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A new formula for the rotation velocity – and density distribution of a
A new formula for the rotation velocity – and density distribution of a

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Fine structure constant and square root of Planck momentum
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Sample Midterm 1 - inst.eecs.berkeley.edu
Sample Midterm 1 - inst.eecs.berkeley.edu

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Overview and historical perspective on Cosmology
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PHYSICS 1-3 - All Science Leads To God
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The Velocity of Light - Gravitational Relativity
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... be possible according to the second postulate of Albert Einstein’s 1905 theory of special relativity, the constant speed of light (186,000 miles per second), since matter cannot travel faster than the speed of light. Einstein’s enshrined speed of light also poses a serious problem for young universe ...
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... The most reasonable conclusion then is that the Universe at early times T>38MeV possessed an asymmetry between baryons and antibaryons which prevented the annihilation catastrophe. At high temperatures T>1GeV, thermal quark-antiquark pairs were present in great numbers, nq ~ nq ~ ng , so that the b ...
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Flatness problem



The flatness problem (also known as the oldness problem) is a cosmological fine-tuning problem within the Big Bang model of the universe. Such problems arise from the observation that some of the initial conditions of the universe appear to be fine-tuned to very 'special' values, and that a small deviation from these values would have had massive effects on the nature of the universe at the current time.In the case of the flatness problem, the parameter which appears fine-tuned is the density of matter and energy in the universe. This value affects the curvature of space-time, with a very specific critical value being required for a flat universe. The current density of the universe is observed to be very close to this critical value. Since the total density departs rapidly from the critical value over cosmic time, the early universe must have had a density even closer to the critical density, departing from it by one part in 1062 or less. This leads cosmologists to question how the initial density came to be so closely fine-tuned to this 'special' value.The problem was first mentioned by Robert Dicke in 1969. The most commonly accepted solution among cosmologists is cosmic inflation, the idea that the universe went through a brief period of extremely rapid expansion in the first fraction of a second after the Big Bang; along with the monopole problem and the horizon problem, the flatness problem is one of the three primary motivations for inflationary theory.
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