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Dark Matter Dark Energy The History of the Universe More of the
Dark Matter Dark Energy The History of the Universe More of the

... luminosity of the supernovae which are used to get distances. All Type Ia Supernovae definitely come from white dwarfs but it is not known whether all involve accretion from a nearby star, merging with another white dwarf, or either/or! ...
100 $100 $100 $100 $100 $100 $200 $200 $200 $200 $200 $200
100 $100 $100 $100 $100 $100 $200 $200 $200 $200 $200 $200

... luminosity of the supernovae which are used to get distances. All Type Ia Supernovae definitely come from white dwarfs but it is not known whether all involve accretion from a nearby star, merging with another white dwarf, or either/or! ...
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The New Cosmology: Our Expanding Universe
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The New Cosmology: Our Expanding Universe
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Star Groups and Big Bang Power Point
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Unit 3 - Section 9.7 Stellar Spectra, Dark Matter0
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STATE UNIVERSITY OF NEW YORK COLLEGE OF TECHNOLOGY CANTON, NEW YORK
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... 7. Hubble’s discovery that there was red shift in the spectra of galaxies led to an understanding that the universe is expanding. 8. Astronomers believe that cosmic background radiation formed shortly after the big bang. 9. The event which began the universe was the big bang. 10. The two elements th ...
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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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