great energy source WILL be tapped anywhere there are living things and sunlight in the same place.  The photosystem-driven form is the only form that gave rise to photosynthesis, however.  Does that mean that this is a rare event on cosmic scales?  Probably not, though I can’t say with certainty.

All photosynthetic organisms use fantastically sophisticated machinery, with little to nothing in the way of intermediate forms that show another independent elaboration of a simpler, worse starting point.  This suggests that once even rudimentary photosynthesis was established, it was souped up to full efficiency and effectiveness very quickly with little opportunity for diversification of ‘half-finished’ lineages, and that the ‘complete’ lineage then radiated rapidly into all the various forms we see today.  This could’ve represented a strong ‘first mover’ advantage, where any newcomers with very bad rudimentary photosynthesis would be outcompeted in environments where photosynthesis were possible by the well-established old guard of efficient photosynthesizers.  I really have no idea how to rigorously tell apart a circumstance in which the first-mover advantage prevents another evolution of sophisticated photosynthesis, and a circumstance in which a fantastically rare evolution of a complicated system happened to occur here and take over the world, though I strongly favor the former due to the lack of half-built intermediate forms and the apparent age of the pathway.

Building phylogenetic trees of bacteria to understand their relationship with each other by analyzing sequence data is a very difficult proposition and not my area of expertise – they trade genes back and forth with each other like mad, passing enzymes around and taking them up from their neighbors.  “Species” is a dicey concept for them, as the complement of all genes present in every member of a given species can be larger than the number of genes in any given individual by a factor of 3.  Most people who do bacterial taxonomy thus focus on a very particular set of genes – those of the protein translation system, which are very resistant to horizontal transfer.  So now, I’m probably going to severely anger any microbial taxonomists in my audience and make a claim based on my analysis of a recent evolutionary tree created from thousands of sequenced microbial genomes (Hug et al., 2016 “A new view of the tree of life” in Nature Microbiology, http://www.nature.com/articles/nmicrobiol201648)

Recent reconstruction of the full tree of life using new sequence analysis and thousands of microbial genomes.  Archaea and eukaryotes branch together below, bacteria above.  Red dots indicate bacteria no one has ever cultured and which are only known from genome sequence data in the last decade or so.  LUCA lies somewhere in the long branch between the bacteria and the archaea/eukaryotes. Figure 1 reproduced from Hug et al., 2016.

This tree will get a lot more analysis in later posts.  But for now, within the Bacterial radiation in the upper half of the tree, I note that the Cyanobacteria, Chloroflexi, several branches within the proteobacteria, the Acidobacteria, and Chlorobi – various photosynthetic lineages with different variations on photosynthesis of the photosystem style – are widely separated along the tree.  This suggests that either photosystem-based photosynthesis underwent repeated massive horizontal transfer among the bacteria – possibly difficult for a large complex system and also allowing a later origin for oxygenic photosynthesis, but possible – or it actually originated very very deep near the base of the bacterial tree, very long ago, and most lineages just lost it and specialized into eating organic molecules created by photosynthesizers or going back to chemosynthesis.  Or that the tree’s topology is wrong, of course.

In conclusion, I think it’s clear from its multiple origins that phototrophy, using light for energy, is likely to show up anywhere there is light and life.  I strongly suspect, but cannot rigorously prove, that photosynthesis of biomass was a very early development in life on Earth near the root of the Bacteria and just produced a very strong first-mover advantage crowding out secondary origins of it, and would probably also show up where there is life and light.  As for oxygen-producing photosynthesis, its origin from more mundane forms of photosynthesis is still being studied.  It required a strange chaining together of multiple modes of photosynthesis to make it work, and only ever happened once.  Its time of emergence, early or late, is pretty unconstrained and I don’t think there’s sufficient evidence to say one way or another if it is likely to happen anywhere there is photosynthesis.  It could be subject to the same sort of ‘first mover advantage’ situation that other photosynthesis may have encountered as well.  But whatever the case once it got going, it would naturally take over biomass production and crowd out other forms of photosynthesis due to its inherent chemical advantages on any wet planet and its effects suppressing other forms of photosynthesis.

