History of the Earth
The history of the Earth concerns the development of the planet Earth from its formation to the present day. Nearly all branches of natural science have contributed to the understanding of the main events of the Earth's past. The age of Earth is approximately one-third of the age of the universe. An immense amount of biological and geological change has occurred in that time span.
Earth formed around 4.54 billion (4.54×109) years ago by accretion from the solar nebula. Volcanic outgassing probably created the primordial atmosphere, but it contained almost no oxygen and would have been toxic to humans and most modern life. Much of the Earth was molten because of frequent collisions with other bodies which led to extreme volcanism. One very large collision is thought to have been responsible for tilting the Earth at an angle and forming the Moon. Over time, the planet cooled and formed a solid crust, allowing liquid water to exist on the surface.
The first life forms appeared between 3.8 and 3.5 billion years ago. The earliest evidences for life on Earth are graphite found to be biogenic in 3.7-billion-year-old metasedimentary rocks discovered in Western Greenland and microbial mat fossils found in 3.48-billion-year-old sandstone discovered in Western Australia. Photosynthetic life appeared around 2 billion years ago, enriching the atmosphere with oxygen. Life remained mostly small and microscopic until about 580 million years ago, when complex multicellular life arose. During the Cambrian period it experienced a rapid diversification into most major phyla. Although more than 99 percent of all species that ever lived on the planet are estimated to be extinct, there are currently 10–14 million species of life on the Earth.
Geological change has been constantly occurring on Earth since the time of its formation and biological change since the first appearance of life. Species continuously evolve, taking on new forms, splitting into daughter species, or going extinct in response to an ever-changing planet. The process of plate tectonics has played a major role in the shaping of Earth's oceans and continents, as well as the life they harbor. The biosphere, in turn, has had a significant effect on the atmosphere and other abiotic conditions on the planet, such as the formation of the ozone layer, the proliferation of oxygen, and the creation of soil.
- 1 Geologic time scale
- 2 Solar System formation
- 3 Hadean and Archean Eons
- 4 Proterozoic Eon
- 5 Phanerozoic Eon
- 6 See also
- 7 Notes
- 8 References
- 9 Further reading
- 10 External links
Geologic time scale
The history of the Earth is organized chronologically in a table known as the geologic time scale, which is split into intervals based on stratigraphic analysis. A full-time scale can be found at the main article.
The following four timelines show the geologic time scale. The first shows the entire time from the formation of the Earth to the present, but this compresses the most recent eon. Therefore the second scale shows the most recent eon with an expanded scale. The second scale compresses the most recent era, so the most recent era is expanded in the third scale. Since the Quaternary is a very short period with short epochs, it is further expanded in the fourth scale. The second, third, and fourth timelines are therefore each subsections of their preceding timeline as indicated by asterisks. The Holocene (the latest epoch) is too small to be shown clearly on the third timeline on the right, another reason for expanding the fourth scale. The Pleistocene (P) epoch. Q stands for the Quaternary period.
Solar System formation
The standard model for the formation of the Solar System (including the Earth) is the solar nebula hypothesis. In this model, the Solar system formed from a large, rotating cloud of interstellar dust and gas called the solar nebula. It was composed of hydrogen and helium created shortly after the Big Bang 13.8 Ga (billion years ago) and heavier elements ejected by supernovae. About 4.5 Ga, the nebula began a contraction that may have been triggered by the shock wave of a nearby supernova. A shock wave would have also made the nebula rotate. As the cloud began to accelerate, its angular momentum, gravity and inertia flattened it into a protoplanetary disk perpendicular to its axis of rotation. Small perturbations due to collisions and the angular momentum of other large debris created the means by which kilometer-sized protoplanets began to form, orbiting the nebular center.
The center of the nebula, not having much angular momentum, collapsed rapidly, the compression heating it until nuclear fusion of hydrogen into helium began. After more contraction, a T Tauri star ignited and evolved into the Sun. Meanwhile, in the outer part of the nebula gravity caused matter to condense around density perturbations and dust particles, and the rest of the protoplanetary disk began separating into rings. In a process known as runaway accretion, successively larger fragments of dust and debris clumped together to form planets. Earth formed in this manner about 4.54 billion years ago (with an uncertainty of 1%) and was largely completed within 10–20 million years. The solar wind of the newly formed T Tauri star cleared out most of the material in the disk that had not already condensed into larger bodies. The same process is expected to produce accretion disks around virtually all newly forming stars in the universe, some of which yield planets.
The proto-Earth grew by accretion until its interior was hot enough to melt the heavy, siderophile metals. Having higher densities than the silicates, these metals sank. This so-called iron catastrophe resulted in the separation of a primitive mantle and a (metallic) core only 10 million years after the Earth began to form, producing the layered structure of Earth and setting up the formation of Earth's magnetic field. J. A. Jacobs  was the first to suggest that the inner core—a solid center distinct from the liquid outer core—is freezing and growing out of the liquid outer core due to the gradual cooling of Earth's interior (about 100 degrees Celsius per billion years).
Hadean and Archean Eons
The first eon in Earth's history, the Hadean, begins with the Earth's formation and is followed by the Archean eon at 3.8 Ga.:145 The oldest rocks found on Earth date to about 4.0 Ga, and the oldest detrital zircon crystals in rocks to about 4.4 Ga, soon after the formation of the Earth's crust and the Earth itself. The giant impact hypothesis for the Moon's formation states that shortly after formation of an initial crust, the proto-Earth was impacted by a smaller protoplanet, which ejected part of the mantle and crust into space and created the Moon.
From crater counts on other celestial bodies it is inferred that a period of intense meteorite impacts, called the Late Heavy Bombardment, began about 4.1 Ga, and concluded around 3.8 Ga, at the end of the Hadean. In addition, volcanism was severe due to the large heat flow and geothermal gradient. Nevertheless, detrital zircon crystals dated to 4.4 Ga show evidence of having undergone contact with liquid water, suggesting that the planet already had oceans or seas at that time.
By the beginning of the Archean, the Earth had cooled significantly. Most present life forms could not have survived in the Archean atmosphere, which lacked oxygen and an ozone layer. Nevertheless, it is believed that primordial life began to evolve by the early Archean, with candidate fossils dated to around 3.5 Ga. Some scientists even speculate that life could have begun during the early Hadean, as far back as 4.4 Ga, surviving the possible Late Heavy Bombardment period in hydrothermal vents below the Earth's surface.
Formation of the Moon
Earth's only natural satellite, the Moon, is larger relative to its planet than any other satellite in the solar system.[nb 1] During the Apollo program, rocks from the Moon's surface were brought to Earth. Radiometric dating of these rocks has shown that the Moon is 4.53 ± .01 billion years old, formed at least 30 million years after the solar system. New evidence suggests the Moon formed even later, 4.48 ± 0.02 Ga, or 70–110 million years after the start of the Solar System.
Theories for the formation of the Moon must explain its late formation as well as the following facts. First, the Moon has a low density (3.3 times that of water, compared to 5.5 for the earth) and a small metallic core. Second, there is virtually no water or other volatiles on the moon. Third, the Earth and Moon have the same oxygen isotopic signature (relative abundance of the oxygen isotopes). Of the theories that have been proposed to account for these phenomena, only one is widely accepted: The giant impact hypothesis proposes that the Moon originated after a body the size of Mars (sometimes named Theia) struck the proto-Earth a glancing blow.:256
The collision released about 100 million times more energy than the more recent Chicxulub impact that is believed to have caused the extinction of the dinosaurs. It was enough to vaporize some of the Earth's outer layers and melt both bodies.:256 A portion of the mantle material was ejected into orbit around the Earth. The giant impact hypothesis predicts that the Moon was depleted of metallic material, explaining its abnormal composition. The ejecta in orbit around the Earth could have condensed into a single body within a couple of weeks. Under the influence of its own gravity, the ejected material became a more spherical body: the Moon.
Mantle convection, the process that drives plate tectonics today, is a result of heat flow from the Earth's interior to the Earth's surface.:2 It involves the creation of rigid tectonic plates at mid-oceanic ridges. These plates are destroyed by subduction into the mantle at subduction zones. During the early Archean (about 3.0 Ga) the mantle was much hotter than today, probably around 1600 °C,:82 so convection in the mantle was faster. While a process similar to present day plate tectonics did occur, this would have gone faster too. It is likely that during the Hadean and Archean, subduction zones were more common, and therefore tectonic plates were smaller.:258
The initial crust, formed when the Earth's surface first solidified, totally disappeared from a combination of this fast Hadean plate tectonics and the intense impacts of the Late Heavy Bombardment. However, it is thought that it was basaltic in composition, like today's oceanic crust, because little crustal differentiation had yet taken place.:258 The first larger pieces of continental crust, which is a product of differentiation of lighter elements during partial melting in the lower crust, appeared at the end of the Hadean, about 4.0 Ga. What is left of these first small continents are called cratons. These pieces of late Hadean and early Archean crust form the cores around which today's continents grew.
The oldest rocks on Earth are found in the North American craton of Canada. They are tonalites from about 4.0 Ga. They show traces of metamorphism by high temperature, but also sedimentary grains that have been rounded by erosion during transport by water, showing rivers and seas existed then. Cratons consist primarily of two alternating types of terranes. The first are so-called greenstone belts, consisting of low grade metamorphosed sedimentary rocks. These "greenstones" are similar to the sediments today found in oceanic trenches, above subduction zones. For this reason, greenstones are sometimes seen as evidence for subduction during the Archean. The second type is a complex of felsic magmatic rocks. These rocks are mostly tonalite, trondhjemite or granodiorite, types of rock similar in composition to granite (hence such terranes are called TTG-terranes). TTG-complexes are seen as the relicts of the first continental crust, formed by partial melting in basalt.:Chapter 5
Oceans and atmosphere
Earth is often described as having had three atmospheres. The first atmosphere, captured from the solar nebula, was composed of light (atmophile) elements from the solar nebula, mostly hydrogen and helium. A combination of the solar wind and Earth's heat would have driven off this atmosphere, as a result of which the atmosphere is now depleted of these elements compared to cosmic abundances. After the impact,[clarification needed] the molten Earth released volatile gases; and later more gases were released by volcanoes, completing a second atmosphere rich in greenhouse gases but poor in oxygen. :256 Finally, the third atmosphere, rich in oxygen, emerged when bacteria began to produce oxygen about 2.8 Ga.:83–84,116–117
In early models for the formation of the atmosphere and ocean, the second atmosphere was formed by outgassing of volatiles from the Earth's interior. Now it is considered likely that many of the volatiles were delivered during accretion by a process known as impact degassing in which incoming bodies vaporize on impact. The ocean and atmosphere would therefore have started to form even as the Earth formed. The new atmosphere probably contained water vapor, carbon dioxide, nitrogen, and smaller amounts of other gases.
