Заключение
Долгосрочное расширение Вселенной зависит от множества факторов, включая вклад, который вносит в общую плотность энергии вакуум (Weinberg, 1989; Carroll, Press and Turner, 1992), массовую плотность Вселенной (недавний обзор см. в работе Turkok, 1997; см. также Loh and Spillar, 1986) и многие другие соображения (например, Ellis and Rothman, 1993; Gott, 1993; Grischuk and Zel'dovich, 1978).
Хотя современные данные астрономических наблюдений свидетельствуют о том, что Вселенная продолжит расширяться (Dekel et al., 1997), мы вкратце рассматриваем сценарий, согласно которому Вселенная, или некоторая ее часть, переживет повторное сжатие. Классическое изложение физических событий, ведущих к Большому сжатию, см. в статье Риса (Rees, 1969).
Тонкая настройка нашей Вселенной обсуждается во многих контекстах и связана с «антропным космологическим принципом» (более подробное изложение см. в трудах Barrow and Tipler, 1986; Carr and Rees, 1979). Идея о том, что наша Вселенная — всего лишь одна из множества возможных, в настоящее время вызывает все более пристальное внимание космологии (например, Rees, 1981); последняя популярная трактовка мультиверса и его следствий представлена в книге Риса (Rees, 1997).
На идее вечной инфляции и вечной сложности часто останавливался А.Линде (см., например, Linde, 1986, 1988, 1989, 1990, 1994; см. также Vilenkin, 1983). Понятие дарвиновской эволюции вселенных ввел и описал в своей последней книге Л. Смолин (Smolin, 1997; см. также Rees, 1997).
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