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Directed panspermia concerns the deliberate transport of microorganisms in space to be used as introduced species on lifeless planets. Directed panspermia may have been sent to Earth to start life here, or may be sent from Earth to seed exoplanets with life.
Historically, Shklovskii and Sagan (1966) and Crick and Orgel (1973) hypothesized that life on Earth may have been seeded deliberately by other civilizations. Conversely, Mautner and Matloff (1979) and Mautner (1995, 1997) proposed that we ourselves should seed new planetary systems, protoplanetary discs or star-forming clouds with microorganisms, to secure and expand our organic gene/protein life-form. To avoid interference with local life, the targets may be young planetary systems where local life is unlikely. Directed panspermia can be motivated by biotic ethics that value the basic patterns of organic gene/protein life with its unique complexity and unity, and its drive for self-propagation.
Belonging to life then implies panbiotic ethics with a purpose to propagate and expand life in space. Directed panspermia for this purpose is becoming possible due to developments in solar sails, precise astrometry, the discovery of extrasolar planets, extremophiles and microbial genetic engineering. Cosmological projections suggests that life in space can then have an immense future.
- 1 History and motivation
- 2 Strategies and targets
- 3 Propulsion and launch
- 4 Astrometry and targeting
- 5 Deceleration and capture
- 6 Biomass requirements
- 7 Biological payload
- 8 Advanced missions
- 9 Motivation and ethics
- 10 Objections and counterarguments
- 11 See also
- 12 References
- 13 External links
History and motivation
An early example of the idea of directed panspermia dates to the early science fiction work Last and First Men by Olaf Stapledon, first published in 1930. It details the manner in which the last humans, upon discovering that the Solar System will soon be destroyed, send microscopic "seeds of a new humanity" towards potentially habitable areas of the universe.
In 1966 Shklovskii and Sagan proposed that life on Earth may have been seeded through directed panspermia by other civilisations. and 1973 Crick and Orgel also discussed  Conversely, Mautner and Matloff proposed in 1979, and Mautner examined in detail in 1995 and 1997 the technology and motivation to secure and expand our organic gene/protein life-form by directed panspermia missions to new planetary systems, protoplanetary discs and star-forming clouds. Technological aspects include propulsion by solar sails, deceleration by radiation pressure or viscous drag at the target, and capture of the colonizing micro-organisms by planets. A possible objection is potential interference with local life at the targets, but targeting young planetary systems where local life, especially advanced life, could not have started yet, avoids this problem. Directed panspermia may be motivated by the desire to perpetuate the common genetic heritage of all terrestrial life. This motivation was formulated as biotic ethics that value the common gene/protein patters of our family of organic life, and as panbiotic ethics that aim to secure and expand life in the universe.
Strategies and targets
Directed panspermia may be aimed at nearby young planetary systems such as Alpha PsA (25 ly (light-years) away) and Beta Pictoris (63.4 ly), both of which show accretion discs and signs of comets and planets. More suitable targets may be identified by space telescopes such as the Kepler mission that will identify nearby star systems with habitable planets. Alternatively, directed panspermia may aim at star-forming interstellar clouds such as Rho Ophiuchi cloud complex (427 ly), that contains clusters of new stars too young to originate local life (425 infrared-emitting young stars aged 100,000 to a million years). Such clouds contain zones with various densities (diffuse cloud < dark fragment < dense core < protostellar condensation < accretion disc) that could selectively capture panspermia capsules of various sizes.
Habitable planets or habitable zones about nearby stars may be targeted by large (10 kg) missions where microbial capsules are bundled and shielded. Upon arrival, microbial capsules in the payload may be dispersed in orbit for capture by planets. Alternatively, small microbial capsules may be sent in large swarms to habitable planets, protoplanetary discs, or zones of various density in interstellar clouds. The microbial swarm provides minimal shielding but does not require high precision targeting, especially when aiming at large interstellar clouds.