Planetesimals at a distance of 1 astronomical unit (AU), the distance of the Earth from the Sun, probably did not contribute any water to the Earth because the solar nebula was too hot for ice to form and the hydration of rocks by water vapor would have taken too long. The water must have been supplied by meteorites from the outer asteroid belt and some large planetary embryos from beyond 2.5 AU. Comets may also have contributed. Though most comets are today in orbits farther away from the Sun than Neptune, computer simulations show they were originally far more common in the inner parts of the solar system.:130-132
As the planet cooled, clouds formed. Rain created the oceans. Recent evidence suggests the oceans may have begun forming as early as 4.4 Ga. By the start of the Archean eon they already covered the Earth. This early formation has been difficult to explain because of a problem known as the faint young Sun paradox. Stars are known to get brighter as they age, and at the time of its formation the Sun would have been emitting only 70% of its current power. Many models predict that the Earth would have been covered in ice. A likely solution is that there was enough carbon dioxide and methane to produce a greenhouse effect. The carbon dioxide would have been produced by volcanoes and the methane by early microbes. Another greenhouse gas, ammonia, would have been ejected by volcanos but quickly destroyed by ultraviolet radiation.:83
Origin of life
One of the reasons for interest in the early atmosphere and ocean is that they form the conditions under which life first arose. There are many models, but little consensus, on how life emerged from non-living chemicals; chemical systems that have been created in the laboratory still fall well short of the minimum complexity for a living organism.
The first step in the emergence of life may have been chemical reactions that produced many of the simpler organic compounds, including nucleobases and amino acids, that are the building blocks of life. An experiment in 1953 by Stanley Miller and Harold Urey showed that such molecules could form in an atmosphere of water, methane, ammonia and hydrogen with the aid of sparks to mimic the effect of lightning. Although the atmospheric composition was probably different from the composition used by Miller and Urey, later experiments with more realistic compositions also managed to synthesize organic molecules. Recent computer simulations have even shown that extraterrestrial organic molecules could have formed in the protoplanetary disk before the formation of the Earth.
The next stage of complexity could have been reached from at least three possible starting points: self-replication, an organism's ability to produce offspring that are very similar to itself; metabolism, its ability to feed and repair itself; and external cell membranes, which allow food to enter and waste products to leave, but exclude unwanted substances.
Replication first: RNA world
Even the simplest members of the three modern domains of life use DNA to record their "recipes" and a complex array of RNA and protein molecules to "read" these instructions and use them for growth, maintenance and self-replication.
The discovery that a kind of RNA molecule called a ribozyme can catalyze both its own replication and the construction of proteins led to the hypothesis that earlier life-forms were based entirely on RNA. They could have formed an RNA world in which there were individuals but no species, as mutations and horizontal gene transfers would have meant that the offspring in each generation were quite likely to have different genomes from those that their parents started with. RNA would later have been replaced by DNA, which is more stable and therefore can build longer genomes, expanding the range of capabilities a single organism can have. Ribozymes remain as the main components of ribosomes, the "protein factories" of modern cells.
Although short, self-replicating RNA molecules have been artificially produced in laboratories, doubts have been raised about whether natural non-biological synthesis of RNA is possible. The earliest ribozymes may have been formed of simpler nucleic acids such as PNA, TNA or GNA, which would have been replaced later by RNA. Other pre-RNA replicators have been posited, including crystals:150 and even quantum systems.
In 2003 it was proposed that porous metal sulfide precipitates would assist RNA synthesis at about 100 °C (212 °F) and ocean-bottom pressures near hydrothermal vents. In this hypothesis, lipid membranes would be the last major cell components to appear and until they did the proto-cells would be confined to the pores.
Metabolism first: iron–sulfur world
Another long-standing hypothesis is that the first life was composed of protein molecules. Amino acids, the building blocks of proteins, are easily synthesized in plausible prebiotic conditions, as are small peptides (polymers of amino acids) that make good catalysts.:295–297 A series of experiments starting in 1997 showed that amino acids and peptides could form in the presence of carbon monoxide and hydrogen sulfide with iron sulfide and nickel sulfide as catalysts. Most of the steps in their assembly required temperatures of about 100 °C (212 °F) and moderate pressures, although one stage required 250 °C (482 °F) and a pressure equivalent to that found under 7 kilometres (4.3 mi) of rock. Hence, self-sustaining synthesis of proteins could have occurred near hydrothermal vents.
A difficulty with the metabolism-first scenario is finding a way for organisms to evolve. Without the ability to replicate as individuals, aggregates of molecules would have "compositional genomes" (counts of molecular species in the aggregate) as the target of natural selection. However, a recent model shows that such a system is unable to evolve in response to natural selection.
Membranes first: Lipid world
It has been suggested that double-walled "bubbles" of lipids like those that form the external membranes of cells may have been an essential first step. Experiments that simulated the conditions of the early Earth have reported the formation of lipids, and these can spontaneously form liposomes, double-walled "bubbles", and then reproduce themselves. Although they are not intrinsically information-carriers as nucleic acids are, they would be subject to natural selection for longevity and reproduction. Nucleic acids such as RNA might then have formed more easily within the liposomes than they would have outside.
The clay theory
Some clays, notably montmorillonite, have properties that make them plausible accelerators for the emergence of an RNA world: they grow by self-replication of their crystalline pattern, are subject to an analog of natural selection (as the clay "species" that grows fastest in a particular environment rapidly becomes dominant), and can catalyze the formation of RNA molecules. Although this idea has not become the scientific consensus, it still has active supporters.:150–158
Research in 2003 reported that montmorillonite could also accelerate the conversion of fatty acids into "bubbles", and that the bubbles could encapsulate RNA attached to the clay. Bubbles can then grow by absorbing additional lipids and dividing. The formation of the earliest cells may have been aided by similar processes.
Last universal ancestor
It is believed that of this multiplicity of protocells, only one line survived. Current phylogenetic evidence suggests that the last universal ancestor (LUA) lived during the early Archean eon, perhaps 3.5 Ga or earlier. This LUA cell is the ancestor of all life on Earth today. It was probably a prokaryote, possessing a cell membrane and probably ribosomes, but lacking a nucleus or membrane-bound organelles such as mitochondria or chloroplasts. Like all modern cells, it used DNA as its genetic code, RNA for information transfer and protein synthesis, and enzymes to catalyze reactions. Some scientists believe that instead of a single organism being the last universal common ancestor, there were populations of organisms exchanging genes by lateral gene transfer.
The Proterozoic eon lasted from 2.5 Ga to 542 Ma (million years ago).:130 In this time span, cratons grew into continents with modern sizes. The change to an oxygen-rich atmosphere was a crucial development. Life developed from prokaryotes into eukaryotes and multicellular forms. The Proterozoic saw a couple of severe ice ages called snowball Earths. After the last Snowball Earth about 600 Ma, the evolution of life on Earth accelerated. About 580 Ma, the Ediacara biota formed the prelude for the Cambrian Explosion.
The earliest cells absorbed energy and food from the surrounding environment. They used fermentation, the breakdown of more complex compounds into less complex compounds with less energy, and used the energy so liberated to grow and reproduce. Fermentation can only occur in an anaerobic (oxygen-free) environment. The evolution of photosynthesis made it possible for cells to manufacture their own food.:377
Most of the life that covers the surface of the Earth depends directly or indirectly on photosynthesis. The most common form, oxygenic photosynthesis, turns carbon dioxide, water and sunlight into food. It captures the energy of sunlight in energy-rich molecules such as ATP, which then provide the energy to make sugars. To supply the electrons in the circuit, hydrogen is stripped from water, leaving oxygen as a waste product. Some organisms, including purple bacteria and green sulfur bacteria, use an anoxygenic form of photosynthesis that use alternatives to hydrogen stripped from water as electron donors; examples are hydrogen sulfide, sulfur and iron. Such organisms are mainly restricted to extreme environments such as hot springs and hydrothermal vents.:379–382
The simpler anoxygenic form arose about 3.8 Ga, not long after the appearance of life. The timing of oxygenic photosynthesis is more controversial; it had certainly appeared by about 2.4 Ga, but some researchers put it back as far as 3.2 Ga. The latter "probably increased global productivity by at least two or three orders of magnitude." Among the oldest remnants of oxygen-producing lifeforms are fossil stromatolites.
At first, the released oxygen was bound up with limestone, iron, and other minerals. The oxidized iron appears as red layers in geological strata called banded iron formations that formed in abundance during the Siderian period (between 2500 Ma and 2300 Ma).:133 When most of the exposed readily reacting minerals were oxidized, oxygen finally began to accumulate in the atmosphere. Though each cell only produced a minute amount of oxygen, the combined metabolism of many cells over a vast time transformed Earth’s atmosphere to its current state. This was Earth’s third atmosphere.:50–51:83–84,116–117
Some oxygen was stimulated by incoming ultraviolet radiation to form ozone, which collected in a layer near the upper part of the atmosphere. The ozone layer absorbed, and still absorbs, a significant amount of the ultraviolet radiation that once had passed through the atmosphere. It allowed cells to colonize the surface of the ocean and eventually the land: without the ozone layer, ultraviolet radiation bombarding land and sea would have caused unsustainable levels of mutation in exposed cells.:219–220
Photosynthesis had another major impact. Oxygen was toxic; much life on Earth probably died out as its levels rose in what is known as the oxygen catastrophe. Resistant forms survived and thrived, and some developed the ability to use oxygen to increase their metabolism and obtain more energy from the same food.
