By Robert C. Yates

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**Extra info for Curves and Their Properties **

**Sample text**

Note that at the end of the 1970s and the beginning of the 1980s, it seemed that the value of ML grows as the mass of the object increases. , 1996), the curve reaches a ‘plateau’. 15 (Fukugita, 2000). It is typically dm (M/10 M ) 150–400. assumed that the distribution of ‘dark matter’ inside rv is isothermal. Then, ML Note that this value is practically the same as the value one finds for groups and clusters of galaxies (Fukugita, 2000). Using the relationships presented above, we can evaluate the parameter dm in the framework of the method outlined above.

10 (a) and (b), the predictions of the theory with regard to current concentrations of He4 , and especially deuterium, are very sensitive to the current density of baryons, provided the temperature and concentration of CMB quanta are known. 9 Dynamics of synthesis of light chemical elements in the hot Universe. Adapted from Taytler et al. (2000). 10 The mass element abundances from the Big Bang nucleosynthesis as a function of η. (a) For He4 , He2 , Li7 ; (b) for Be9 , B10 and B11 . Solid lines for Be9 and B10 correspond to uncertainties in the theoretical predictions.

1998). Hui et al. 045. In this case, we speak about uncertainty characterized by a factor of 2, even though it could be possible that all subsequent improvements of the models would lead to a significantly reduced estimate. 3 for the expected values of density of the baryonic fraction of matter based on the above-listed observational tests and on their theoretical interpretation. 02 in order to estimate the total density of the baryonic fraction, it 2 bh cm−3 . 3 Baryonic component of matter in the Universe comparison, the concentration of CMB quanta is 412 cm−3 , and therefore nb ξ10 = 1010 = 274 b h 2 .