Quintessential inflation from a variable cosmological constant in a 5 D vacuum
نویسنده
چکیده
We explore an effective 4D cosmological model for the universe where the variable cosmological constant governs its evolution and the pressure remains negative along all the expansion. This model is introduced from a 5D vacuum state where the (space-like) extra coordinate is considered as noncompact. The expansion is produced by the inflaton field, which is considered as non-minimally coupled to gravity. We conclude from experimental data that the coupling of the inflaton with gravity should be weak, but variable in different epochs of the evolution of the universe.
منابع مشابه
- qc / 0 60 61 19 v 1 2 8 Ju n 20 06 Quintessential inflation from a variable cosmological constant in a 5 D vacuum
We explore an effective 4D cosmological model for the universe where the variable cosmological constant governs its evolution and the pressure remains negative along all the expansion. This model is introduced from a 5D vacuum state where the (space-like) extra coordinate is considered as noncompact. The expansion is produced by the inflaton field, which is considered as non-minimally coupled t...
متن کاملar X iv : h ep - p h / 98 11 37 5 v 1 1 7 N ov 1 99 8 LBNL – 42536 LANCS – TH / 9821 hep - ph / 9811375 November 1998 Quintessential difficulties
An alternative to a cosmological constant is quintessence, defined as a slowlyvarying scalar field potential V (φ). If quintessence is observationally significant, an epoch of inflation is beginning at the present epoch, with φ the slowly-rolling inflaton field. In contrast with ordinary inflation, quintessence seems to require extreme fine tuning of the potential V (φ). The degree of fine-tuni...
متن کاملSelf-tuning of Cosmological Constant and Exit from Inflation *
I review the recent 5D self-tuning solutions of the cosmological constant problem, and try to unify two cosmological constant problems within the framework of the self-tuning solutions. One problem, the large cosmological constant needed for inflation, is interpreted by starting with the parameters allowing only the dS vacuum, and the vanishing cosmological constant at a true vacuum is realized...
متن کاملar X iv : h ep - p h / 98 11 37 5 v 2 5 D ec 1 99 8 LBNL – 42536 LANCS – TH / 9821 hep - ph / 9811375 November 1998 Quintessential difficulties
An alternative to a cosmological constant is quintessence, defined as a slowlyvarying scalar field potential V (φ). If quintessence is observationally significant, an epoch of inflation is beginning at the present epoch, with φ the slowly-rolling inflaton field. In contrast with ordinary inflation, quintessence seems to require extreme fine tuning of the potential V (φ). The degree of fine-tuni...
متن کاملar X iv : h ep - p h / 98 11 37 5 v 3 2 5 M ay 1 99 9 LBNL – 42536 LANCS – TH / 9821 hep - ph / 9811375 November 1998 Quintessential difficulties
An alternative to a cosmological constant is quintessence, defined as a slowlyvarying scalar field potential V (φ). If quintessence is observationally significant, an epoch of inflation is beginning at the present epoch, with φ the slowly-rolling inflaton field. In contrast with ordinary inflation, quintessence seems to require extreme fine tuning of the potential V (φ). The degree of fine-tuni...
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