Cosmic couple

Once the cosmic abundance ratios are chosen, one can solve the coupled kinetic equations in a variety of approximations to determine the concentrations of the species in the model as functions of the total gas density. Division of the concentrations by the total gas density utilized in the calculation then yields the relative concentrations or abundances. The simplest approximation is the steady-state treatment, in which the time derivatives of all the concentrations are set equal to zero. In this approximation, the coupled differential equations become coupled algebraic equations and are much easier to solve. This was the approach used by Herbst and Klemperer (1973) and by later investigators such as Mitchell, Ginsburg, and Kuntz (1978). In more recent years, however, improvements in computers and computational methods have permitted modelers to solve the differential equations directly as a function of initial abundances (e.g. atoms). Prasad and Huntress (1980 a, b) pioneered this approach and demonstrated that it takes perhaps 107 yrs for a cloud to reach steady state assuming that the physical conditions of a cloud remain constant. Once steady state is reached, the results for specific molecules are not different from those calculated earlier via the steady-state approximation if the same reaction set is utilized. Both of these approaches typically although not invariably yield calculated abundances at steady-state in order-of-magnitude agreement with observation for the smaller interstellar molecules. 

It is possible for instance to test the mode couplings as the gravitational instabilities develop. The amount of non-Gaussianities embedded in cosmic shear surveys then betrays the details of the gravitational instability scenario, allowing for instance the possibility of measuring the mass density of the universe in a totally independent way. That would contribute in the consolidation of the current concordance model of cosmology. 

At the transition to the next section, we find (1) naturally soft bosons that could also be responsible for cosmic acceleration (ApOO), and (2) a unified "dark sector" in which the energy density of a scalar field acts like a cosmological constant and the value of the field sets the DM particle masses via Yukawa coupling (77). Current data can be fit, but some of the predictions are different from those of standard CDM, including the long... 

It has been known for decades that there is coupling between elements of the global circuit and magnetospheric and solar phenomena. The modulation of galactic cosmic... 

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