Evolution of the Solar System

Solar system abundances are a cornerstone of our understanding of the origin and evolution of the solar system and the elements from which it formed. To understand... 

Several proposals have been made about the origin of the matter from which the earth and the solar system have been formed. These proposals are mainly based on the isotopie eomposition. The supernova hypothesis explains the presence of heavy nuelei in the solar system by a supernova explosion some time before the evolution of the solar system. This hypothesis is supported by the isotopie analysis of meteorites whieh shows an anomaly in the Xe eontent. This anomaly is attributed to the decay of (ti/2 = 1.57 10 y) which must have been present during the evolution of the solar system. 

Wark D. A. and Lovering J. F. (1977) Marker events in the early evolution of the solar system evidence from rims on Ca-Al-rich inclusions from carbonaceous chondrites. Proc. 8th Lunar Planet. Sci. Cortf. 95-112. 

Alfven H. and Arrhenius G. (1976) Evolution of the Solar System. NASA, 599p. 

The cratered surfaces of asteroids and terrestrial planets underscore the importance of impacts for the formation and evolution of the solar system. Early in the history of the solar system such collisions were the mechanism for accretion of planetesimals and finally the planets themselves [1], The effects of these still ongoing collisions are visible from the megascopic down to the submicroscopic length scale, i.e., they range from large impact craters and their ejecta blankets down to shock-metamorphic effects in minerals [2-4]. These effects form as a result of the interaction of strong shock waves with the affected solid matter. 

BCnowledge about the evolution of the solar system is mainly based on meteorite investigations. With the exception of material brought to earth by spacecrafts from the... 

What are the origins of Earth and other planets in the solar system Questions such as these have challenged philosophers and scientists for centuries. One of the earliest theories for the formation and evolution of the solar system was proposed by the French philosopher and mathematician Rene Descartes (1596-1650). Descartes suggested that the Sun and planets originally formed out of a swirling mass of matter that slowly condensed into one very large body (the Sun) and other smaller bodies (the planets) at various distances from the Sun. With some important refinements, that theory is one most astronomers subscribe to today. 

Using the classical methods of Celestial Mechanics, we can expand the distance A in the Hamiltonian (19) as a function of the Poincare variables, and we can calculate the so called secular system at order two in the masses (used, for instance, in Laskar 1988 in a model with 8 planets, to study the long term evolution of the solar system). In the secular system the dependency on the angles Ai, A2 (which evolve much faster than the other Poincare variables) is dropped out by simply averaging the Hamiltonian over the angles themselves. Thus, the actions Ai, A2 are first integrals for the secular system, which are replaced with their numerical values corresponding to the data for the real system Sun-Jupiter-Saturn at a fixed initial time. Therefore, we can actually expand the secular Hamiltonian as a power series in the form... 

Although equilibrium chemical processes have been widely used to model the early evolution of the Solar System, there is growing evidence, particularly in isotopic abundances, that non-equilibrium chemistry was also important. The specific process of isotopic self-shielding in the photolysis of carbon monoxide may have played a major role. A key test of this hypothesis will be provided by laboratory-based isotopic analysis of the solar wind sampled in the NASA Genesis mission. 

Oxides and mixed catalysts Manufacturing of cement, concrete Refractory ceramics, a brick Faience and porcelain Safe life of medicines Terms and conditions of safe storage Recycling (processing) of products Formation and evolution of breeds (karsts) Evolution of the Solar System and the Universe Development of technologies for the production of materials for optoelectronics (GaN)... 

One of the scientific benefits we have already derived from the study of Antarctic meteorites is that a significant number of the specimens that have been collected there are nngronped, which means that they do not fit into the arbitrary classification scheme that has been devised (Table 18.1). The nngrouped meteorite specimens expand the classification and provide new and additional insight into the origin and evolution of the solar system. 

Most chemical elements known at present have been discovered in nature (in various ores and minerals, the earth s atmosphere, etc.) and one can say with confidence that there are no more undiscovered elements in nature, including both stable elements and those referred to as naturally radioactive ones. They can be called elements discovered by means of analysis . They exist independently of man, his knowledge, and methods of investigation. They existed at the earliest stages of evolution of the solar system when the Earth was being formed as a planet. 

MS provides a powerful capability for in situ exploration of planetary environments. MS can be used to identify the abundances of atomic and molecular species, determine isotopic ratios, and thereby answer many of the fundamental questions regarding the creation and evolutions of the solar system. Here we discuss briefly some of the results from mass spectroscopic instruments on previous and on-going space missions as listed chronologically in Table 17.1. 

The question of the origin and evolution of the solar system is one of the most fundamental in astronomy. It bears directly on such related issues as stellar evolution, the formation of planetary systems, and on the existence of life itself. Gamma-ray observations from spacecraft, either via remote sensing from orbit or through in situ measurements... 

Edgeworth, K. E. (1949). The origin and evolution of the solar system. Monthly Notices of the Royal Astronomical Society, 109,600-9. 

Collisions between comets and planets have occurred often during the evolution of the solar system. Cometary impacts on early Earth may have deposited a substantial amount of water to the Earth. The masses of lost and retained water after the impacts of comets and asteroids on oceans of various depths were studied by Svetsov, 2009 [330], The bombardment of an atmosphereless planet by fast asteroids can wipe out the most part of an ocean. Because of their mass loss during perihelion passage, it is difficult to predict cometary orbits with high precision. Therefore an impact of a comet on a planet cannot be predicted precisely. 

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