The natural evolution of the Sun made it progressively more luminous during the Archean and Proterozoic eons; the Sun's luminosity increases 6% every billion years.:165 As a result, the Earth began to receive more heat from the Sun in the Proterozoic eon. However, the Earth did not get warmer. Instead, the geological record seems to suggest it cooled dramatically during the early Proterozoic. Glacial deposits found in South Africa date back to 2.2 Ga, at which time, based on paleomagnetic evidence, they must have been located near the equator. Thus, this glaciation, known as the Makganyene glaciation, may have been global. Some scientists suggest this and following Proterozoic ice ages were so severe that the planet was totally frozen over from the poles to the equator, a hypothesis called Snowball Earth.
The ice age around 2.3 Ga could have been directly caused by the increased oxygen concentration in the atmosphere, which caused the decrease of methane (CH4) in the atmosphere. Methane is a strong greenhouse gas, but with oxygen it reacts to form CO2, a less effective greenhouse gas.:172 When free oxygen became available in the atmosphere, the concentration of methane could have decreased dramatically, enough to counter the effect of the increasing heat flow from the Sun.
Emergence of eukaryotes
Modern taxonomy classifies life into three domains. The time of the origin of these domains is uncertain. The Bacteria domain probably first split off from the other forms of life (sometimes called Neomura), but this supposition is controversial. Soon after this, by 2 Ga, the Neomura split into the Archaea and the Eukarya. Eukaryotic cells (Eukarya) are larger and more complex than prokaryotic cells (Bacteria and Archaea), and the origin of that complexity is only now becoming known.
Around this time, the first proto-mitochondrion was formed. A bacterial cell related to today’s Rickettsia, which had evolved to metabolize oxygen, entered a larger prokaryotic cell, which lacked that capability. Perhaps the large cell attempted to digest the smaller one but failed (possibly due to the evolution of prey defenses). The smaller cell may have tried to parasitize the larger one. In any case, the smaller cell survived inside the larger cell. Using oxygen, it metabolized the larger cell’s waste products and derived more energy. Part of this excess energy was returned to the host. The smaller cell replicated inside the larger one. Soon, a stable symbiosis developed between the large cell and the smaller cells inside it. Over time, the host cell acquired some genes from the smaller cells, and the two kinds became dependent on each other: the larger cell could not survive without the energy produced by the smaller ones, and these in turn could not survive without the raw materials provided by the larger cell. The whole cell is now considered a single organism, and the smaller cells are classified as organelles called mitochondria.
A similar event occurred with photosynthetic cyanobacteria entering large heterotrophic cells and becoming chloroplasts.:60–61:536–539 Probably as a result of these changes, a line of cells capable of photosynthesis split off from the other eukaryotes more than 1 billion years ago. There were probably several such inclusion events. Besides the well-established endosymbiotic theory of the cellular origin of mitochondria and chloroplasts, there are theories that cells led to peroxisomes, spirochetes led to cilia and flagella, and that perhaps a DNA virus led to the cell nucleus, though none of them are widely accepted.
Archaeans, bacteria, and eukaryotes continued to diversify and to become more complex and better adapted to their environments. Each domain repeatedly split into multiple lineages, although little is known about the history of the archaea and bacteria. Around 1.1 Ga, the supercontinent Rodinia was assembling. The plant, animal, and fungi lines had split, though they still existed as solitary cells. Some of these lived in colonies, and gradually a division of labor began to take place; for instance, cells on the periphery might have started to assume different roles from those in the interior. Although the division between a colony with specialized cells and a multicellular organism is not always clear, around 1 billion years ago the first multicellular plants emerged, probably green algae. Possibly by around 900 Ma:488 true multicellularity had also evolved in animals.
At first it probably resembled today’s sponges, which have totipotent cells that allow a disrupted organism to reassemble itself.:483-487 As the division of labor was completed in all lines of multicellular organisms, cells became more specialized and more dependent on each other; isolated cells would die.
Supercontinents in the Proterozoic
Reconstructions of tectonic plate movement in the past 250 million years (the Cenozoic and Mesozoic eras) can be made reliably using fitting of continental margins, ocean floor magnetic anomalies and paleomagnetic poles. No ocean crust dates back further than that, so earlier reconstructions are more difficult. Paleomagnetic poles are supplemented by geologic evidence such as orogenic belts, which mark the edges of ancient plates, and past distributions of flora and fauna. The further back in time, the scarcer and harder to interpret the data get and the more diverse the reconstructions.:370
Throughout the history of the Earth, there have been times when continents collided and formed a supercontinent, which later broke up into new continents. About 1000 to 830 Ma, most continental mass was united in the supercontinent Rodinia.:370 Rodinia may have been preceded by Early-Middle Proterozoic continents called Nuna and Columbia.:374
After the break-up of Rodinia about 800 Ma, the continents may have formed another short-lived supercontinent, Pannotia, around 550 Ma. The hypothetical supercontinent is sometimes referred to as Pannotia or Vendia.:321–322 The evidence for it is a phase of continental collision known as the Pan-African orogeny, which joined the continental masses of current-day Africa, South America, Antarctica and Australia. The existence of Pannotia depends on the timing of the rifting between Gondwana (which included most of the landmass now in the Southern Hemisphere, as well as the Arabian Peninsula and the Indian subcontinent) and Laurentia (roughly equivalent to current-day North America).:374 It is at least certain that by the end of the Proterozoic eon, most of the continental mass lay united in a position around the south pole.
Late Proterozoic climate and life
The end of the Proterozoic saw at least two Snowball Earths, so severe that the surface of the oceans may have been completely frozen. This happened about 716.5 and 635 Ma, in the Cryogenian period. The intensity and mechanism of both glaciations are still under investigation and harder to explain than the early Proterozoic Snowball Earth. Most paleoclimatologists think the cold episodes were linked to the formation of the supercontinent Rodinia. Because Rodinia was centered on the equator, rates of chemical weathering increased and carbon dioxide (CO2) was taken from the atmosphere. Because CO2 is an important greenhouse gas, climates cooled globally. In the same way, during the Snowball Earths most of the continental surface was covered with permafrost, which decreased chemical weathering again, leading to the end of the glaciations. An alternative hypothesis is that enough carbon dioxide escaped through volcanic outgassing that the resulting greenhouse effect raised global temperatures. Increased volcanic activity resulted from the break-up of Rodinia at about the same time.
The Cryogenian period was followed by the Ediacaran period, which was characterized by a rapid development of new multicellular lifeforms. Whether there is a connection between the end of the severe ice ages and the increase in diversity of life is not clear, but it does not seem coincidental. The new forms of life, called Ediacara biota, were larger and more diverse than ever. Though the taxonomy of most Ediacaran life forms is unclear, some were ancestors of groups of modern life. Important developments were the origin of muscular and neural cells. None of the Ediacaran fossils had hard body parts like skeletons. These first appear after the boundary between the Proterozoic and Phanerozoic eons or Ediacaran and Cambrian periods.
The Phanerozoic is the current eon on Earth, which started approximately 542 million years ago. It consists of three eras: The Paleozoic, Mesozoic, and Cenozoic, and is the time when multi-cellular life greatly diversified into almost all the organisms known today.
The Paleozoic era (meaning: era of old life forms) was the first and longest era of the Phanerozoic eon, lasting from 542 to 251 Ma. During the Paleozoic, many modern groups of life came into existence. Life colonized the land, first plants, then animals. Life usually evolved slowly. At times, however, there are sudden radiations of new species or mass extinctions. These bursts of evolution were often caused by unexpected changes in the environment resulting from natural disasters such as volcanic activity, meteorite impacts or climate changes.
The continents formed at the break-up of Pannotia and Rodinia at the end of the Proterozoic would slowly move together again during the Paleozoic. This would eventually result in phases of mountain building that created the supercontinent Pangaea in the late Paleozoic.
The rate of the evolution of life as recorded by fossils accelerated in the Cambrian period (542–488 Ma). The sudden emergence of many new species, phyla, and forms in this period is called the Cambrian Explosion. The biological fomenting in the Cambrian Explosion was unpreceded before and since that time.:229 Whereas the Ediacaran life forms appear yet primitive and not easy to put in any modern group, at the end of the Cambrian most modern phyla were already present. The development of hard body parts such as shells, skeletons or exoskeletons in animals like molluscs, echinoderms, crinoids and arthropods (a well-known group of arthropods from the lower Paleozoic are the trilobites) made the preservation and fossilization of such life forms easier than those of their Proterozoic ancestors. For this reason, much more is known about life in and after the Cambrian than about that of older periods. Some of these Cambrian groups appear complex but are quite different from modern life; examples are Anomalocaris and Haikouichthys.
During the Cambrian, the first vertebrate animals, among them the first fishes, had appeared.:357 A creature that could have been the ancestor of the fishes, or was probably closely related to it, was Pikaia. It had a primitive notochord, a structure that could have developed into a vertebral column later. The first fishes with jaws (Gnathostomata) appeared during the next geological period, the Ordovician. The colonisation of new niches resulted in massive body sizes. In this way, fishes with increasing sizes evolved during the early Paleozoic, such as the titanic placoderm Dunkleosteus, which could grow 7 meters long.
The diversity of life forms did not increase greatly because of a series of mass extinctions that define widespread biostratigraphic units called biomeres. After each extinction pulse, the continental shelf regions were repopulated by similar life forms that may have been evolving slowly elsewhere. By the late Cambrian, the trilobites had reached their greatest diversity and dominated nearly all fossil assemblages.:34
Paleozoic tectonics, paleogeography and climate
At the end of the Proterozoic, the supercontinent Pannotia had broken apart in the smaller continents Laurentia, Baltica, Siberia and Gondwana. During periods when continents move apart, more oceanic crust is formed by volcanic activity. Because young volcanic crust is relatively hotter and less dense than old oceanic crust, the ocean floors rise during such periods. This causes the sea level to rise. Therefore, in the first half of the Paleozoic, large areas of the continents were below sea level.
