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How and When Granitoid Magmas Appeared LITHOSPHERE (RUSSIA), 2018, volume 18, No. 5A, pp. 5–19 EARLY EVOLUTION OF EARTH AND BEGINNING OF ITS GEOLOGICAL HISTORY: HOW AND WHEN GRANITOID MAGMAS APPEARED Mikhail I. Kuzmin1, Vladimir V. Yarmolyuk2, Alexander B. Kotov3 1Institute of Geochemistry SB RAS, 1A Favorsky St., Irkutsk 664033, Russia, e-mail: [email protected] 2Institute of Geology of Ore Deposits, Petrography, Mineralogy and Geochemistry (IGEM RAS), 35 Staromonetny lane, Moscow 119017, Russia 3Institute of Precambrian Geology and Geochronology, Russian Academy of Sciences (IGGD RAS), 2 Makarova quay, St.Petersburg 199034, Russia Received 17.11.2017, accepted 11.01.2018 Earth has a number of differences from the planets of the Solar System, as well as other stellar-planetary systems, which were acquired during its formation and geological history. The early Chaotian aeon was marked by Earth’s accretion, the differentiation of its primary material into a mantle and a core, as well as the by formation of its satellite (Moon). Earth’s geological history began 4500 million years ago in the Hadean aeon. At that time, the endogenous processes on Earth were largely controlled by meteorite and asteroid bombardments, which caused large-scale melting and differentiation of its up- per layers. In magmatic chambers, differentiation proceeded until the appearance of granitoid melts. The Hadean continen- tal crust was almost completely destroyed by meteorite bombardments, with the last heavy bombardment occurring at the end of the Hadean aeon (4000–3900 Ma). Conclusions about the geological situation of this aeon can be drawn only from the preserved Hadean zircons. In particular, their geochemical features indicate that Earth had an atmosphere. The Hadean aeon was replaced by the Archaean one, starting from which the processes of self-organisation were predominant on Earth. At that time, a crust composed of komatiite-basalt and tonalite-trondhjemite-granodiorite (TTG) rock series was forming. Its formation was driven by sagduction processes – vertical growth of the crust over rising mantle plumes. Thus, the low- er basaltic crust subsided into the mantle, eclogitised and melted, which led to the appearance of sodium TTG rocks se- ries. At the end of the Archaean aeon (3.1–3.0 Ga), lid tectonics, which determined the structure and development of the Archaean crust, was replaced by small-plate tectonics that later evolved into modern plate tectonics combined with man- tle plume tectonics. Keywords: Chaotian and Hadean aeons, Archaean period, lid tectonics, plume tectonics, sagduction, mantle convection INTRODUCTION Hadean and Archaean aeons will be discussed in this work. Earth is different from other terrestrial planets of the Knowing when the tectonics of lithospheric plates Solar System. What is more, it has no analogues among got started is of great importance for understanding the the planets of 600 stellar-planetary systems that have geological history of our planet. The mechanisms of been discovered in recent decades. It is not a coinciden- endogenous processes stipulated by this theory are well ce that the authors of the article “Born from the cha- studied. They describe the formation of basic geologi- os” [S. Batygin et al., 2016] called Earth a black sheep. cal structures, such as continents, oceans, orogens. Not An outstanding geologist K. Condy identified a number coincidentally, in 2008 following a corresponding con- of characteristics inherent to Earth [Condie, 2011], ference the Geological Society of America published which allowed it to become the cradle of humankind. a special issue, which contained articles by a number The characteristic features of our planet, including its of prominent geologists covering the onset of plate size and mass, a near-circular orbit, existence of a sat- tectonics on Earth. In his article published in this is- ellite (Moon), were acquired during the birth of the So- sue K. Condi writes: “It is unlikely that plate tecton- lar System and then during the Chaotian aeon [Gold- ics began on Earth as a single global ‘event’ at a dis- blatt et al., 2010]. Earth acquired its other important tinct time, but rather it is probable that it began local- characteristics, such as the division of Earth’s interi- ly and progressively became more widespread from the or into a number of layers, during its subsequent histo- early to the late Archaean”. However, even today, such ry. The above-mentioned layers include the continental well-known Japanese geologists as S. Maruyama and crust containing a significant amount of granitoids, as his colleague [Maruyama, Ebisuzaki, 2017], establish well as the atmosphere and hydrosphere. The first gran- the exact start date of plate tectonics (4.37–4.20 Ga) ites on Earth appeared in the Hadean aeon, while gran- when proposing a new model of the Earth’s formation itoids, well-preserved