Oxygen in the atmosphere had some important side effects, one which most people care about being allowing big complicated energy-gobbling organisms like animals – all that energy that organisms can get burning biomass in oxygen lets organisms that do so do a lot of interesting stuff.  Looking for oxygen in the atmospheres of other terrestrial planets would be an extremely informative experiment, as the presence of this substance would suggest that a process very similar to the process that created our huge diverse and active biosphere were underway.


In the week since I posted this, I’ve been pointed to some recent amazing work from the last five years, in journals that I don’t frequent much, supporting the idea that photosynthesis is very ancient.  I will link to them below.  The end result of recent work by people who study photosynthesis specifically suggests that the two different photosystems did in fact originate in the same cell via a duplication, and that cyanobacteria are just the only photosynthetic lineage that kept both rather than combining them horizontally later.  On top of this, looking at the evolution of the photosystems and the enzymes that make the various pigments suggests that most of the photosynthetic lineages inherited everything vertically from their ancestors rather than acquiring them horizontally, and in particular that cyanobacteria never acquired any of these things horizontally.

The fact that most of the photosynthetic lineages inherited photosynthesis vertically along with the topology of most suggested bacterial trees suggests that an actual majority of bacterial groups are descended from photosynthesizers.  This puts photosystem-based photosynthesis very close to the root of the bacterial tree, and very early in the history of life on Earth, bolstering the idea that the origin of photosynthesis was relatively easy but crowded out second origins of this process because the original pathway was so much better than any new origins that would have started out very bad at it.  Oxygen producing photosynthesis is still unclear, since nobody really knows how long ago the two photosystems were chained together to break water.  On the one hand, everything needed to create oxygenic photosynthesis was around quite early in the same cell, on the other hand it only arose once and the case for the crowding out of secondary origins is not as clear.


Cardona T, 2016, Origin of Bacteriochlorophyll a and the Early Diversification of Photosynthesis., PLoS One, Vol: 11

Cardona T, 2015, A fresh look at the evolution and diversification of photochemical reaction centers., Photosynth Res, Vol: 126, Pages: 111-134

Cardona T, 2016, Reconstructing the Origin of Oxygenic Photosynthesis: Do Assembly and Photoactivation Recapitulate Evolution?, Frontiers in Plant Science, Vol: 7

Blankenship RE. 2010. Early evolution of photosynthesis. Plant Physiol. 154:434–38

The Solar System: Why Earth?

Welcome to the new “Great A’Tuin”!   Blogger was proving unworkable, and getting my inevitable graphs to work right was completely impossible with their templates.  Wordpress it is.

So after another entirely too long hiatus, I’m back.  This time even more intense work on my PhD ate my time, along with a number of personal things.  In whatever case, I didn’t exactly have much time to write for myself over the last few months.  I’m almost glad though – the last year or so has seen a positive EXPLOSION of amazing origin of life research and I can’t wait to pick through it on the record.

But for now before jumping into origin of life research I think I have to instead talk about the Earth itself for a while.  So far I’ve talked about the position of Earth’s biosphere in the extremely large context of the history of the universe, our position in time relative to the formation of stars and planets and our position in space relative to different galaxies.  This has been informative, but we are necessarily working with very little information and coarse scales here.  By comparison within our own solar system there a massive wealth of information that we have nonetheless only barely started to look at.  By looking at the history of Earth and comparing it to other objects in our own solar system, I think some very important principles driving the appearance of biospheres like ours become clear and some very important questions we do not know the answers to fall out.

Earth is a very special place.  It is a world utterly out of chemical equilibrium.