Early Paleozoic climates were warmer than today, but the end of the Ordovician saw a short ice age during which glaciers covered the south pole, where the huge continent Gondwana was situated. Traces of glaciation from this period are only found on former Gondwana. During the Late Ordovician ice age, a few mass extinctions took place, in which many brachiopods, trilobites, Bryozoa and corals disappeared. These marine species could probably not contend with the decreasing temperature of the sea water. After the extinctions new species evolved, more diverse and better adapted. They would fill the niches left by the extinct species.
The continents Laurentia and Baltica collided between 450 and 400 Ma, during the Caledonian Orogeny, to form Laurussia (also known as Euramerica). Traces of the mountain belt this collision caused can be found in Scandinavia, Scotland, and the northern Appalachians. In the Devonian period (416–359 Ma) Gondwana and Siberia began to move towards Laurussia. The collision of Siberia with Laurussia caused the Uralian Orogeny, the collision of Gondwana with Laurussia is called the Variscan or Hercynian Orogeny in Europe or the Alleghenian Orogeny in North America. The latter phase took place during the Carboniferous period (359–299 Ma) and resulted in the formation of the last supercontinent, Pangaea.
Colonization of land
Oxygen accumulation from photosynthesis resulted in the formation of an ozone layer that absorbed much of the Sun’s ultraviolet radiation, meaning unicellular organisms that reached land were less likely to die, and prokaryotes began to multiply and become better adapted to survival out of the water. Prokaryote lineages had probably colonized the land as early as 2.6 Ga even before the origin of the eukaryotes. For a long time, the land remained barren of multicellular organisms. The supercontinent Pannotia formed around 600 Ma and then broke apart a short 50 million years later. Fish, the earliest vertebrates, evolved in the oceans around 530 Ma.:354 A major extinction event occurred near the end of the Cambrian period, which ended 488 Ma.
Several hundred million years ago, plants (probably resembling algae) and fungi started growing at the edges of the water, and then out of it.:138–140 The oldest fossils of land fungi and plants date to 480–460 Ma, though molecular evidence suggests the fungi may have colonized the land as early as 1000 Ma and the plants 700 Ma. Initially remaining close to the water’s edge, mutations and variations resulted in further colonization of this new environment. The timing of the first animals to leave the oceans is not precisely known: the oldest clear evidence is of arthropods on land around 450 Ma, perhaps thriving and becoming better adapted due to the vast food source provided by the terrestrial plants. There is also unconfirmed evidence that arthropods may have appeared on land as early as 530 Ma.
Evolution of tetrapods
At the end of the Ordovician period, 443 Ma, additional extinction events occurred, perhaps due to a concurrent ice age. Around 380 to 375 Ma, the first tetrapods evolved from fish. Fins evolved to become limbs that the first tetrapods used to lift their heads out of the water to breathe air. This would let them live in oxygen-poor water, or pursue small prey in shallow water. They may have later ventured on land for brief periods. Eventually, some of them became so well adapted to terrestrial life that they spent their adult lives on land, although they hatched in the water and returned to lay their eggs. This was the origin of the amphibians. About 365 Ma, another period of extinction occurred, perhaps as a result of global cooling. Plants evolved seeds, which dramatically accelerated their spread on land, around this time (by approximately 360 Ma).
About 20 million years later (340 Ma:293–296), the amniotic egg evolved, which could be laid on land, giving a survival advantage to tetrapod embryos. This resulted in the divergence of amniotes from amphibians. Another 30 million years (310 Ma:254–256) saw the divergence of the synapsids (including mammals) from the sauropsids (including birds and reptiles). Other groups of organisms continued to evolve, and lines diverged—in fish, insects, bacteria, and so on—but less is known of the details.
The Mesozoic ("middle life") era lasted from 251 Ma to 66 Ma. It is subdivided into the Triassic, Jurassic, and Cretaceous periods. The era began with the Permian–Triassic extinction event, the most severe extinction event in the fossil record; 95% of the species on Earth died out. It ended with the Cretaceous–Paleogene extinction event that wiped out the dinosaurs. The Permian-Triassic event was possibly caused by some combination of the Siberian Traps volcanic event, an asteroid impact, methane hydrate gasification, sea level fluctuations, and a major anoxic event. Either the proposed Wilkes Land crater in Antarctica or Bedout structure off the northwest coast of Australia may indicate an impact connection with the Permian-Triassic extinction. But it remains uncertain whether either these or other proposed Permian-Triassic boundary craters are either real impact craters or even contemporaneous with the Permian-Triassic extinction event. Life persevered, and around 230 Ma, dinosaurs split off from their reptilian ancestors. The Triassic–Jurassic extinction event at 200 Ma spared many of the dinosaurs, and they soon became dominant among the vertebrates. Though some mammalian lines began to separate during this period, existing mammals were probably small animals resembling shrews.:169
By 180 Ma, Pangaea broke up into Laurasia and Gondwana. The boundary between avian and non-avian dinosaurs is not clear, but Archaeopteryx, traditionally considered one of the first birds, lived around 150 Ma. The earliest evidence for the angiosperms evolving flowers is during the Cretaceous period, some 20 million years later (132 Ma). In 66 Ma, a 10-kilometre (6.2 mi) asteroid struck Earth just off the Yucatán Peninsula - somewhere in the south western tip of then Laurasia - where the Chicxulub crater is today. This ejected vast quantities of particulate matter and vapor into the air that occluded sunlight, inhibiting photosynthesis. Most large animals, including the non-avian dinosaurs, became extinct, marking the end of the Cretaceous period and Mesozoic era.
The Cenozoic era began at 66 Ma, and is subdivided into the Paleogene, Neogene, and Quaternary periods. Mammals and birds were able to survive the Cretaceous–Paleogene extinction event that killed off the dinosaurs and many other forms of life, and this is the era during which they diversified into their modern forms.
Diversification of mammals
|This section does not cite any references or sources. (May 2013)|
Mammals have existed since the late Triassic, but prior to the Cretaceous–Paleogene extinction event they remained small. During the Cenozoic, mammals rapidly diversified to fill some niches that the dinosaurs and other extinct animals had left behind, branching out into many of the modern orders. With many marine reptiles extinct, some mammals began living in the oceans and became cetaceans. Others became felids and canids, swift and agile land predators. The drier global climate of the Cenozoic led to the expansion of grasslands and the evolution of grazing and hoofed mammals such as equids and bovids. Some arboreal mammals became the primates, of which one lineage would lead to modern humans.
A small African ape living around 6 Ma was the last animal whose descendants would include both modern humans and their closest relatives, the chimpanzees.:100–101 Only two branches of its family tree have surviving descendants. Very soon after the split, for reasons that are still unclear, apes in one branch developed the ability to walk upright.:95–99 Brain size increased rapidly, and by 2 Ma, the first animals classified in the genus Homo had appeared.:300 Of course, the line between different species or even genera is somewhat arbitrary as organisms continuously change over generations. Around the same time, the other branch split into the ancestors of the common chimpanzee and the ancestors of the bonobo as evolution continued simultaneously in all life forms.:100–101
The ability to control fire probably began in Homo erectus (or Homo ergaster), probably at least 790,000 years ago but perhaps as early as 1.5 Ma.:67 The use and discovery of controlled fire may even predate Homo erectus. Fire was possibly used by the early Lower Paleolithic (Oldowan) hominid Homo habilis or strong australopithecines such as Paranthropus.
It is more difficult to establish the origin of language; it is unclear whether Homo erectus could speak or if that capability had not begun until Homo sapiens.:67 As brain size increased, babies were born earlier, before their heads grew too large to pass through the pelvis. As a result, they exhibited more plasticity, and thus possessed an increased capacity to learn and required a longer period of dependence. Social skills became more complex, language became more sophisticated, and tools became more elaborate. This contributed to further cooperation and intellectual development.:7 Modern humans (Homo sapiens) are believed to have originated around 200,000 years ago or earlier in Africa; the oldest fossils date back to around 160,000 years ago.
The first humans to show signs of spirituality are the Neanderthals (usually classified as a separate species with no surviving descendants); they buried their dead, often with no sign of food or tools.:17 However, evidence of more sophisticated beliefs, such as the early Cro-Magnon cave paintings (probably with magical or religious significance):17–19 did not appear until 32,000 years ago. Cro-Magnons also left behind stone figurines such as Venus of Willendorf, probably also signifying religious belief.:17–19 By 11,000 years ago, Homo sapiens had reached the southern tip of South America, the last of the uninhabited continents (except for Antarctica, which remained undiscovered until 1820 AD). Tool use and communication continued to improve, and interpersonal relationships became more intricate.
Throughout more than 90% of its history, Homo sapiens lived in small bands as nomadic hunter-gatherers.:8 As language became more complex, the ability to remember and communicate information resulted in a new replicator: the meme. Ideas could be exchanged quickly and passed down the generations. Cultural evolution quickly outpaced biological evolution, and history proper began. Between 8500 and 7000 BC, humans in the Fertile Crescent in Middle East began the systematic husbandry of plants and animals: agriculture. This spread to neighboring regions, and developed independently elsewhere, until most Homo sapiens lived sedentary lives in permanent settlements as farmers. Not all societies abandoned nomadism, especially those in isolated areas of the globe poor in domesticable plant species, such as Australia. However, among those civilizations that did adopt agriculture, the relative stability and increased productivity provided by farming allowed the population to expand.
Agriculture had a major impact; humans began to affect the environment as never before. Surplus food allowed a priestly or governing class to arise, followed by increasing division of labor. This led to Earth’s first civilization at Sumer in the Middle East, between 4000 and 3000 BC.:15 Additional civilizations quickly arose in ancient Egypt, at the Indus River valley and in China. The invention of writing enabled complex societies to arise: record-keeping and libraries served as a storehouse of knowledge and increased the cultural transmission of information. Humans no longer had to spend all their time working for survival—curiosity and education drove the pursuit of knowledge and wisdom.
