The Precambrian Earth: Tempos and Events Edited by EG. Eriksson, W. Altermann, D.R. Nelson, W.U. Mueller and O. Catuneanu Developments in Precambrian Geology, Vol. 12 (K.C. Condie, Series Editor) 9 2004 Elsevier B.V. All rights reserved
Chapter 9
TOWARDS A SYNTHESIS
RG. ERIKSSON, O. CATUNEANU, D.R. NELSON, W.U. MUELLER AND W. ALTERMANN
The principal theme of this book is change through time, or tempos and events in the Precambrian (Preface). Each chapter portrays a different part of the Earth's history but there is a unifying theme: Earth's evolution. Chapter 1 explains the celestial origin of our planet and the early development of the Earth into core, mantle, crust and primitive atmosphere. Chapter 2 discusses the generation of continental crust, with the emphasis on granite-greenstone terranes. Chapter 3 builds further upon its predecessor, empha- sising the interaction between tectonism and mantle plumes through Precambrian time. Chapter 4 examines the volcanic attributes of the Archaean Earth and how they may have changed, as exemplified by plume-generated komatiites, the constant interaction between arc-plume volcanism and subaqueous caldera formation. Chapter 5 deals with the evolution of Earth's atmosphere and hydrosphere, and chapter 6 with related concepts of the evolu- tion of Precambrian life and bio-geology. Chapter 7 details sedimentation regimes through Precambrian time, while chapter 8 discusses the application of sequence stratigraphy to the Precambrian rock record.
9.1. EVOLUTION OF THE SOLAR SYSTEM AND THE EARLY EARTH
Investigation of pre-4 Ga Earth history relies largely upon study of the most ancient rocks thus far identified, and upon modelling of the differentiation of Earth's chemical reservoirs (Nelson, section 1.1). As the known preserved rock record dates from 4030 Ma (Stern and Bleeker, 1998; Bowring and Williams, 1999), more than 500 My of Earth's ear- liest evolution remains essentially speculative. It was only with the identification within meteorites of daughter products from radiogenic decay of long-extinct nuclides (firstly by Reynolds, 1960), that the timing of accretion and differentiation of the early Earth could be investigated (summarised by Nelson, in section 1.2). The short-lived parent nu- clides were synthesised during supernova explosions shortly before formation of our solar system; their short half-lives enable precise determination of the chronology of the earli- est history of the solar system (section 1.2). Collision and amalgamation of smaller, rocky planetesimals within a protoplanetary disk formed the terrestrial planets, including Earth. As proto-Earth and its Moon grew by these violent accretion processes, earlier differenti- ation products were largely obliterated; with the growth of embryonic planets the impact rate decreased and concomitantly, the likelihood of preservation of fragments of the early
Earth increased.
Current evidence (section 1.2) suggests that short-lived nuclides with atomic masses
< 140, together with a part of the heavy elements in our solar system, were synthesised
during a core-collapse supernova event at c. 4571 Ma (Lugmair and Shukolyukov, 2001;
Gilmour and Saxton, 2001 ). Formation of the Sun and solar system may have been initiated
by shock waves from this supernova explosion (probably one of a number of successive
such events); injection of short-lived nuclides into a nearby interstellar gas and dust cloud
may have triggered its collapse, forming a proto-Sun of radius c. five times its present
value, over a time period of < 105 years (Cameron, 1995; Nelson, section 1.2). Progressive
collapse from inner to outer parts of the cloud, together with conservation of angular
momentum, caused it to spin faster; colliding gas and dust particles orbiting the proto-
Sun in the same direction lost their energy, causing flattening of the cloud, especially near
its centre.
Gravitational energy was converted to heat during collapse of the nebula. At some time
during collapse, the density and temperature became high enough for hydrogen burning
to commence, and the proto-Sun began its violent T-Tauri phase (Cameron, 1995;
Nelson, section 1.2). More abundant Fe, Ni and silicate-rich components condensed within
lower temperature parts of the nebula in its medial to central parts, while volatile elements
(e.g., water, ammonia, methane ice) condensed in cold, outer parts of the accretionary disk.
Volatiles were possibly carried by the solar wind from inner to outer reaches of the emerging
solar system (Shu et al., 1994).
Spectroscopy and simulation modelling suggest only a few million years from star formation
and large scale accretion of disks into the young solar-type T-Tauri stars. Larger
planetesimals may have formed within ~< 2 My of solar system formation (Hutchison et al.,
2001). Coagulation consequent upon icy particle collisions within an ice sublimation belt
in the cold outer parts of the nebula being more efficient than that between metal or silicate
particles, large gas-rich proto-planets (Jupiter and Saturn precursors) formed before
the nebula gas dissipated (Cameron, 1995). Collision and amalgamation of chemically refractory
dust particles within the inner part of the disk occurred more slowly. Collisions of
smaller planetesimals with larger bodies continued to rework early planetary-sized bodies
for at least a further 100 My, and triggered large scale melting and magmatic differentiation
of silicate components of the larger planetesimals. Dating of meteoritic remnants from
these early differentiated planetary bodies indicates that planetesimals of at least 10s-100s
of kilometres in diameter underwent internal magmatic differentiation within < 10 My
after the supernova event. 187Re-187Os isotopic data from pallasites and iron meteorites
(Morgan et al., 1995; Shen et al., 1998; Horan et al., 1998) suggest formation of metallic
cores within c. ~< 50 My of formation of the solar system. There is intriguing evidence for
hydrothermal alteration processes involving aqueous fluids within planetesimals ~< 2 My
after solar system formation.
Planetary embryos had thus existed within <~ 5 My of the supernova event that triggered
formation of the solar system. Accretion of these embryos within a c. 0.5-2.5 AU range
of the Sun (Wetherill, 1994) was largely responsible for formation of the terrestrial plan