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Linde, A.D.1
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A similar argument for the coincidence of the galaxy formation time (Formula presented) with the curvature domination time (Formula presented) in models of open inflation was given in Ref
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A similar argument for the coincidence of the galaxy formation time (Formula presented) with the curvature domination time (Formula presented) in models of open inflation was given in Ref. 9.
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34
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85037184915
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fact, for a Salpeter initial mass function
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In fact, for a Salpeter initial mass function 25 and under simple assumptions, the highest probability for the time to evolve an intelligent civilization, (Formula presented) lies in the neighborhood of the Sun’s lifetime 23.
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37
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85037183274
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It is conceivable that new civilizations may form long after most of the carbon has been created. However, with our definition of (Formula presented) as the time when lambda is first measured by a civilization, it is unclear whether such late bloomers would play a role. The early civilizations are likely to colonize the galaxy, and the late civilizations may be better described as late stages of earlier ones
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It is conceivable that new civilizations may form long after most of the carbon has been created. However, with our definition of (Formula presented) as the time when lambda is first measured by a civilization, it is unclear whether such late bloomers would play a role. The early civilizations are likely to colonize the galaxy, and the late civilizations may be better described as late stages of earlier ones.
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Actually, the fraction of baryonic matter (Formula presented) is also relevant for cooling. Following
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Actually, the fraction of baryonic matter (Formula presented) is also relevant for cooling. Following 10 we shall take (Formula presented)
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47
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85037220119
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This upper bound on t is determined by line cooling in helium. For (Formula presented) there is also a narrow interval near (Formula presented) where cooling is again efficient due to hydrogen line cooling. However, the interval is very narrow and we shall disregard the galaxies which may form during this short late period
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This upper bound on t is determined by line cooling in helium. For (Formula presented) there is also a narrow interval near (Formula presented) where cooling is again efficient due to hydrogen line cooling. However, the interval is very narrow and we shall disregard the galaxies which may form during this short late period.
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There exist some indications that the IMF may depend on density. For example, it has been suggested that the IMF is biased towards high masses in very active regions like starbursts
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There exist some indications that the IMF may depend on density. For example, it has been suggested that the IMF is biased towards high masses in very active regions like starbursts 41, and towards low masses in regions of extreme inactivity, like the field population 42. These suggestions are not very certain because the observations are influenced by selection effects and by evolution.
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