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

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 the way every little 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 longer term carry? and at last, why is there anything instead of nothing?"

One of the few admired scientists this day to have crossed the chasm among technological know-how and pop culture, Krauss describes the staggeringly appealing experimental observations and mind-bending new theories that exhibit not just can anything come up from not anything, anything will regularly come up from not anything. With a brand new preface in regards to the value 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, featuring the latest proof for a way our universe evolved—and the results for a way it's going to end.

Provocative, not easy, and delightfully readable, this can be a game-changing examine the main simple underpinning of life and a strong antidote to outdated philosophical, spiritual, and clinical considering.

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Extra resources for A Universe from Nothing: Why There is Something Rather than Nothing

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When Einstein did this calculation, he said he was so excited it gave him palpitations of the heart. When his prediction of 43 seconds of arc per century matched the exact amount of unexplained rotation astronomers had already observed, he was overjoyed. Einstein then calculated how much light itself should bend as it passed near the limb of the Sun. 75 seconds of arc. 87 seconds of arc. The effect could be tested during a total eclipse of the Sun, when the Moon blocks the Sun’s bright surface, allowing background stars to be observed near it.

Galaxies would be like pennies taped to the surface of a balloon: as you blew up the balloon, it got bigger, and the distances between the pennies would increase. If you sat on a penny, all the other pennies would move away from you as the balloon expanded. The space between the galaxies would be expanding. A penny twice as far away would recede from you at twice the velocity. Start with the balloon at a certain size and consider one penny an inch away from your penny, a second penny 2 inches away, and a third penny 3 inches away.

Einstein convinced himself that the age argument might have a loophole—if stars were inhomogeneous in composition— and he became willing to adopt the simple Friedmann models without a cosmological constant. In an April 1931 report to the German Academy, he favored Friedmann’s original 1922 spherical Ω0 > 1, Big Bang– Big Crunch model. By January 1932, he had teamed up with de Sitter to champion an Ω0 = 1, flat Friedmann-type model that expands forever. By 1948 physicist George Gamow and his students, Herman and Alpher, were using an expanding Ω0 < 1 Friedmann model to predict that the early universe should be hot and filled with thermal radiation.

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