Propulsion and launch
Panspermia missions should deliver microorganisms that can grow in the new habitats. They may be sent in 10−10 kg, 30 micrometer radius capsules that allow intact atmospheric entry at the target planets, each containing 100,000 diverse microorganisms suited to various environments. Both for bundled large mass missions and microbial capsule swarms, solar sails may provide the most simple propulsion for interstellar transit. Spherical sails will avoid orientation control both at launch and at deceleration at the targets. For bundled shielded missions to nearby star systems, solar sails with thicknesses of 10−7 m and areal densities of 0.0001 kg/m2 seem feasible, and sail/payload mass ratios of 10:1 will allow exit velocities near the maximum possible for such sails. Sails with about 540 m radius and area of 106 m2 can impart 10 kg payloads with interstellar cruise velocities of 0.0005 c (1.5x105 m/s) when launched from 1 au (astronomical unit). At this speed, voyage to the Alpha PsA star will last 50,000 y, and to the Rho Opiuchus cloud, 824,000 years.
At the targets, the microbial payload would decompose into 1011 (100 billion) 30 µm capsules to increase the probability of capture. In the swarm strategy to protoplanetary discs and interstellar clouds, 1 mm radius, 4.2x10−6 kg microbial capsules are launched from 1 au using sails of 4.2x10−5 kg with radius of 0.37 m and area of 0.42 m2 to achieve cruising speeds of 0.0005 c. At the target, each capsule decomposes into 4,000 delivery microcapsules of 10−10 kg and of 30 micrometer radius that allow intact entry to planetary atmospheres. For missions that do not encounter dense gas zones, such as interstellar transit to mature planets or to habitable zones about stars, the microcapsules can be launched directly from 1 au using 10−9 kg sails of 1.8 mm radius to achieve velocities of 0.0005 c to be decelerated by radiation pressure for capture at the targets. The 1 mm and 30 micrometer radius vehicles and payloads needed in large numbers for both the bundled and swarm missions. These capsules and the miniature sails for swarm missions can be mass manufactured readily.
Astrometry and targeting
The panspermia vehicles would be aimed at moving targets whose locations at the time of arrival must be predicted. This can be calculated using their measured proper motions, their distances, and the cruising speeds of the vehicles. The positional uncertainty and size of the target object then allow estimating the probability that the panspermia vehicles will arrive at their targets. The positional uncertainty δy (m) of the target at arrival time is given by equation (1), where α(p) is the resolution of proper motion of the target object (arsec/year), d is the distance (m) and v is the velocity of the vehicle (m/s)
δy = 1.5x10−13 αpd2v
Given the positional uncertainty, the vehicles may be launched with a scatter in a circle about the predicted position of the target. The probability Ptarget for a capsule to hit the target area with radius rtarget (m) is the given by the ratio of the targeting scatter and the target area.
target = Atarget/π(δy)2 = 4.4x1025 rtarget2v2/(αp2d4)
To apply these equations, the precision of astrometry of star proper motion of 0.00001 parsec/year, and the solar sail vehicle velocity of 0.0005 c (1.5 x 105 m/s) may be expected within a few decades. For a chosen planetary system, the area Atarget may be the width of the habitable zone, while for interstellar clouds, it may be the sizes of the various density zones of the cloud.
Deceleration and capture
Solar sail missions to Sun-like stars can decelerate by radiation pressure in reverse dynamics of the launch. The sails must be properly oriented at arrival, but orientation control may be avoided using spherical sails. The vehicles must approach the target Sun-like stars at radial distances similar to the launch, about 1 au. After the vehicles are captured in orbit, the microbial capsules may be dispersed in a ring orbiting the star, some within the gravitational capture zone of planets. Missions to accretion discs of planets and to star-forming clouds will decelerate by viscous drag at the rate dv/dt as determined by equation (3), where v is the velocity, rc the radius of the spherical capsule, ρc is density of the capsule and ρm is the density of the medium.
