Summary
In the actionS=(c 4/16πG 0)∫(R+2ϰε)√−g d4 x the «constant» χ is assumed to be the function of the matter energy density: χ=χ(ɛ). In this case the variation ofS with respect to the metricg ik automatically leads to Einstein equations with a Λ-like term. The conditions under which the initial state of the Universe turns out to be a De Sitter one are considered.
Riassunto
Nell’azioneS=(c 4/16πG 0)∫(R+2ϰε)√−g d4ϰ si assume che la costante ϰ è funzione della densità di energia della materia: ϰ=ϰ(ɛ). In questo caso, la variazione diS rispetto alla metricag ik porta automaticamente alle equazioni di Einstein con un termine tipo Λ. Si considerano le condizioni in cui lo stato iniziale dell’Universo risulta essere uno stato di De Sitter.
Резюме
В действииS=(c 4/16πG 0)∫(R+2ϰε)√−g d4ϰ предполагается, что «константа» ϰ является функцией плотности энергии вещества: ϰ=ϰ(ɛ). В этом случае вариацияS относительно метрикиg ik автоматически приводит к уравнениям Эйнштейна с Λ-подобным членом. Рассматриваются условия, при которых начальное состояние Вселенной оказывается Вселенной де Ситтера.
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Markov, M.A., Mukhanov, V.F. De Sitter-like initial state of the Universe as a result of asymptotical disappearance of gravitational interactions of matter. Nuov Cim B 86, 97–102 (1985). https://doi.org/10.1007/BF02732276
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DOI: https://doi.org/10.1007/BF02732276