Cosmology

Download A Universe from Nothing: Why There is Something Rather than by Lawrence M. Krauss PDF

By Lawrence M. Krauss

Author note: Afterword through Richard Dawkins
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Bestselling writer and acclaimed physicist Lawrence Krauss bargains a paradigm-shifting view of ways every thing that exists got here to be within the first place.

"Where did the universe come from? What used to be there prior to it? what's going to the long run deliver? and eventually, why is there anything instead of nothing?"

One of the few in demand scientists this present day to have crossed the chasm among technology and pop culture, Krauss describes the staggeringly appealing experimental observations and mind-bending new theories that display not just can whatever come up from not anything, anything will continually come up from not anything. With a brand new preface in regards to the importance of the invention of the Higgs particle, A Universe from not anything makes use of Krauss's attribute wry humor and fantastically transparent causes to take us again to the start of the start, proposing the latest facts for a way our universe evolved—and the consequences for the way it's going to end.

Provocative, not easy, and delightfully readable, this can be a game-changing examine the main simple underpinning of lifestyles and a strong antidote to superseded philosophical, non secular, and clinical considering.

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33) with a = 2π/N . The corresponding effective potential for the complex field ρ = σ + iα had a minimum at finite, moderately large values of the volume modulus field σ0 , which fixed the volume modulus in a state with a negative vacuum energy. Then an anti-D3 brane with the positive energy ∼ σ −2 was added. This addition uplifted the minimum of the potential to the state with a positive vacuum energy, see Fig. 6. Instead of adding an anti-D3 brane, which explicitly breaks supersymmetry, one can add a D7 brane with fluxes.

One can easily check that for λn , ξ m2 the higher with λn , ξ order terms can be ignored at the last stages of inflation, where φ = O(1). In other words, the theory behaves as purely quadratic during the last stages of inflation when the observable part of the universe was formed. One can come to the same conclusion if one takes into account only the part of inflation at smaller values of the field φ, when the stage of eternal inflation is over. This suggests that the simplest version of chaotic inflation scenario is the best.

23) √ where v = m/ λ is the amplitude of spontaneous symmetry breaking. If v is very large, v 102 , inflation occurs near the minimum of the potential, and all properties of inflation are the same as in the simplest chaotic inflation model with quadratic potential m2 φ2 . 28. If v takes some intermediate values, such as v = O(10), then two different inflationary regimes are possible in this model: at large φ and at small φ. e. 14). 14 to 10−2 , see Fig. 4 [68, 69]. If one considers chaotic inflation with the potential including terms φ2 , φ3 and φ4 , one can considerably alter the properties of inflationary perturbations [70].

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