Various disciplines, including science (in a primitive form), arose. New civilizations sprang up, traded with one another, and fought for territory and resources. Empires soon began to develop. By around 500 BC, there were advanced civilizations in the Middle East, Iran, India, China, and Greece, at times expanding, at times entering into decline.:3 In 221 BC, China became a single polity that would grow to spread its culture throughout eastern Asia, and it has remained the most populous nation in the world. The fundamentals of the Western world were largely shaped by the ancient Greco-Roman culture. The Roman Empire was Christianized by Emperor Constantine in the early fourth century and declined by the end of the fifth. Beginning with the seventh century, Christianization of Europe began. In 610, Islam was founded and quickly became the dominant religion in western Asia. In 1054 AD the Great Schism between the Roman Catholic Church and the Eastern Orthodox Church led to the prominent cultural differences between Western and Eastern Europe.
In the fourteenth century, the Renaissance began in Italy with advances in religion, art, and science.:317–319 At that time the Christian Church as a political entity lost much of its power. In 1492, Christopher Columbus reached the Americas, initiating great changes to the new world. European civilization began to change beginning in 1500, leading to the scientific and industrial revolutions. That continent began to exert political and cultural dominance over human societies around the planet, a time known as the Colonial era (also see Age of Discovery).:295–299 In the eighteenth century a cultural movement known as the Age of Enlightenment further shaped the mentality of Europe and contributed to its secularization. From 1914 to 1918 and 1939 to 1945, nations around the world were embroiled in world wars. Established following World War I, the League of Nations was a first step in establishing international institutions to settle disputes peacefully. After failing to prevent World War II, mankind's bloodiest conflict, it was replaced by the United Nations. After the war, many new states were formed, declaring or being granted independence in a period of decolonization. The United States and Soviet Union became the world's dominant superpowers for a time, and they held an often-violent rivalry known as the Cold War until the dissolution of the latter. In 1992, several European nations joined in the European Union. As transportation and communication improved, the economies and political affairs of nations around the world have become increasingly intertwined. This globalization has often produced both conflict and cooperation.
Change has continued at a rapid pace from the mid-1940s to today. Technological developments include nuclear weapons, computers, genetic engineering, and nanotechnology. Economic globalization spurred by advances in communication and transportation technology has influenced everyday life in many parts of the world. Cultural and institutional forms such as democracy, capitalism, and environmentalism have increased influence. Major concerns and problems such as disease, war, poverty, violent radicalism, and recently, human-caused climate change have risen as the world population increases.
In 1957, the Soviet Union launched the first artificial satellite into orbit and, soon afterward, Yuri Gagarin became the first human in space. Neil Armstrong, an American, was the first to set foot on another astronomical object, the Moon. Unmanned probes have been sent to all the known planets in the solar system, with some (such as Voyager) having left the solar system. The Soviet Union and the United States were the earliest leaders in space exploration in the 20th century. Five space agencies, representing over fifteen countries, have worked together to build the International Space Station. Aboard it, there has been a continuous human presence in space since 2000. The World Wide Web became a part of everyday life in the 1990s, and since then has become an indispensable source of information in the developed world.
- Stanley 2005
- Gradstein, Ogg & Smith 2004
- Yoko Ohtomo; Takeshi Kakegawa; Akizumi Ishida; Toshiro Nagase et al. (8 December 2013). "Evidence for biogenic graphite in early Archaean Isua metasedimentary rocks". Nature Geoscience. doi:10.1038/ngeo2025. Retrieved 9 Dec 2013.
- Borenstein, Seth (13 November 2013). "Oldest fossil found: Meet your microbial mom". AP News. Retrieved 15 November 2013.
- Noffke, Nora; Christian, Daniel; Wacey, David; Hazen, Robert M. (8 November 2013). "Microbially Induced Sedimentary Structures Recording an Ancient Ecosystem in the ca. 3.48 Billion-Year-Old Dresser Formation, Pilbara, Western Australia". Astrobiology (journal) 13 (12): 1103–24. Bibcode:2013AsBio..13.1103N. doi:10.1089/ast.2013.1030. PMC 3870916. PMID 24205812. Retrieved 15 November 2013.
- Stearns, Beverly Peterson; Stearns, S. C.; Stearns, Stephen C. (2000). Watching, from the Edge of Extinction. Yale University Press. p. 1921. ISBN 978-0-300-08469-6. Retrieved 27 December 2014.
- Novacek, Michael J. (8 November 2014). "Prehistory’s Brilliant Future". New York Times. Retrieved 25 December 2014.
- G. Miller; Scott Spoolman (2012). Environmental Science - Biodiversity Is a Crucial Part of the Earth's Natural Capital. Cengage Learning. p. 62. ISBN 1-133-70787-4. Retrieved 27 December 2014.
- Gradstein, Ogg & van Kranendonk 2008
- Encrenaz, T. (2004). The solar system (3rd ed.). Berlin: Springer. p. 89. ISBN 978-3-540-00241-3.
- Matson, John (July 7, 2010). "Luminary Lineage: Did an Ancient Supernova Trigger the Solar System's Birth?". Scientific American. Retrieved 2012-04-13.
- P. Goldreich; W. R. Ward (1973). "The Formation of Planetesimals". Astrophysical Journal 183: 1051–1062. Bibcode:1973ApJ...183.1051G. doi:10.1086/152291.
- Newman, William L. (2007-07-09). "Age of the Earth". Publications Services, USGS. Retrieved 2007-09-20.
- Stassen, Chris (2005-09-10). "The Age of the Earth". TalkOrigins Archive. Retrieved 2008-12-30.
- "Age of the Earth". U.S. Geological Survey. 1997. Retrieved 2006-01-10.
- Stassen, Chris (2005-09-10). "The Age of the Earth". The TalkOrigins Archive. Retrieved 2007-09-20.
- Yin, Qingzhu; Jacobsen, S. B.; Yamashita, K.; Blichert-Toft, J.; Télouk, P.; Albarède, F. (2002). "A short timescale for terrestrial planet formation from Hf-W chronometry of meteorites". Nature 418 (6901): 949–952. Bibcode:2002Natur.418..949Y. doi:10.1038/nature00995. PMID 12198540.
- Kokubo, Eiichiro; Ida, Shigeru (2002). "Formation of protoplanet systems and diversity of planetary systems". The Astrophysical Journal 581 (1): 666–680. Bibcode:2002ApJ...581..666K. doi:10.1086/344105.
- Charles Frankel, 1996, Volcanoes of the Solar System, Cambridge University Press, pp. 7–8, ISBN 0-521-47770-0
- J.A. Jacobs (1953). "The Earth’s inner core". Nature 172 (4372): 297–298. Bibcode:1953Natur.172..297J. doi:10.1038/172297a0.
- van Hunen, J.; van den Berg, A.P. (2007). "Plate tectonics on the early Earth: Limitations imposed by strength and buoyancy of subducted lithosphere". Lithos 103 (1-2): 217–235. Bibcode:2008Litho.103..217V. doi:10.1016/j.lithos.2007.09.016.
- Wilde, S. A.; Valley, J.W.; Peck, W.H. & Graham, C.M. (2001). "Evidence from detrital zircons for the existence of continental crust and oceans on the Earth 4.4 Gyr ago" (PDF). Nature 409 (6817): 175–178. Bibcode:2001Natur.409..175W. doi:10.1038/35051550. PMID 11196637. Retrieved 2013-05-25.
- Lindsey, Rebecca; David Morrison; Robert Simmon (March 1, 2006). "Ancient crystals suggest earlier ocean". Earth Observatory. NASA. Retrieved April 18, 2012.
- Cavosie, A. J.; Valley, J. W.; Wilde, S. A.; Edinburgh Ion Microprobe Facility (E.I.M.F.) (2005). "Magmatic δ18O in 4400-3900 Ma detrital zircons: A record of the alteration and recycling of crust in the Early Archean". Earth and Planetary Science Letters 235 (3–4): 663–681. Bibcode:2005E&PSL.235..663C. doi:10.1016/j.epsl.2005.04.028.
- Belbruno, E.; Gott, J. Richard III (2005). "Where Did The Moon Come From?". The Astronomical Journal 129 (3): 1724–1745. arXiv:astro-ph/0405372. Bibcode:2005AJ....129.1724B. doi:10.1086/427539.
- Münker, Carsten; Jörg A. Pfänder; Stefan Weyer; Anette Büchl; Thorsten Kleine; Klaus Mezger (July 4, 2003). "Evolution of Planetary Cores and the Earth-Moon System from Nb/Ta Systematics". Science 301 (5629): 84–87. Bibcode:2003Sci...301...84M. doi:10.1126/science.1084662. PMID 12843390. Retrieved 2012-04-13.
- Nield, Ted (2009). "Moonwalk". Geoscientist (Geological Society of London) 18 (9): 8. Retrieved April 18, 2012.
- Britt, Robert Roy (2002-07-24). "New Insight into Earth’s Early Bombardment". Space.com. Retrieved 2012-02-09.
- Green, Jack (2011). "Academic Aspects of Lunar Water Resources and Their Relevance to Lunar Protolife". International Journal of Molecular Sciences 12 (9): 6051–6076. doi:10.3390/ijms12096051. PMC 3189768. PMID 22016644.
- Taylor, Thomas N.; Edith L. Taylor; Michael Krings (2006). Paleobotany: the biology and evolution of fossil plants. Academic Press. p. 49. ISBN 9780123739728.
- Steenhuysen, Julie (May 21, 2009). "Study turns back clock on origins of life on Earth". Reuters.com. Reuters. Retrieved May 21, 2009.
- "Space Topics: Pluto and Charon". The Planetary Society. Retrieved 6 April 2010.
- "Pluto: Overview". Solar System Exploration. National Aeronautics and Space Administration. Retrieved 19 April 2012.
- Kleine, T.; Palme, H.; Mezger, K.; Halliday, A.N. (2005). "Hf-W Chronometry of Lunar Metals and the Age and Early Differentiation of the Moon". Science 310 (5754): 1671–1674. Bibcode:2005Sci...310.1671K. doi:10.1126/science.1118842. PMID 16308422.
- Halliday, A.N. (2006). The Origin of the Earth; What's New?. Elements 2 (4). pp. 205–210. doi:10.2113/gselements.2.4.205.