dv/dt = -(3v2/2ρc) ρ m/rc
A vehicle entering the cloud with a velocity of 0.0005 c (1.5 x 105 m/s) will be captured when decelerated to 2,000 m/s, the typical speed of grains in the cloud. The size of the capsules can be designed to stop at zones with various densities in the interstellar cloud. Simulations show that a 35 micron radius capsule will be captured in a dense core, and a 1 mm radius capsule in a protostellar condensation in the cloud. As for approach to accretion discs about stars, a millimetre size capsule entering the 1000 km thick disc face at 0.0005 c will be captured at 100 km into the disc. Therefore 1 mm sized objects may be the best for seeding protoplanetary discs about new stars and protostellar condensations in interstellar clouds.
The captured panspermia capsules will mix with dust. A fraction of the dust and a proportional fraction of the captured capsules will be delivered to planets. Dispersing the payload into delivery microcapsules will increase the chance that some will be delivered to planets. Particles of 0.6 - 60 micron radius can remain cold enough to preserve organic matter during atmospheric entry to planets. Accordingly, each 1 mm, 4.2 x10−6 kg capsule captured in the viscous medium can be dispersed into 42,000 delivery microcapsules of 30 micron radius, each weighing 10−10 kg and containing 100,000 microbes. These objects will not be ejected from the dust cloud by radiation pressure from the star, and will remain mixed with the dust. A fraction of the dust, containing the captured microbial capsules, will be captured by planets, or captured in comets and delivered by them later to planets. The probability of capture, Pcapture, can be estimated from similar processes, such as the capture of interplanetary dust particles by planets in our Solar System, where 10−5 of the Zodiacal cloud maintained by comet ablation, and also a similar fraction of asteroid fragments, is collected by the Earth. The probability of capture of an initially launched capsule by a planet, Pplanet is given by the equation below, where Ptarget is the probability that the capsule reaches the target accretion disc or cloud zone, and Pcapture is the probability of capture from this zone by a planet.
Pplanet = Ptarget x Pcapture
The probability Pplanet depends on the mixing ratio of the capsules with the dust and on the fraction of the dust delivered to planets. These variables can be estimated for capture in planetary accretion discs or in various zones in the interstellar cloud.
After determining the composition of chosen meteorites, astroecologists performed laboratory experiments that suggest that many colonizing microorganisms and some plants could obtain most of their chemical nutrients from asteroid and cometary materials. However, the scientists noted that phosphate (PO4) and nitrate (NO3–N) critically limit nutrition to many terrestrial lifeforms. For successful missions, enough biomass must be launched and captured for a reasonable chance to initiate life at the target planet. An optimistic requirement is the capture by the planet of 100 capsules with 100,000 microorganisms each, for a total of 10 million organisms with a total biomass of 10−8 kg.
The required biomass to launch for a successful mission is given by following equation. mbiomass (kg) = 10−8 / Pplanet Using the above equations for Ptarget with transit velocities of 0.0005 c, the known distances to the targets, and the masses of the dust in the target regions then allows calculating the biomass that needs to be launched for probable success. With these parameters, as little as 1 gram of biomass (1012 microorganisms) could seed Alpha PsA and 4.5 gram could seed Beta Pictoris. More biomass needs to be launched to the Rho Ophiuchi cloud complex, mainly because its larger distance. A biomass on the order of 300 tons would need to be launched to seed a protostellar condensation or an accretion disc, but two hundred kilograms would be sufficient to seed a young stellar object in the Rho Ophiuchi cloud complex.
Consequently, as long as the required physical range of tolerance are met (e.g.: growth temperature, cosmic radiation shielding, atmosphere and gravity), lifeforms viable on Earth may be chemically nourished by watery asteroid and planetary materials in this and other planetary systems.
