Titlebook: Cosmology for the Curious; Delia Perlov,Alex Vilenkin Book 2024Latest edition The Editor(s) (if applicable) and The Author(s), under exclu

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Hubble’s Law and the Expanding Universeeriously had spectral lines that were red-shifted, indicating that they were moving away from the Earth, some at speeds of up to 1000?km/s. Motion at high speed is not uncommon in the cosmos—the Sun, for example, orbits around the center of our Galaxy at 240 km/s.

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The Quantum Worlde, was single handedly accomplished by Einstein with his special and general theories of relativity. The development ofby a number of physicists ushered in the second revolution, which shook the foundations of physics even more than the first. Quantum mechanics was developed as a theory of the micro

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The Hot Big Bangnd that the universe was denser in its past than it is today. In fact, the density of the universe grows without bound as we wind the clock back to the big bang. Furthermore, the temperature of the universe also soars to extremely high values. How do we know this? And what does this imply about the

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Structure Formations are grouped in clusters, which are in turn grouped into still larger structures, called superclusters. The formation of cosmic structures is an active area of research, and we now believe we have a good idea of how they emerged.

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The Very Early Universebang, the fireball gets hotter and denser, and other types of particles emerge. They move at nearly the speed of light, colliding frequently and violently. As we shall see, some of the most dramatic events in the history of the universe occurred within a small fraction of a second after the big bang

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A Test Bed for the Numerical Tool, using the language of modern physics and abstract mathematics. Yet, at its core, our cosmological knowledge is the answer to a few fundamental questions. Have you ever drifted off deep into thought, wondering: Is the universe finite or infinite? Has it existed forever? If not, when and how did it

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Shuzhuo Li,Quanbao Jiang,Marcus W. Feldmanatible with Newton’s law of gravitation. Newton himself, and some ten generations of physicists and astronomers that followed, used this law to describe the motion of planets with remarkable accuracy. Granted, there was a tiny discrepancy in the calculated precession rate of the orbit of Mercury, bu

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https://doi.org/10.1007/978-94-017-8987-5niverse beyond our Milky Way galaxy was then completely unknown, so Einstein had to make some assumptions. Following Newton, he assumed that on average matter is uniformly distributed in the cosmos. There are of course local variations, with the density of stars higher in some places and lower in ot