- Halliday, Alex N (November 28, 2008). "A young Moon-forming giant impact at 70–110 million years accompanied by late-stage mixing, core formation and degassing of the Earth". Philosophical Transactions of the Royal Society A (Philosophical Transactions of the Royal Society) 366 (1883): 4163–4181. Bibcode:2008RSPTA.366.4163H. doi:10.1098/rsta.2008.0209. PMID 18826916.
- Williams, David R. (2004-09-01). "Earth Fact Sheet". NASA. Retrieved 2010-08-09.
- High Energy Astrophysics Science Archive Research Center (HEASARC). "StarChild Question of the Month for October 2001". NASA Goddard Space Flight Center. Retrieved 20 April 2012.
- Canup, R.M.; Asphaug, E. (2001). "Origin of the Moon in a giant impact near the end of the Earth's formation". Nature 412 (6848): 708–712. Bibcode:2001Natur.412..708C. doi:10.1038/35089010. PMID 11507633.
- Liu, Lin-Gun (1992). "Chemical composition of the Earth after the giant impact". Earth, Moon and Planets 57 (2): 85–97. Bibcode:1992EM&P...57...85L. doi:10.1007/BF00119610.
- Newsom, Horton E.; Taylor, Stuart Ross (1989). "Geochemical implications of the formation of the Moon by a single giant impact". Nature 338 (6210): 29–34. Bibcode:1989Natur.338...29N. doi:10.1038/338029a0.
- Taylor, G. Jeffrey (April 26, 2004). "Origin of the Earth and Moon". NASA. Retrieved 2006-03-27., Taylor (2006) at the NASA website.
- Davies, Geoffrey F. Mantle convection for geologists. Cambridge, UK: Cambridge University Press. ISBN 978-0-521-19800-4.
- Cattermole, Peter; Moore, Patrick (1985). The story of the earth. Cambridge: Cambridge University Press. ISBN 978-0-521-26292-7.
- Bleeker, W.; B. W. Davis (May 2004). What is a craton?. Spring meeting. American Geophysical Union. T41C-01.
- Lunine 1999
- Condie, Kent C. (1997). Plate tectonics and crustal evolution (4th ed.). Oxford: Butterworth Heinemann. ISBN 978-0-7506-3386-4.
- Holland, Heinrich D. (June 2006). "The oxygenation of the atmosphere and oceans". The Royal Society. doi:10.1098/rstb.2006.1838+Phil.+Trans.+R.+Soc.+B+29+June+2006+vol.+361+no.+1470+903-915. Retrieved 2010-02-17.
- Kasting, James F. (1993). "Earth's early atmosphere". Science 259 (5097): 920–926. doi:10.1126/science.11536547. PMID 11536547.
- Gale, Joseph (2009). Astrobiology of Earth : the emergence, evolution, and future of life on a planet in turmoil. Oxford: Oxford University Press. ISBN 978-0-19-920580-6.
- Kasting, James F.; Catling, David (2003). "Evolution of a habitable planet". Annual Review of Astronomy and Astrophysics 41 (1): 429–463. Bibcode:2003ARA&A..41..429K. doi:10.1146/annurev.astro.41.071601.170049.
- Kasting, James F.; Howard, M. Tazewell (September 7, 2006). "Atmospheric composition and climate on the early Earth". Philosophical Transactions of the Royal Society B 361 (361): 1733–1742. doi:10.1098/rstb.2006.1902.
- Selsis, Franck (2005). "Chapter 11. The Prebiotic Atmosphere of the Earth". Astrobiology: Future perspectives. Astrophysics and space science library 305. pp. 267–286. doi:10.1007/1-4020-2305-7_11.
- Morbidelli, A.; Chambers, J.; Lunine, J. I.; Petit, J. M.; Robert, F.; Valsecchi, G. B.; Cyr, K. E. (2000). "Source regions and timescales for the delivery of water to the Earth". Meteoritics & Planetary Science 35 (6): 1309–1320. Bibcode:2000M&PS...35.1309M. doi:10.1111/j.1945-5100.2000.tb01518.x.
- Sagan, Carl; Mullen, George (July 7, 1972). "Earth and Mars: Evolution of Atmospheres and Surface Temperatures". Science 177 (4043): 52–56. Bibcode:1972Sci...177...52S. doi:10.1126/science.177.4043.52. PMID 17756316.
- Szathmáry, E. (February 2005). "In search of the simplest cell". Nature 433 (7025): 469–470. Bibcode:2005Natur.433..469S. doi:10.1038/433469a. PMID 15690023. Retrieved 2008-09-01.
- Luisi, P. L.; Ferri, F. & Stano, P. (2006). "Approaches to semi-synthetic minimal cells: a review". Naturwissenschaften 93 (1): 1–13. Bibcode:2006NW.....93....1L. doi:10.1007/s00114-005-0056-z. PMID 16292523.
- A. Lazcano, J. L. Bada (June 2004). "The 1953 Stanley L. Miller Experiment: Fifty Years of Prebiotic Organic Chemistry". Origins of Life and Evolution of Biospheres 33 (3): 235–242. doi:10.1023/A:1024807125069. PMID 14515862.
- Dreifus, Claudia (2010-05-17). "A Conversation With Jeffrey L. Bada: A Marine Chemist Studies How Life Began". nytimes.com.
- Moskowitz, Clara (29 March 2012). "Life's Building Blocks May Have Formed in Dust Around Young Sun". Space.com. Retrieved 30 March 2012.
- Peretó, J. (2005). "Controversies on the origin of life" (PDF). Int. Microbiol. 8 (1): 23–31. PMID 15906258. Retrieved 2007-10-07.
- Joyce, G.F. (2002). "The antiquity of RNA-based evolution". Nature 418 (6894): 214–21. Bibcode:2002Natur.418..214J. doi:10.1038/418214a. PMID 12110897.
- Hoenigsberg, H. (December 2003). "Evolution without speciation but with selection: LUCA, the Last Universal Common Ancestor in Gilbert's RNA world". Genetic and Molecular Research 2 (4): 366–375. PMID 15011140. Retrieved 2008-08-30.(also available as PDF)
- Forterre, Patrick (2005). "The two ages of the RNA world, and the transition to the DNA world: a story of viruses and cells". Biochimie 87 (9–10): 793–803. doi:10.1016/j.biochi.2005.03.015. PMID 16164990.
- Cech, T.R. (August 2000). "The ribosome is a ribozyme". Science 289 (5481): 878–9. doi:10.1126/science.289.5481.878. PMID 10960319. Retrieved 2008-09-01.
- Johnston WK, Unrau PJ et al. (2001). "RNA-Catalyzed RNA Polymerization: Accurate and General RNA-Templated Primer Extension". Science 292 (5520): 1319–1325. Bibcode:2001Sci...292.1319J. doi:10.1126/science.1060786. PMID 11358999.
- Levy, M. & Miller, S.L. (July 1998). "The stability of the RNA bases: Implications for the origin of life". Proc. Natl. Acad. Sci. U.S.A. 95 (14): 7933–8. Bibcode:1998PNAS...95.7933L. doi:10.1073/pnas.95.14.7933. PMC 20907. PMID 9653118.
- Larralde, R.; Robertson, M. P. & Miller, S. L. (August 1995). "Rates of decomposition of ribose and other sugars: implications for chemical evolution". Proc. Natl. Acad. Sci. U.S.A. 92 (18): 8158–60. Bibcode:1995PNAS...92.8158L. doi:10.1073/pnas.92.18.8158. PMC 41115. PMID 7667262.
- Lindahl, T. (April 1993). "Instability and decay of the primary structure of DNA". Nature 362 (6422): 709–15. Bibcode:1993Natur.362..709L. doi:10.1038/362709a0. PMID 8469282.
- Orgel, L. (November 2000). "A simpler nucleic acid". Science 290 (5495): 1306–7. doi:10.1126/science.290.5495.1306. PMID 11185405.
- Nelson, K.E.; Levy, M. & Miller, S.L. (April 2000). "Peptide nucleic acids rather than RNA may have been the first genetic molecule". Proc. Natl. Acad. Sci. U.S.A. 97 (8): 3868–71. Bibcode:2000PNAS...97.3868N. doi:10.1073/pnas.97.8.3868. PMC 18108. PMID 10760258.
- Dawkins, Richard (1996) . "Origins and miracles". The Blind Watchmaker. New York: W. W. Norton & Company. ISBN 0-393-31570-3.
- Davies, Paul (October 6, 2005). "A quantum recipe for life". Nature 437 (7060): 819. Bibcode:2005Natur.437..819D. doi:10.1038/437819a. PMID 16208350. (subscription required).
- Martin, W. & Russell, M.J. (2003). "On the origins of cells: a hypothesis for the evolutionary transitions from abiotic geochemistry to chemoautotrophic prokaryotes, and from prokaryotes to nucleated cells". Philosophical Transactions of the Royal Society B 358 (1429): 59–85. doi:10.1098/rstb.2002.1183. PMC 1693102. PMID 12594918.
- Kauffman, Stuart A. (1993). The origins of order : self-organization and selection in evolution (Reprint ed.). New York: Oxford University Press. ISBN 978-0-19-507951-7.
- Wächtershäuser, G. (August 2000). "Life as we don't know it". Science 289 (5483): 1307–8. doi:10.1126/science.289.5483.1307. PMID 10979855.
- Vasas, V.; Szathmáry, E.; Santos, M. (4 January 2010). "Lack of evolvability in self-sustaining autocatalytic networks constraints metabolism-first scenarios for the origin of life". Proceedings of the National Academy of Sciences 107 (4): 1470–1475. Bibcode:2010PNAS..107.1470V. doi:10.1073/pnas.0912628107.
- Trevors, J.T. & Psenner, R. (2001). "From self-assembly of life to present-day bacteria: a possible role for nanocells". FEMS Microbiol. Rev. 25 (5): 573–82. doi:10.1111/j.1574-6976.2001.tb00592.x. PMID 11742692.
- Segré, D.; Ben-Eli, D.; Deamer, D. & Lancet, D. (February–April 2001). "The Lipid World" (PDF). Origins of Life and Evolution of Biospheres 2001 31 (1–2): 119–45. doi:10.1023/A:1006746807104. PMID 11296516. Retrieved 2008-09-01.
