Calculate the temperature of the universe when photons can no longer disassociate deuterons. Use the mean value of the distribution.
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Calculate the temperature of the universe when photons can no longer disassociate deuterons. Use the mean value of the distribution.
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- 1. Assuming a spatially flat Universe, find the time dependence of: (a) the density of matter when the Universe is radiation dominated and (b) the density of radiation when the Universe is matter dominated.For each of the hadrons below, fill in the table to show that the charge, baryon number, and strangeness of these particles equal the respective sums of these numbers for their quark constituents. (Enter your charges as a multiple of e.) (a) A**, quark composition: uuu total strangeness baryon number charge (b) A", quark composition: ddd total strangeness baryon number charge (c) K* meson, quark composition: us total strangeness baryon number charge (d) K- meson, quark composition: su total strangeness baryon number charge 00Explain the process of electron-holes recombination.
- Give examples of nonbaryonic matter.At what temperature is the thermal radiation in the universe energetic enough to produce nucleons and antinucleons?With the aid of a diagram, explain the physical origin of cosmological redshift in an expanding universe, and how this differs from the Doppler shift due to relative motion. Observations of distantgalaxies indicate that their recession velocities, v, and their distances, d, follow a Hubble Law:v = H0d, where H0 is a constant. Using the analogy of an expanding grid or ruler, demonstratethat Hubble’s Law indicates that the Universe is undergoing uniform expansion.
- Estimate the critical density of the universe if the Hubble's constant was 100 km/s/Mpc.In Chapter 7 we discussed the need for the addition of the cosmological constant A to the Einstein Field Equations and further to our derived equations. iii. Starting with the fluid equation, show that the pressure exerted due to the cosmological constant is PA = -Pac? (Recall that we define an energy density due to the cosmological constant as the following scaled parameter PA = THIS IS A COSMOLOGY QUESTION!!!!!!!!