That is not to say that other worlds in our solar system are in equilibrium – equilibrium is stasis and death, the lack of any energy flow from concentrated sources to diffuse sinks.  The atmospheres of Venus and the gas giants act as vast heat engines, transferring the energy of their daylit sides to the nightside and the poles creating winds and clouds in the process.  Geology driven by radioactive decay and primordial heat of formation deep inside solid worlds turns over rock through volcanoes and drives chemical cycling of elements into the atmosphere and back into rock.  But Earth is a world apart in its disequilibrium.  Our atmosphere and upper geosphere are charged up with energy, all this oxygen mixed with methane just itching to oxidize on decadal timescales.  The ground itself is full of geologically dredged-up iron and other substances constantly sucking oxygen out of the air on rather longer timescales.  And that is to say nothing of all the highly flammable carbon, biomass, ripped out of CO2 and reduced from that highly oxidized form to all kinds of substances and then left laying around or buried.  Anyone with a good enough spectrometer, looking at the Earth across the solar system or even from another star if their instruments were good enough could tell something strange was going on here.  A very dynamic, active process transducing lots of energy and utterly remaking the atmosphere and geochemistry for billions of years, creating an extraordinarily reactive atmosphere and oxidizing the crust to great depth.

It’s this complete transformation of Earth and only Earth that I think can be explained much more simply than most people think.

Proponents of the ‘rare-Earth hypothesis’ like to point to everything unique about Earth in our solar system and suggest that unless every single aspect of our world were recapitulated elsewhere, you wouldn’t get a big happy biosphere like ours.  I’m not a big fan of this approach.  Every body in the solar system is the product of a unique history and every body in the universe will be unique if you look close enough.  If you look at enough properties, eventually you will convince yourself that the particular combination is unlikely to be found elsewhere and you will probably be right.  Be it the large moon birthed in a collision that may have temporarily vaporized a significant fraction of the proto-Earth’s mantle, plate tectonics smoothing the carbon cycle and delivering fresh nutrients to the surface constantly, or its particular amount of water, Earth has many unique properties.  But with exactly one known biosphere to go on, you run a very real risk of overfitting your models to that one data point.  We really cannot say with any certainty which of these properties might be necessary to create a biosphere in another solar system, or how common such sets of properties could be.

I think we can be more confident when we compare Earth to other objects in our solar system where we have more information.  The conditions in this cluster of worlds are diverse, but there is exactly one known biosphere orbiting the Sun.  Emphasis on ‘known’ – I will argue in a moment that our knowledge in this area is absurdly incomplete and there could be half a dozen biospheres in our own solar system that we would never have noticed with the science done so far.  Still, ultimately, I would say Earth is unique in exactly one way that matters for any biology and has driven its evolution for at least 3.5 gigayears:

Earth is the only place in the solar system where solvents and clement temperatures meet diverse small-molecule feedstocks and minerals in the presence of large amounts of sunlight.

There’s several things going on here.  The first few are what most people think of when they talk about the presence of life on a planet: an environment in which something we would call ‘life’ is chemically possible.  The question of what exactly ‘life’ is is a complicated one and one I’ll address when talking about its origin at some point, but for now I’m calling it complicated organic chemistry that can carry heredity and dissipate energy in its environment to do its business.

To allow the kinds of organic chemistry needed by life as we know it, you need a few things in the environment.  Firstly, temperature and solvent – it needs to be warm enough for reactions to proceed with some speed and for solvents to be liquid at least some of the time, but not so hot that large complex molecules you need for catalysis and heredity break down into their constituent parts.  Life as we know it seems to have a hard limit of ~120 Celsius on the high side, and rather below freezing in the presence of specialized antifreeze chemicals on the low side even if living things can lay dormant doing nothing when they’re much colder.  Secondly, small-molecule feedstocks.  All life on Earth ultimately builds its biomolecules from simple, inorganic molecules – H2O, CO2, and N2 for the vast majority of biomass on Earth.  Anything that eats organic molecules ultimately, if you follow the food webs, will get them from something fixing carbon into biomass from CO2, and very nearly all nitrogen in protein ultimately derives from the pool of N2 in the same air.  Third, minerals.  No living thing on Earth can do without mineral nutrients.  Our genetic material itself contains huge amounts of phosphate, an inorganic ion leached from rocks, and almost every functional energy metabolism on the planet depends completely on electrons hopping along beautifully orchestrated chains of iron, sulfur, copper, and molybdenum ions clutched by proteins that are really just acting as scaffolds for them rather than enzymes.  Even if we didn’t need all that calcium in our bones, minerals are needed as catalysts and components of basic biomolecules.