The seeding organisms need to survive and multiply in the target environments and establish a viable biosphere. Some of the new branches of life may develop intelligent beings who will further expand life in the galaxy. The messenger microorganisms may find diverse environments, requiring extremophile microorganisms with a range of tolerances, including thermophile (high temperature), psychrophile (low temperature), acidophile (high acidity), halophile (high salinity), oligotroph (low nutrient concentration), xerophile (dry environments) and radioresistant (high radiation tolerance) microorganisms. Genetic engineering may produce polyextremophile microorganisms with several tolerances. The target atmospheres will probably lack oxygen, so the colonizers should include anaerobic microorganisms. Colonizing anaerobic cyanobacteria may later establish atmospheric oxygen that is needed for higher evolution, as it happened on Earth. Aerobic organisms in the biological payload may be delivered to the planets later when the conditions are right, by comets that captured and preserved the capsules.
The development of eukaryote microorganisms was a major bottleneck to higher evolution on Earth. Including eukaryote microrganisms in the payload can bypass this barrier. Multicellular organisms are even more desirable, but being much heavier than bacteria, fewer can be sent. Hardy tardigrades (water-bears) may be suitable but they are similar to arthropods and would lead to insects. The body-plan of rotifers could lead to higher animals, if the rotifers can be hardened to survive interstellar transit.
Microorganisms or capsules captured in the accretion disc can be captured along with the dust into asteroids. During aqueous alteration the asteroids contain water, inorganic salts and organics, and astroecology experiments with meteorites showed that algae, bacteria, fungi and plant cultures can grow in the asteroids in these media. Microorganisms can then spread in the accreting solar nebula, and will be delivered to planets in comets and in asteroids. The microorganisms can grow on nutrients in the carrier comets and asteroids in the aqueous planetary environments, until they adapt to the local environments and nutrients on the planets.
Signal in the genome
A number of publications since 1979 have proposed the idea that directed panspermia could be demonstrated to be the origin of all life on Earth if a distinctive 'signature' message were found, deliberately implanted into either the genome or the genetic code of the first microorganisms by our hypothetical progenitor. In 2013 a team of physicists claimed that they had found mathematical and semiotic patterns in the genetic code which, they believe, is evidence for such a signature. Further investigations are needed.
Significantly, panspermia missions can be launched by present or near-future technologies. However, more advanced technologies may be also used when these become available. The biological aspects of directed panspermia may be improved by genetic engineering to produce hardy polyextremophile microorganisms and multicellular organisms, suitable to diverse planetary environments. Hardy polyextremophile anaerobic multicellular eukaryots with high radiation resistance, that can form a self-sustaining ecosystem with cyanobacteria, would combine ideally the features needed for survival and higher evolution.
For advanced missions, ion thrusters or solar sails using beam-powered propulsion accelerated by Earth-based lasers can achieve speeds up to 0.01 c (3 x 106 m/s). Robots may provide in-course navigation, may control the reviving of the frozen microbes periodically during transit to repair radiation damage, and may also choose suitable targets. These propulsion methods and robotics are under development.
Microbial payloads may be also planted on hyperbolic comets bound for interstellar space. This strategy follows the mechanisms of natural panspermia by comets, as suggested by Hoyle and Wikramasinghe. The microorganisms would be frozen in the comets at interstellar temperatures of a few kelvins and protected from radiation for eons. It is unlikely that an ejected comet will be captured in another planetary system, but the probability can be increased by allowing the microbes to multiply during warm perihelion approach to the Sun, then fragmenting the comet. A 1 km radius comet would yield 4.2 x 1012 one-kg seeded fragments, and rotating the comet would eject these shielded icy objects in random directions into the galaxy. This increases a trilion-fold the probability of capture in another planetary system, compared with transport by a single comet. Such manipulation of comets is a speculative long-term prospect.
