Rodinia formed at c. 1.23 Ga by accretion and collision of fragments produced by breakup of an older supercontinent, Columbia, assembled by global-scale 2.0-1.8 Ga collisional events.
Rodinia broke up in the Neoproterozoic with its continental fragments reassembled to form Pannotia 633-573 million years ago. In contrast with Pannotia, little is known yet about the exact configuration and geodynamic history of Rodinia. Paleomagnetic evidence provides some clues to the paleolatitude of individual pieces of the Earth's crust, but not to their longitude, which geologists have pieced together by comparing similar geologic features, often now widely dispersed.
The extreme cooling of the global climate around 717-635 million years ago (the so-called Snowball Earth of the Cryogenianperiod) and the rapid evolution of primitive life during the subsequent Ediacaran and Cambrian periods are thought to have been triggered by the breaking up of Rodinia or to a slowing down of tectonic processes.
Rodinia at 900 Ma. "Consensus" reconstruction of Li et al. 2008.
Since then, many alternative reconstructions have been proposed for the configuration of the cratons in this supercontinent. Most of these reconstructions are based on the correlation of the orogens on different cratons. Though the configuration of the core cratons in Rodinia is now reasonably well known, recent reconstructions still differ in many details. Geologists try to decrease the uncertainties by collecting geological and paleomagnetical data.
SWEAT-Configuration (Southwest US-East Antarctica craton): Antarctica is on the Southwest of Laurentia and Australia is at the North of Antarctica.
AUSWUS-Configuration (Australia-western US): Australia is at the West of Laurentia.
AUSMEX-Configuration (Australia-Mexico): Australia is at the location of current day Mexico relative to Laurentia.
The "Missing-link" model by Li et al. 2008 which has South China between Australia and the west coast of Laurentia. A revised "Missing-link" model is proposed in which Tarim Block serves as an extended or alternative missing-link between Australia and Laurentia.
Little is known about the paleogeography before the formation of Rodinia. Paleomagnetic and geologic data are only definite enough to form reconstructions from the breakup of Rodinia onwards. Rodinia is considered to have formed between 1.3 and 1.23 billion years ago and broke up again before 750 million years ago. Rodinia was surrounded by the superocean geologists call Mirovia (from Russian ?, mirovoy, meaning "global").
According to J.D.A. Piper, Rodinia is one of two models for the configuration and history of the continental crust in the latter part of Precambrian times. The other is Paleopangea, Piper's own concept. Piper proposes an alternative hypothesis for this era and the previous ones. This idea rejects that Rodinia ever existed as a transient supercontinent subject to progressive break-up in the latter part of Proterozoic times and instead that this time and earlier times were dominated by a single, persistent "Paleopangaea" supercontinent. As evidence, he suggests an observation that the palaeomagnetic poles from the continental crust assigned to this time conform to a single path between 825 and 633 million years ago and latterly to a near-static position between 750 and 633 million years. This latter solution predicts that break-up was confined to the Ediacaran period and produced the dramatic environmental changes that characterised the transition between Precambrian and Phanerozoic times.
In 2009 UNESCO's IGCP project 440, named 'Rodinia Assembly and Breakup', concluded that Rodinia broke up in four stages between 825-550 Ma:
The break up was initiated by a superplume around 825-800 Ma whose influence--such as crustal arching, intense bimodal magmatism, and accumulation of thick rift-type sedimentary successions--have been recorded in South Australia, South China, Tarim, Kalahari, India, and the Arabian-Nubian Craton.
Rifting progressed in the same cratons 800-750 Ma and spread into Laurentia and perhaps Siberia. India (including Madagascar) and the Congo-Säo Francisco Craton were either detached from Rodinia during this period or simply never were part of the supercontinent.
As the central part of Rodinia reached the Equator around 750-700 Ma, a new pulse of magmatism and rifting continued the disassembly in western Kalahari, West Australia, South China, Tarim, and most margins of Laurentia.
650-550 Ma several events coincided: the opening of the Iapetus Ocean; the closure of the Braziliano, Adamastor, and Mozambique oceans; and the Pan-African orogeny. The result was the formation of Gondwana.
The Rodinia hypothesis assumes that rifting did not start everywhere simultaneously. Extensive lava flows and volcanic eruptions of Neoproterozoic age are found on most continents, evidence for large scale rifting about 750 million years ago. As early as 850 and 800 million years ago, a rift developed between the continental masses of present-day Australia, East Antarctica, India and the Congo and Kalahari cratons on one side and later Laurentia, Baltica, Amazonia and the West African and Rio de la Plata cratons on the other. This rift developed into the Adamastor Ocean during the Ediacaran.
Around 550 million years ago, on the boundary between the Ediacaran and Cambrian, the first group of cratons eventually fused again with Amazonia, West Africa and the Rio de la Plata cratons. This tectonic phase is called the Pan-African orogeny. It created a configuration of continents that would remain stable for hundreds of millions of years in the form of the continent Gondwana.
In a separate rifting event about 610 million years ago (halfway in the Ediacaran period), the Iapetus Ocean formed. The eastern part of this ocean formed between Baltica and Laurentia, the western part between Amazonia and Laurentia. Because the exact moments of this separation and the partially contemporaneous Pan-African orogeny are hard to correlate, it might be that all continental mass was again joined in one supercontinent between roughly 600 and 550 million years ago. This hypothetical supercontinent is called Pannotia.
Influence on paleoclimate and life
Unlike later supercontinents, Rodinia would have been entirely barren. Rodinia existed before complex life colonized dry land. Based on sedimentary rock analysis Rodinia's formation happened when the ozone layer was not as extensive as it is today. Ultraviolet light discouraged organisms from inhabiting its interior. Nevertheless, its existence did significantly influence the marine life of its time.
Low temperatures may have been exaggerated during the early stages of continental rifting. Geothermal heating peaks in crust about to be rifted; and since warmer rocks are less dense, the crustal rocks rise up relative to their surroundings. This rising creates areas of higher altitude, where the air is cooler and ice is less likely to melt with changes in season, and it may explain the evidence of abundant glaciation in the Ediacaran period.
The eventual rifting of the continents created new oceans and seafloor spreading, which produces warmer, less dense oceanic lithosphere. Due to its lower density, hot oceanic lithosphere will not lie as deep as old, cool oceanic lithosphere. In periods with relatively large areas of new lithosphere, the ocean floors come up, causing the eustatic sea level to rise. The result was a greater number of shallower seas.
^See for example the correlation between the North American Grenville and European Dalslandian orogenies in Ziegler 1990, p. 14; for the correlation between the Australian Musgrave orogeny and the Grenville orogeny see Wingate, Pisarevsky & Evans 2002, Implications for Rodinia reconstructions, pp. 124-126; fig. 5, p. 127
^Wen, Bin; Evans, David A. D.; Li, Yong-Xiang (2017-01-15). "Neoproterozoic paleogeography of the Tarim Block: An extended or alternative "missing-link" model for Rodinia?". Earth and Planetary Science Letters. 458: 92-106. Bibcode:2017E&PSL.458...92W. doi:10.1016/j.epsl.2016.10.030.