Last comes what I think is far too often overlooked: energy.  All this complex chemistry doesn’t just happen.  A reaction that is thermodynamically favorable – releasing energy in the form of heat or introducing entropy by moving something from high concentration to low – will happen spontaneously, but before too long everything that can happen has happened and everything stops.  To drive complex chemistry and the production of biomolecules, there has to be energy flux into the system, a disequilibrium to be tapped.  And this is where Earth shines.  Other places in our solar system have liquid solvents, small molecule feedstocks, minerals, or all three.  But there is nowhere else in the solar system that has all those material requirements, PLUS the flux of over a kilowatt of energy per square meter the sun pours down onto the surface of Earth where they all meet.

The surface of Mars and the cloudtops of venus get plenty of sunlight, but Mars is nearly vacuum-dessicated and UV-radiation-blasted while Venus’s clouds are lacking in anything resembling a mineral surface within 70 kilometers even though sulfuric acid might be a workable biological solvent for something that evolved in it.  The icy moons of the outer solar system have plenty of liquid water underground at clement temperatures full of dissolved minerals and feedstocks, but these clement environments are all under up to kilometers of ice.  Even on Titan, where you might imagine some kind of very low-temperature reactions happening in hydrocarbon solvents, the sunlight at the top of the clouds is something like 1% as bright as here and under the cloud deck it’s more like 0.1%.

But on Earth, you have solvent falling from a sky made out of every small molecule feedstock you could want onto mineral surfaces bathed in a kilowatt per square meter of energy.  And photosynthesis capturing this vast energy flux is ultimately what makes the Earth’s biosphere what it is, splitting water into oxygen and building biomass by combining the resultant hydrogen with CO2 and N2.  It is what has transformed the planet so completely you could tell it was alive from light-years away if you could get a quick glimpse of its atmosphere.

I promised when I started this blog to talk about actual observables, what we can know and what we can’t with the information actually at hand.  In that spirit, after talking about how Earth is so special when it comes to biology in our solar system I need to insert a vital caveat.

There could be half a dozen active biospheres in this solar system right now and we would never know it with the information at hand.

A distinction has to be made between the presence of life, and the presence of a huge high-energy high-biomass biosphere like that of the Earth that chemically transforms a world.  There are plenty of places on Earth that have every attribute I talked about above except sunlight.  Fifty years ago you might have assumed that without sunlight to drive the primary producers of biomass there would be no life there – and as we have seen recently, you would have been wrong.

Sunlight is a vast, concentrated energy source as biological energy sources go: 170,000 terawatts hitting the Earth at all times is NOT shabby, and even if photosynthesis often only captures a small fraction of that it drives the vast majority of the metabolism on Earth.  But in recent decades, the discovery of organisms creating biomass from CO2 using energy not derived from the sun has shown that photosynthesis is not the only biological energy source on Earth.  Microbes can be found kilometers under the surface of the continents and the ocean, and a large fraction of the biomass of the planet may be living at very low cell densities and metabolic rates kilometers underground where they have no interaction with sunlight or energy derived from it at all.  To quote Jan Amend, a geochemist at the University of Southern California, “We keep digging and digging and digging deeper and have not hit the bottom of the biosphere.”

Photosynthesis and related activities (i.e. us) on the surface of the Earth definitely represents the majority of the metabolic activity of the planet.  But it is NOT all there is, and perhaps more importantly, given how complicated a process photosynthesis in all its forms is it can not have been how the first life on Earth got its energy.  Something else has to have been the energy source for the earliest life.

Chemolithotrophs, organisms that fix CO2 into biomass like plants but using energy from small chemical disequilibria within rock to do it, have been found kilometers deep under the continents.  Methanogens and acetogens, organisms that take H2 and oxidize it with CO2 into methane and acetate for their energy (and may have a key role to play in the origin of life on Earth – more on that in a future post) are found anywhere biological processes create H2 but also deep on the bottom of the ocean, living off  geological processes that make H2.  The total wattage available to these organisms is constrained.  I am unsure how to quantify it precisely, but given sheer thermodynamics it probably has to be comfortably less than the estimated geological heat flux of the Earth (about 47 terawatts, ~0.03% of what the planet gets from the Sun) plus a little extra for chemical reactions that occur at the mouths of certain types of hydrothermal vents, but the discoveries in this new sector of the biosphere just keep coming.