Motivation and ethics
Directed panspermia aims to secure and expand our family of organic gene/protein life. It may be motivated by the desire to perpetuate the common genetic heritage of all terrestrial life. This motivation was formulated as biotic ethics, that value the common gene/protein patters of organic life, and as panbiotic ethics that aim to secure and expand life in the universe.
Molecular biology shows complex patterns common to all cellular life, a common genetic code and a common mechanism to translate it into proteins, which in turn help to reproduce the DNA code. Also, shared are the basic mechanisms of energy use and material transport. These self-propagating patterns and processes are the core of organic gene/protein life. Life is unique because of this complexity, and because of the exact coincidence of the laws of physics that allow life to exist. Also unique to life is the pursuit of self-propagation, which implies a human purpose to secure and expand life. These objectives are best secured in space, suggesting a panbiotic ethics aimed to secure this future.
The longevity of our space-faring technological society is uncertain, and it would be prudent to start a directed panspermia program promptly. This program can secure life and allow it to expand in space and in biodiversity with an immense future for trillions of eons.
Objections and counterarguments
The main objection to directed panspermia is that it may interfere with local life at the targets. The colonizing microorganisms may out-compete local life for resources, or infect and harm local organisms. However, this probability can be minimized by targeting newly forming planetary systems, accretion discs and star-forming clouds, where local life, and especially advanced life, could not have emerged yet. If there is local life that is fundamentally different, the colonizing microorganisms may not harm it. If there is local organic gene/protein life, it may exchange genes with the colonizing microorganisms, increasing galactic biodiversity.
Another objection is that space should be left pristine for scientific studies, a reason for planetary quarantine. However, directed panspermia may reach only a few, at best a few hundred new stars, still leaving a hundred billion pristine for local life and for research. A technical objection is the uncertain survival of the messenger organisms during long interstellar transit. Research by simulations, and the development on hardy colonizers is needed to address this questions.
- Mautner, Michael N. (2005). "Life in the cosmological future: Resources, biomass and populations". Journal of the British Interplanetary Society 58: 167–180. Bibcode:2005JBIS...58..167M.
- Mautner, Michael N. (2000). Seeding the Universe with Life: Securing Our Cosmological Future. Washington D. C.: Legacy Books (www.amazon.com). ISBN 047600330X.
- Stapledon, Olaf (2008). Last and first men (Unabridged republ. ed.). Mineola, N.Y.: Dover Publications. p. 238. ISBN 978-0486466828.
- Shklovskii, I. S.; Sagan, C. (1966). Intelligent life in the universe. New York: Dell. ISBN 978-1892803023.
- Crick, F. H.; Orgel, L. E. (1973). "Directed panspermia". Icarus 19: 341. Bibcode:1973Icar...19..341C. doi:10.1016/0019-1035(73)90110-3.
- Mautner, M.; Matloff, G. L. (1979). "A technical and ethical evaluation of seeding nearby solar systems". J. British Interplanetary Soc. 32: 419–423.
- Mautner, Michael N. (1995). "Directed Panspermia. 2. Technological Advances Toward Seeding Other Solar Systems, and the Foundations of Panbiotic Ethics". J. British Interplanetary Soc. 48: 435–440.
- Mautner, Michael N. (1997). "Directed panspermia. 3. Strategies and motivation for seeding star-forming clouds". J. British Interplanetary Soc. 50: 93–102.
- Mautner, Michael N. (2009). "Life-centered ethics and the human future in space". Bioethics 23: 433–440. doi:10.1111/j.1467-8519.2008.00688.x. PMID 19077128.
- Mezger, P. G. B. F. Burke, J. H. Rahe and E. E. Roettger, ed. "The search for protostars using millimetre/submillimeter dust emission as a tracer". Planetary Systems: Formation, Evolution and Detection: 208–220.
- Vulpetti, G.; Johnson, L.; Matloff, G. L. (2008). Solar Sails : A Novel Approach to Interplanetary Flight. New York: Springer. ISBN 978-0-387-34404-1.