- Cairns-Smith, A.G. (1968). "An approach to a blueprint for a primitive organism". In Waddington, C,H. Towards a Theoretical Biology 1. Edinburgh University Press. pp. 57–66.
- Ferris, J.P. (June 1999). "Prebiotic Synthesis on Minerals: Bridging the Prebiotic and RNA Worlds". Biological Bulletin. Evolution: A Molecular Point of View (Biological Bulletin, Vol. 196, No. 3) 196 (3): 311–314. doi:10.2307/1542957. JSTOR 1542957. PMID 10390828.
- Hanczyc, M.M.; Fujikawa, S.M. & Szostak, Jack W. (October 2003). "Experimental Models of Primitive Cellular Compartments: Encapsulation, Growth, and Division". Science 302 (5645): 618–622. Bibcode:2003Sci...302..618H. doi:10.1126/science.1089904. PMID 14576428. Retrieved 2008-09-01.
- Hartman, H. (October 1998). "Photosynthesis and the Origin of Life". Origins of Life and Evolution of Biospheres 28 (4–6): 512–521. Bibcode:1998OLEB...28..515H. doi:10.1023/A:1006548904157. Retrieved 2008-09-01.
- Penny, David; Poole, Anthony (December 1999). "The nature of the last universal common ancestor" (PDF). Current Opinion in Genetics & Development 9 (6): 672–677. doi:10.1016/S0959-437X(99)00020-9. PMID 10607605. (PDF)
- "Earliest Life". University of Münster. 2003. Retrieved 2006-03-28.
- Condie, Kent C. Earth as an Evolving Planetary System (2nd ed.). Burlington: Elsevier Science. ISBN 978-0-12-385228-1.
- Leslie, M. (2009). "On the Origin of Photosynthesis". Science 323 (5919): 1286–1287. doi:10.1126/science.323.5919.1286. PMID 19264999.
- Nisbet, E. G.; Sleep, N. H. (2001). "The habitat and nature of early life". Nature 409 (6823): 1083–1091. Bibcode:2001Natur.409.1083N. doi:10.1038/35059210. PMID 11234022.
- De Marais, David J.; D (September 8, 2000). "Evolution: When Did Photosynthesis Emerge on Earth?". Science 289 (5485): 1703–1705. doi:10.1126/science.289.5485.1703. PMID 11001737.
- Olson, John M. (February 2, 2006). "Photosynthesis in the Archean Era". Photosynthesis Research 88 (2 / May, 2006): 109–17. doi:10.1007/s11120-006-9040-5. PMID 16453059. Retrieved 2010-02-16.
- Fortey, Richard (September 1999) . "Dust to Life". Life: A Natural History of the First Four Billion Years of Life on Earth. New York: Vintage Books. ISBN 0-375-70261-X.
- Chaisson, Eric J. (2005). "Early Cells". Cosmic Evolution. Tufts University. Retrieved 2006-03-29.
- "Snowball Earth". snowballearth.org. 2006–2009. Retrieved 2012-04-13.
- "What caused the snowball earths?". snowballearth.org. 2006–2009. Retrieved 2012-04-13.
- Woese, Carl; Gogarten, J. Peter (October 21, 1999). "When did eukaryotic cells evolve? What do we know about how they evolved from earlier life-forms?". Scientific American. Retrieved 2012-04-13.
- Andersson, Siv G. E.; Zomorodipour, Alireza; Andersson, Jan O.; Sicheritz-Pontén, Thomas; Alsmark, U. Cecilia M.; Podowski, Raf M.; Näslund, A. Kristina; Eriksson, Ann-Sofie; Winkler, Herbert H.; Kurland, Charles G. (November 12, 1998). "The genome sequence of Rickettsia prowazekii and the origin of mitochondria". Nature 396 (6707): 133–140. Bibcode:1998Natur.396..133A. doi:10.1038/24094. PMID 9823893.
- "From prokaryotes to eukaryotes". Understanding evolution: your one-stop source for information on evolution. University of California Museum of Paleontology. Retrieved 2012-04-16.
- Berglsand, Kristin J.; Haselkorn, Robert (June 1991). "Evolutionary Relationships among the Eubacteria, Cyanobacteria, and Chloroplasts: Evidence from the rpoC1 Gene of Anabaena sp. Strain PCC 7120". Journal of Bacteriology 173 (11): 3446–3455. PMC 207958. PMID 1904436. (PDF)
- Dawkins 2004
- Takemura, Masaharu (May 2001). "Poxviruses and the origin of the eukaryotic nucleus". Journal of Molecular Evolution 52 (5): 419–425. doi:10.1007/s002390010171. PMID 11443345.
- Bell, Philip J (September 2001). "Viral eukaryogenesis: was the ancestor of the nucleus a complex DNA virus?". Journal of Molecular Evolution 53 (3): 251–256. doi:10.1007/s002390010215. PMID 11523012.
- Gabaldón, Toni; Berend Snel; Frank van Zimmeren; Wieger Hemrika; Henk Tabak; Martijn A. Huynen (March 23, 2006). "Origin and evolution of the peroxisomal proteome" (PDF). Biology Direct 1 (1): 8. doi:10.1186/1745-6150-1-8. PMC 1472686. PMID 16556314.
- Hanson RE, James L. Crowley, Samuel A. Bowring, Jahandar Ramezani et al. (May 21, 2004). "Coeval Large-Scale Magmatism in the Kalahari and Laurentian Cratons During Rodinia Assembly". Science 304 (5674): 1126–1129. Bibcode:2004Sci...304.1126H. doi:10.1126/science.1096329. PMID 15105458. Retrieved 2012-04-13.
- Li, Z.X.; Bogdanova, S.V.; Collins, A.S.; Davidson, A.; De Waele, B.; Ernst, R.E.; Fitzsimons, I.C.W.; Fuck, R.A.; Gladkochub, D.P.; Jacobs, J.; Karlstrom, K.E.; Lu, S.; Natapov, L.M.; Pease, V.; Pisarevsky, S.A.; Thrane, K.; Vernikovsky, V. (2008). "Assembly, configuration, and break-up history of Rodinia: A synthesis". Precambrian Research 160 (1–2): 179–210. doi:10.1016/j.precamres.2007.04.021.
- Chaisson, Eric J. (2005). "Ancient Fossils". Cosmic Evolution. Tufts University. Retrieved 2006-03-31.
- Bhattacharya, Debashish; Medlin, Linda (1998). "Algal Phylogeny and the Origin of Land Plants". Plant Physiology 116 (1): 9–15. doi:10.1104/pp.116.1.9. (PDF)
- Kearey, Philip; Keith A. Klepeis; Frederick J. Vine (2009). Global tectonics. (3rd ed.). Oxford: Wiley-Blackwell. ISBN 9781405107778.
- Torsvik, T. H. (30 May 2003). "The Rodinia Jigsaw Puzzle". Science 300 (5624): 1379–1381. doi:10.1126/science.1083469. PMID 12775828.
- Zhao, Guochun; Cawood, Peter A.; Wilde, Simon A.; Sun, M. (2002). "Review of global 2.1–1.8 Ga orogens: implications for a pre-Rodinia supercontinent". Earth-Science Reviews 59 (1–4): 125–162. Bibcode:2002ESRv...59..125Z. doi:10.1016/S0012-8252(02)00073-9.
- Zhao, Guochun; Sun, M.; Wilde, Simon A.; Li, S.Z. (2004). "A Paleo-Mesoproterozoic supercontinent: assembly, growth and breakup". Earth-Science Reviews 67 (1–2): 91–123. Bibcode:2004ESRv...67...91Z. doi:10.1016/j.earscirev.2004.02.003.
- McElhinny, Michael W.; Phillip L. McFadden (2000). Paleomagnetism continents and oceans (2nd ed.). San Diego: Academic Press. ISBN 9780124833555.
- Dalziel, I.W.D. (1995). "Earth before Pangea". Scientific American 1 (1): 58–63. Bibcode:1995SciAm.272a..58D. doi:10.1038/scientificamerican0195-58.
- "Snowball Earth: New Evidence Hints at Global Glaciation 716.5 Million Years Ago". Science Daily. Mar 4, 2010. Retrieved April 18, 2012.
- "'Snowball Earth' Hypothesis Challenged". Retrieved 29 September 2012.
- Hoffman, P.F.; Kaufman, A.J.; Halverson, G.P.; Schrag, D.P. (1998). "A Neoproterozoic Snowball Earth". Science 281 (5381): 1342–1346. Bibcode:1998Sci...281.1342H. doi:10.1126/science.281.5381.1342. PMID 9721097.
- "Two Explosive Evolutionary Events Shaped Early History Of Multicellular Life". Science Daily. Jan 3, 2008. Retrieved April 18, 2012.
- Xiao, S.; Laflamme, M. (2009). "On the eve of animal radiation: phylogeny, ecology and evolution of the Ediacara biota". Trends in Ecology and Evolution 24 (1): 31–40. doi:10.1016/j.tree.2008.07.015. PMID 18952316.
- Patwardhan, A.M. (2010). The Dynamic Earth System. New Delhi: PHI Learning Private Limited. p. 146. ISBN 978-81-203-4052-7.
- Runkel, Anthony C.; Mackey, Tyler J.; Cowan, Clinton A.; Fox, David L. (1 November 2010). "Tropical shoreline ice in the late Cambrian: Implications for Earth's climate between the Cambrian Explosion and the Great Ordovician Biodiversification Event". GSA Today: 4–10. doi:10.1130/GSATG84A.1.
- Palmer, Allison R. (1984). "The biomere problem: Evolution of an idea". Journal of Paleontology 58 (3): 599–611.
- Hallam, A.; Wignall, P.B. (1997). Mass extinctions and their aftermath (Repr. ed.). Oxford [u.a.]: Oxford Univ. Press. ISBN 978-0-19-854916-1.
- "Pannotia". UCMP Glossary. Retrieved 2006-03-12.