Pictured above is Desulforudis audaxviator, image taken from the Microbe Wiki (https://microbewiki.kenyon.edu/index.php/Desulforudis_audaxviator).  This bacterium was discovered kilometers underground in an anoxic aquifer at a pH of 9.3 and a temperature of 60 C.  It dies from the tiniest whiff of oxygen, and carries out all the reactions necessary to take rock and N2 and CO2 and turn it into biomass, functions that can be spread out across a dozen species in a surface ecosystem.  It is believed to live off the energy of radioactive decay in the rocks around it that splits water and creates the tiniest of chemical disequlibria for it to insert itself into as a middleman in their dissipation.

This planet has been crawling with scientists for a few hundred years, and swarming with pretty-damn-smart people for two hundred thousand years before that.  D. audaxviator was discovered in 2005.  These non-solar-driven living things are very easy to miss.  They can be detected with the latest molecular biology techniques because we know exactly what we are looking for, chemicals that are shared by all terrestrial living things that we have learned to detect at the single-molecule level, and because of recent advances in telling apart geochemistry from biochemistry which is not always as straightforward as it appears.

What have we done on other worlds in our own solar system compared to the massive, systematic exploration that was needed to find these things on  Earth?  It’s very hard to do science somewhere by dropping a few kilograms of automated scientific instruments from the sky every few years that cost well over their weight in gold and have severe bandwidth constraints.  Big things are being missed all the time, let alone small things.  It took until 2008 to figure out a basic, extremely important fact about the Martian soil – the fact that it contains up to 0.5% extremely reactive (and toxic) perchlorate created by the interaction of radiation and ancient salt deposits.  Every result from every instrument that probed and sampled the Martian soil from the Viking landers in the 1970s onwards had to be reinterpreted in the light of this finding and it was only conclusively discovered in the first place because one of the Phoenix lander’s instruments basically malfunctioned in the presence of the unexpected substance.  The geysers of Enceladus, discovered in 2004 when the Cassini probe reached Saturn, spew the ocean of that tiny geologically active moon into space where it can be sampled.  The instruments on Cassini are not sensitive enough to resolve the composition in all but the most general of terms – I have been to a talk in which one of the head scientists of the mission shrugged while pointing at a graph from the mass spec and said “there are molecules with at least five carbons in there somewhere.”

Would we ever detect the presence of D. audaxviator deep underground at Mars, or microbes living in hydrothermal vents within Europa or Enceladus from this kind of data?  At this point, I really don’t think so. By my count, there are at least 6 places in our own solar system with everything necessary for a low-biomass biosphere and the origin of life (again more on this later) that we simply couldn’t detect with the data at hand – underground at Mars, the oceans of Europa, the oceans of Ganymede, the deep underground water oceans of Titan, the surface hydrocarbon lakes of Titan, and the oceans of Enceladus.  Count me in  halfway for more speculative ideas about the cloudtops of Venus (where the limiting factor would be availability of minerals and not getting plunged down into the sterilizing depths of the atmosphere) and potential oceans within other icy moons and Kuiper belt objects like Pluto and Eris.  It’s not inconceivable that subsurface oceans could host the majority of biospheres in the universe by number, if not necessarily by mass.  We don’t know if there are biospheres in these places, but with current data we can’t know.  The answer is just insufficiently constrained.

We have only just gotten to the good part of solar system exploration.  It wasn’t that many decades ago that the planets were only small discs through telescopes to us with rudimentary maps if any.  Now they are worlds, and we finally know enough about them and about Earth itself to actually start asking the really interesting questions and to start looking for things that are hard to find.  The presence or the absence of another biosphere in our solar system would be extremely informative.  A second origin of life in our solar system would suggest that biospheres are extremely common, even if you need special circumstances for them to explode in scale and remake a world. Only one origin in this system would be a little data in favor of the origin of life being tougher, but we need a LOT of information before we would be able to say that.  Proving a negative is difficult to say the least, and proving that there was never a biosphere elsewhere in our solar system that died out later is even harder.

