Cosmic gases

Yoneda, S. and Grossman, L. (1995) Condensation of Ca0-Mg0-Al203-Si02 liquids from cosmic gases. Geochimica et Cosmochimica Acta, 59, 3413-3444. 

Larimer J. W. and Bartholomay M. (1979) The role of carbon and oxygen in cosmic gases some applications to the chemistry and mineralogy of enstatite chondrites. Geochim. Cosmochim. Acta 43, 1455-1466. 

Dissipation of cosmic gases from the Earth s atmosphere... 

After the dissipation of cosmic gases (approximately 4 x 109 years ago) several gaseous materials were liberated from the solid Earth. The substances formed in this way are termed secondary constituents. These atmospheric components were due either to volcanic, desorption and thermal processes or to chemical reactions. 

Bob pushes the thoughts out of his mind and enjoys the grass. For centuries, scientists hypothesized that the Sun and planets were born from a rotating disk of cosmic gas and dust. The flat disk constrained the nascent planets to have orbits lying roughly in the same plane. This nebular theory was proposed as far back as 1755 by the philosopher Immanuel Kant. 

There is a very low cosmic abundance of boron, but its occurrence at all is surprising for two reasons. First, boron s isotopes are not involved in a star s normal chain of thermonuclear reactions, and second, boron should not survive a star s extreme thermal condition. The formation of boron has been proposed to arise predominantly from cosmic ray bombardment of interstellar gas in a process called spallation (1). 

Colorless, reactive gas. Oxygen was not present in the initial atmosphere of the Earth, although at 50 % it is the most common element in the crust of the Earth (oxides, silicates, carbonates, etc.). The compound with hydrogen is remarkable. The hydrides of all other elements are unpleasant compounds, but H20 is the molecule of life. The 02 found in the air today, of which it makes up 20 %, was formed in the process of evolution by photosynthesis of algae, which then also allowed life on solid land. Oxidation with oxygen became and is still the dominant pathway of life forms for obtaining energy (respiration). Used in medicine in critical situations. Oxidations play a key role in chemistry (sulfuric acid, nitric acid, acetic acid, ethylene oxide, etc.). The ozone layer in space protects the Earth from cosmic UV radiation. Ozone (03) is used in the... 

Once a significant amount of molecular hydrogen is produced, a rich gas-phase chemistry ensues.24 Ion-molecule processes are initiated in the interiors of dense clouds mainly via cosmic ray ionization, the most important reaction being,... 

Radiation chemical processes involving cosmic and UV irradiation The extremely low density of material in interstellar space (ISM gas and ISM nuclei), which could affect the cometary material in the course of millions of years... 

The ionization of nitrogen, oxygen and trace gas molecules in the air due to the presence of the natural radioelements in the soil and air and the cosmic radiation has a direct effect upon the electrical characteristics of the atmosphere. 

The primordial Li abundance was sought primarily because of its ability to constrain the baryon to photon ratio in the Universe, or equivalently the baryon contribution to the critical density. In this way, Li was able to complement estimates from 4He, the primordial abundance of which varied only slightly with baryon density. Li also made up for the fact that the other primordial isotopes, 2H (i.e. D) and 3He, were at that time difficult to observe and/or interpret. During the late 1990 s, however, measurements of D in damped Lyman alpha systems (high column-density gas believed to be related to galaxy discs) provided more reliable constraints on the baryon density than Li could do (e.g. [19]). Even more recently, the baryon density has been inferred from the angular power spectrum of the cosmic microwave background radiation, for example from the WMAP measurements [26]. We consider the role of Li plateau observations post WMAP. 

The state of matter within these regions needs to be determined before the balance of energy and chemistry can be understood. Extreme photon fluxes break all chemical bonds, prevent molecule formation and ionise atoms but as the density of species increases the UV and far-UV photons are absorbed and molecules begin to form. Chemical reactions are, however, slow in the gas phase due to the low temperature, and molecules condense out on the surface of dust particles, perhaps forming ice grains. Once on the surface, molecules continue to be photoprocessed by the starlight as well as by the continual bombardment of cosmic rays. 

Table 1. Cosmic Ray Produced Noble Gas Radioisotopes Tl/2 > 1 month.

Keywords fluxon gas in thermalized Josefson systems the criteria of degeneracy of the relativistic ideal gas absolute minimum realization of the most probable state in the equilibrium system temperature of the primary microwave cosmic background primary quantum magnetic flow. 

The human body is equipped to deal with nominal levels of radiation doses. Background (natural) radiation from radon gas, cosmic sources, soil, and water produces an average dose of about 0.3 rem (0.003 Sv) per year.4 However, large doses of radiation generated after a terrorist attack can overwhelm the body s ability to repair damage, leading to stochastic or acute health effects. 

Cosmic rays Protons and a particles that enter Earth s atmosphere from outer space. When they collide with atoms or molecules of atmospheric gas, high-energy neutrons can be given off These neutrons can then undergo nuclear reactions with other atmospheric gas atoms and molecules. 

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