to our days, were already fairly (ABEL). Similar start dates of the plate tectonics on widespread in the Archaean aeon. The Earth’s birth, its Earth are proposed in the works of other geologists. In formation as a planet, as well as possible mechanisms the same issue published by the Geological Society of for the development of the first granitoid rocks in the America, R. Stern wrote more cautiously and prudent- 5 6 Kuzmin et al. ly about the significance of the early tectonic style on tures associated the formation of the Solar System and Earth saying that we will not be able to understand the Earth in particular. current system until we know when the current tectonic The calculations of astronomers and planetary sci- style began and what preceded it [Stern, 2008]. entists show that a star (proto-Sun) appeared in the cen- tre of the nebula under the influence of gravity in less ORIGIN OF THE SOLAR SYSTEM AND EARLY than 100 thousand years. The proto-Sun was surround- STAGES OF ITS EVOLUTION ed by a wide disk of gas and dust – a protoplanetary disk [Lin, 2008], which served as the building material The solar system originated 4568 million years for the planets of the Solar System. When moving, par- ago in a massive dust and gas cloud. The reason for ticles of dust and gas collided and slowed down, with the formation of this protosolar nebula, which must many of them spiralling onto the proto-Star. Upon col- have included a large variety of chemical elements lision, solid particles heated, whereas water and other along with various short- and long-lived isotopes, is volatiles having a low boiling point evaporated. This of the essence here. This cloud (nebula) could have resulted in a natural boundary between the areas of originated from the explosion of a supernova in the the protoplanetary disk, with the predominance of sol- vicinity of the future Solar System. Due to nucle- id particles in one part and volatiles in the other. This ar reactions, the explosion of a massive star brought boundary (a region between the orbits of Mars and Ju- about the synthesis (nucleosynthesis) and, naturally, piter) is referred to as the snow line, dividing the Solar the appearance of various elements, in particular, ra- System into the inner region, where the terrestrial plan- dioactive isotopes. This explosion could have induced ets were formed, and the outer one, where the gas giant the condensation of interstellar matter resulting from planets were located [Batygin et al., 2016]. This sep- gravitational compression. Short-lived isotopes and aration occurred 2 million years after the onset of the their decay products help to identify a number of fea- Solar System formation (Fig. 1). Fig. 1. Initial stage of the Solar System’s evolution 4568 Ma ago [Batygin et al., 2016]. The beginning of the Chaotian aeon of the Solar System; birth of the proto-Sun; formation of the internal area consisting of stony fragments; snow lines – internal border of the external gas-ice region, where giant planets Saturn and Jupiter were formed 2 mil- lion years after the birth of the Solar System. LITHOSPHERE (RUSSIA) volume 18 No. 5A 2018 Early evolution of Earth, beginning of its geological history, the granitoid magmas 7 Thus, in the first 2 million years of the Solar Sys- first crust in the geological history of our planet. Ap- tem’s history, numerous planetary embryos (planetes- proximately 3.9 billion years ago, the giant planets set- imals), as well as giant planets beyond the snow line tled down. Thus, the Solar System acquired its current (Jupiter and Saturn) were formed. In this respect, the structure [Batygin et al., 2016]. Solar System is very different from other planetary sys- Astronomers distinguish a chaotic period in the So- tems, where similar giants are located much closer to lar System’s development (beginning of Earth’s forma- the sun. According to K. Batygin and his colleagues tion to 4.0–3.9 billion years). In the geological liter- [2016], such features of the Solar System are prod- ature, this period is divided into two aeons: Chaotian ucts of its youth, which included more drama and cha- (4568–4500 Ma) and Hadean (4500–4000 / 3900 Ma) os. The complex interaction of giant peripheral plan- [Goldblatt et al., 2010]. ets constituted an important part of the primary cha- os. For the first time, this was noted in the computer EARLY STAGES OF EARTH’S FORMATION model of F. Masset and M. Snellgrove [Masset, Snell- AND EVOLUTION grove, 2001], who described the simultaneous evolu- tion of Saturn’s and Jupiter’s orbits in the protoplane- Chaotian Eon (4568–4500 Ma) tary disk. These studies showed that due to inward mi- gration, the giant planets acquired a certain mutual con- The accretion of Earth took place in this period. As figuration, due to which they were able to influence the little as 11 million years after the onset of its formation, protoplanetary disk.
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