- "The Mass Extinctions: The Late Ordovician Extinction". BBC. Archived from the original on 2006-02-21. Retrieved 2006-05-22.
- Murphy, Dennis C. (May 20, 2006). "The paleocontinent Euramerica". Devonian Times. Retrieved April 18, 2012.
- Battistuzzi, Fabia U.; Feijao, Andreia; Hedges, S. Blair (2004). "A genomic timescale of prokaryote evolution: insights into the origin of methanogenesis, phototrophy, and the colonization of land". BMC Evolutionary Biology 4: 44. doi:10.1186/1471-2148-4-44. PMC 533871. PMID 15535883.
- Pisani, Davide; Poling, Laura L.; Lyons-Weiler, Maureen; Hedges, S. Blair (January 19, 2004). "The colonization of land by animals: molecular phylogeny and divergence times among arthropods". BMC Biology 2: 1. doi:10.1186/1741-7007-2-1. PMC 333434. PMID 14731304.
- Lieberman, Bruce S. (2003). "Taking the Pulse of the Cambrian Radiation". Integrative and Comparative Biology 43 (1): 229–237. doi:10.1093/icb/43.1.229. PMID 21680426.
- "The Mass Extinctions: The Late Cambrian Extinction". BBC. Retrieved 2006-04-09.
- Landing, E.; Bowring, S. A.; Davidek, K. L.; Fortey, R. A.; Wimbledon, W. A. P. (2000). "Cambrian–Ordovician boundary age and duration of the lowest Ordovician Tremadoc Series based on U–Pb zircon dates from Avalonian Wales". Geological Magazine 137 (5): 485–494. doi:10.1017/S0016756800004507. (abstract)
- Fortey, Richard (September 1999) . "Landwards, Humanity". Life: A Natural History of the First Four Billion Years of Life on Earth. New York: Vintage Books. pp. 138–140, 300. ISBN 0-375-70261-X.
- Heckman, D. S.; D. M. Geiser; B. R. Eidell; R. L. Stauffer; N. L. Kardos; S. B. Hedges (August 10, 2001). "Molecular evidence for the early colonization of land by fungi and plants". Science 293 (5532): 1129–1133. doi:10.1126/science.1061457. PMID 11498589. (abstract)
- Johnson, E. W.; D. E. G. Briggs; R. J. Suthren; J. L. Wright; S. P. Tunnicliff (1 May 1994). "Non-marine arthropod traces from the subaereal Ordivician Borrowdale volcanic group, English Lake District". Geological Magazine 131 (3): 395–406. doi:10.1017/S0016756800011146. Retrieved 2012-04-13. (abstract)
- MacNaughton, Robert B.; Jennifer M. Cole; Robert W. Dalrymple; Simon J. Braddy; Derek E. G. Briggs; Terrence D. Lukie (2002). "First steps on land: Arthropod trackways in Cambrian-Ordovician eolian sandstone, southeastern Ontario, Canada". Geology 30 (5): 391–394. Bibcode:2002Geo....30..391M. doi:10.1130/0091-7613(2002)030<0391:FSOLAT>2.0.CO;2. ISSN 0091-7613. (abstract)
- Clack, Jennifer A. (December 2005). "Getting a Leg Up on Land". Scientific American 293 (6): 100–7. Bibcode:2005SciAm.293f.100C. doi:10.1038/scientificamerican1205-100. PMID 16323697. Retrieved 2012-04-13.
- McGhee, Jr, George R. (1996). The Late Devonian Mass Extinction: the Frasnian/Famennian Crisis. Columbia University Press. ISBN 0-231-07504-9.
- Willis, K. J.; J. C. McElwain (2002). The Evolution of Plants. Oxford: Oxford University Press. p. 93. ISBN 0-19-850065-3.
- "Plant Evolution". Evolution for teaching. University of Waikato. October 2004. Retrieved April 18, 2012.
- "The Day the Earth Nearly Died". Horizon. BBC. 2002. Retrieved 2006-04-09.
- "Big crater seen beneath ice sheet". BBC News. 3 June 2006. Retrieved April 18, 2012.
- Wright, Jo (1999). "New Blood". Walking with Dinosaurs. Episode 1. http://www.bbc.co.uk/sn/prehistoric_life/dinosaurs/chronology/220mya1.shtml.
- "The Mass Extinctions: The Late Triassic Extinction". BBC. Archived from the original on 2006-08-13. Retrieved 2006-04-09.
- "Archaeopteryx: An Early Bird". University of California, Berkeley Museum of Paleontology. 1996. Retrieved 2006-04-09.
- Soltis, Pam; Doug Soltis; Christine Edwards (2005). "Angiosperms". The Tree of Life Project. Retrieved 2006-04-09.
- Chaisson, Eric J. (2005). "Recent Fossils". Cosmic Evolution. Tufts University. Retrieved 2006-04-09.
- Reed, David L.; Smith, Vincent S.; Hammond, Shaless L.; Rogers, Alan R. et al. (2004). "Genetic Analysis of Lice Supports Direct Contact between Modern and Archaic Humans". PLoS Biology 2 (11): e340. doi:10.1371/journal.pbio.0020340. PMC 521174. PMID 15502871.
- Goren-Inbar, Naama; Nira Alperson; Mordechai E. Kislev; Orit Simchoni; Yoel Melamed; Adi Ben-Nun; Ella Werker (2004-04-30). "Evidence of Hominin Control of Fire at Gesher Benot Ya'aqov, Israel". Science 304 (5671): 725–727. Bibcode:2004Sci...304..725G. doi:10.1126/science.1095443. PMID 15118160. Retrieved 2012-04-13. (abstract)
- McClellan (2006). Science and Technology in World History: An Introduction. Baltimore, Maryland: JHU Press. ISBN 0-8018-8360-1. Page 8-12
- McNeill 1999
- Gibbons, Ann (2003). "Oldest Members of Homo sapiens Discovered in Africa". Science 300 (5626): 1641. doi:10.1126/science.300.5626.1641. PMID 12805512. Retrieved 2012-04-13. (abstract)
- Hopfe, Lewis M. (1987) . "Characteristics of Basic Religions". Religions of the World (4th ed.). New York: MacMillan Publishing Company. pp. 17, 17–19. ISBN 0-02-356930-1.
- "Chauvet Cave". Metropolitan Museum of Art. Retrieved 2006-04-11.
- Patrick K. O’Brien, ed. (2003) . "The Human Revolution". Atlas of World History (concise ed.). New York: Oxford University Press. p. 16. ISBN 0-19-521921-X.
- Dawkins, Richard (1989) . "Memes: the new replicators". The Selfish Gene (2nd ed.). Oxford: Oxford University Press. pp. 189–201. ISBN 0-19-286092-5.
- Tudge, Colin (1998). Neanderthals, Bandits and Farmers: How Agriculture Really Began. London: Weidenfeld & Nicolson. ISBN 0-297-84258-7.
- Diamond, Jared (1999). Guns, Germs, and Steel. W. W. Norton & Company. ISBN 0-393-31755-2.
- "Human Spaceflight and Exploration – European Participating States". ESA. 2006. Retrieved 2006-03-27.
- "Expedition 13: Science, Assembly Prep on Tap for Crew". NASA. January 11, 2006. Retrieved 2006-03-27.
- Dalrymple, G. B. (1991). The Age of the Earth. California: Stanford University Press. ISBN 0-8047-1569-6.
- Dalrymple, G. Brent (2001). "The age of the Earth in the twentieth century: a problem (mostly) solved". Geological Society, London, Special Publications 190 (1): 205–221. Bibcode:2001GSLSP.190..205D. doi:10.1144/GSL.SP.2001.190.01.14. Retrieved 2012-04-13.
- Dawkins, Richard (2004). The Ancestor's Tale: A Pilgrimage to the Dawn of Life. Boston: Houghton Mifflin Company. ISBN 0-618-00583-8.
- Gradstein, F. M.; Ogg, James George; Smith, Alan Gilbert, eds. (2004). A Geological Time Scale 2004. Reprinted with corrections 2006. Cambridge University Press. ISBN 978-0-521-78673-7.
- Gradstein, Felix M.; Ogg, James G.; van Kranendonk, Martin (2008). On the Geological Time Scale 2008 (PDF) (Report). International Commission on Stratigraphy. Fig. 2. Retrieved 20 April 2012.
- Levin, H. L. (1987). The Earth through time (3rd ed.). Saunders College Publishing. ISBN 0-03-008912-3.
- Lunine, J. I. (1999). Earth: evolution of a habitable world. United Kingdom: Cambridge University Press. ISBN 0-521-64423-2.
- McNeill, Willam H. (1999) . A World History (4th ed.). New York: Oxford University Press. ISBN 0-19-511615-1.
- Melosh, H. J.; Vickery, A. M. & Tonks, W. B. (1993). Impacts and the early environment and evolution of the terrestrial planets, in Levy, H.J. & Lunine, J.I. (eds.): Protostars and Planets III, University of Arizona Press, Tucson, pp. 1339–1370.
- Stanley, Steven M. (2005). Earth system history (2nd ed.). New York: Freeman. ISBN 978-0-7167-3907-4.
- Stern, T. W.; Bleeker, W. (1998). "Age of the world's oldest rocks refined using Canada's SHRIMP: The Acasta Gneiss Complex, Northwest Territories, Canada". Geoscience Canada 25: 27–31.
- Wetherill, G. W. (1991). "Occurrence of Earth-Like Bodies in Planetary Systems". Science 253 (5019): 535–538. Bibcode:1991Sci...253..535W. doi:10.1126/science.253.5019.535. PMID 17745185.
- Cosmic Evolution – a detailed look at events from the origin of the universe to the present
- Valley, John W. "A Cool Early Earth?" Scientific American. 2005 October 58–65. – discusses the timing of the formation of the oceans and other major events in Earth’s early history.
- Davies, Paul. "Quantum leap of life". The Guardian. 2005 December 20. – discusses speculation on the role of quantum systems in the origin of life
- Evolution timeline (uses Shockwave). Animated story of life shows everything from the big bang to the formation of the earth and the development of bacteria and other organisms to the ascent of man.