- Anders, E. (1989). "Prebiotic organic matter from comets and asteroids". Nature 342 (6247): 255–257. Bibcode:1989Natur.342..255A. doi:10.1038/342255a0.
- Morrison, D. (1977). "Sizes and albedos of the larger asteroids". Comets, Asteroids and Meteorites: Interrelations, Evolution and Origins, A. H. Delsemme, ed., U. of Toledo Press: 177–183.
- Sekanina, Z. (1977). "Meteor streams in the making". Comets, Asteroids and Meteorites: Interrelations, Evolution and Origins, A. H. Delsemme, ed., U. of Toledo Press: 159–169.
- Weatherill, G. W. (1977). "Fragmentation of asteroids and delivery of fragments to Earth". Comets, Asteroids and Meteorites: Interrelations, Evolution and Origins, A. H. Delsemme, ed., U. of Toledo Press: 283–291.
- Kyte, F. T.; Wasson, J. T. (1989). "Accretion rate of exraterrestrial matter: Iridium deposited 33 to 67 million years ago". Science 232: 1225–1229. doi:10.1126/science.232.4755.1225.
- Mautner, Michael N. (2002). "Planetary bioresources and astroecology. 1. Planetary microcosm bioessays of Martian and meteorite materials: soluble electrolytes, nutrients, and algal and plant responses". Icarus 158: 72–86. Bibcode:2002Icar..158...72M. doi:10.1006/icar.2002.6841. PMID 12449855.
- Mautner, Michael N. (2002). "Planetary resources and astroecology. Planetary microcosm models of asteroid and meteorite interiors: electrolyte solutions and microbial growth. Implications for space populations and panspermia". Astrobiology 2: 59–76. Bibcode:2002AsBio...2...59M. doi:10.1089/153110702753621349.
- Olsson-Francis, Karen; Cockell, Charles S. (2010). "Use of cyanobacteria for in-situ resource use in space applications". Planetary and Space Science 58: 1279–1285. Bibcode:2010P&SS...58.1279O. doi:10.1016/j.pss.2010.05.005.
- G. Marx (1979). "Message through time". Acta Astronautica 6 (1-2): 221–225. doi:10.1016/0094-5765(79)90158-9.
- H. Yokoo, T. Oshima (1979). "Is bacteriophage φX174 DNA a message from an extraterrestrial intelligence?". Icarus 38 (1): 148–153. doi:10.1016/0019-1035(79)90094-0.
- Overbye, Dennis (26 June 2007). "Human DNA, the Ultimate Spot for Secret Messages (Are Some There Now?)". Retrieved 2014-10-09.
- Davies, Paul C.W. (2010). The Eerie Silence: Renewing Our Search for Alien Intelligence. Boston, Massachusetts: Houghton Mifflin Harcourt. ISBN 978-0-547-13324-9.
- V. I. shCherbak, M. A. Makukov (2013). "The "Wow! signal" of the terrestrial genetic code". Icarus 224 (1): 228–242. doi:10.1016/j.icarus.2013.02.017.
- Makukov, Maxim (4 October 2014). "Claim to have identified extraterrestrial signal in the universal genetic code thereby confirming directed panspermia.". Maxim Makukov. The New Reddit Journal of Science. Retrieved 2014-10-09.
- M. A. Makukov, V. I. shCherbak (2014). "Space ethics to test directed panspermia". Life Sciences in Space Research 3: 10–17. doi:10.1016/j.lssr.2014.07.003.
- Hoyle, F.; Wickramasinghe, C. (1978). Lifecloud: The Origin of Life in the Universe. London: J. M. Dent and Sons.
- Society for Life in Space (SOLIS) Interstellar Panspermia Society, for research and education on directed panspermia. Aims to launch directed panspermia missions in this century.
- Astro-ecology and resources for life in space. Experimental research on nutrients in asteroids and meteorites, and on microorganisms and plants that grow on these in-situ space resources.