Apparently every time I write for this blog, I wind up producing huge essays.  Up next, I want to talk about the history of life on Earth and its main developments over time and what they may (or may not) tell us about the types of biospheres that could exist elsewhere.

What’s all this about?

NOTE:  This is a repost from my original site at blogger.

This blog is to be a repository for the thoughts and analysis I’ve accrued over the years on the topic of astrobiology, and the place of life and intelligence in the universe.  All my life I’ve been pulled to the very large and the very small.  Life has always struck me as the single most interesting thing on Earth, with its incredibly fine structure and vast, amazing history and fantastic abilities.  At the same time, the vast majority of what exists is NOT on Earth.  Going up in size from human-scale by the same number of orders of magnitude as you go down through to get to a hydrogen atom, you get just about to Venus at its closest approach to Earth – or one billionth the distance to the nearest star.  The large is much larger than the small is small.  On top of this, we now know that the universe as we know it is much older than life on Earth.  And we know so little of the vast majority of the universe.

There’s a strong tendency towards specialization in the sciences.  These days, there pretty much has to be for anybody to get anywhere.  Much of the great foundational work of physics was done on tabletops, and the law of gravitation was derived from data on the motions of the planets taken without the benefit of so much as a telescope.  All the low-hanging fruit has been picked.  To continue to further knowledge of the universe, huge instruments and vast energies are put to bear in astronomy and physics.  Biology is arguably a bit different, but the very complexity that makes living systems so successful and so fascinating to study means that there is so much to study that any one person is often only looking at a very small problem.

This has distinct drawbacks.  The universe does not care for our abstract labels of fields and disciplines – it simply is, at all scales simultaneously at all times and in all places.  When people focus narrowly on their subject of interest, it can prevent them from realizing the implications of their findings on problems usually considered a different field.

It is one of my hopes to try to bridge some gaps between biology and astronomy here.  I very nearly double-majored in biology and astronomy in college; the only thing that prevented this (leading to an astronomy minor) was a bad attitude towards calculus.  As is, I am a graduate student studying basic cell biology at a major research university, who nonetheless keeps in touch with a number of astronomer friends and keeps up with the field as much as possible.  I quite often find that what I hear and read about has strong implications for questions of life elsewhere in the universe, but see so few of these implications actually get publicly discussed. All kinds of information shedding light on our position in space and time, the origins of life, the habitability of large chunks of the universe, the course that biospheres take, and the possible trajectories of intelligences seem to me to be out there unremarked.

It is another of my hopes to try, as much as is humanly possible, to take a step back from the usual narratives about extraterrestrial life and instead focus from something closer to first principles.  What we actually have observed and have not, what we can observe and what we cannot, and what this leaves open, likely, or unlikely.  In my study of the history of the ideas of extraterrestrial life and extraterrestrial intelligence, all too often these take a back seat to popular narratives of the day.  In the 16th century the notion that the Earth moved in a similar way to the planets gained currency and lead to the suppositions that they might be made of similar stuff and that the planets might even be inhabited.  The hot question was, of course, if their inhabitants would be Christians and their relationship with God given the anthropocentric biblical creation stories.  In the late 19th and early 20th century, Lowell’s illusory canals on Mars were advanced as evidence for a Martian socialist utopia.  In the 1970s, Carl Sagan waxed philosophical on the notion that contacting old civilizations might teach us how to save ourselves from nuclear warfare.  Today, many people focus on the Fermi paradox – the apparent contradiction that since much of the universe is quite old, extraterrestrials experiencing continuing technological progress and growth should have colonized and remade it in their image long ago and yet we see no evidence of this.  I move that all of these notions have a similar root – inflating the hot concerns and topics of the day to cosmic significance and letting them obscure the actual, scientific questions that can be asked and answered.

Life and intelligence in the universe is a topic worth careful consideration, from as many angles as possible.  Let’s get started.