-
4
-
-
33845744597
-
-
See http://map.gsfc.nasa.gov/
-
-
-
-
5
-
-
33845803433
-
-
note
-
In special cases, such as that studied in Ref. [6], two or more scalar fields might be involved. As an alternative to the inflation hypothesis, a "pre-big-bang" [7-9] or "ekpyrotic" [10-12] era of collapse has been proposed, but there is so far no accepted theory of a bounce and therefore no firm prediction from collapsing cosmologies. In particular, there is so far no accepted string-theoretic description of a bounce [13].
-
-
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6
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2342438930
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K. Dimopoulos, G. Lazarides, D. Lyth, and R. Ruiz de Austri, J. High Energy Phys. 05, 057 (2003).
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J. High Energy Phys.
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, pp. 057
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Dimopoulos, K.1
Lazarides, G.2
Lyth, D.3
Ruiz De Austri, R.4
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7
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33845741846
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G. Veneziano, hep-th/0002094
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G. Veneziano, hep-th/0002094.
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8
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0000037508
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R. Brustein, M. Gasperini, M. Giovannini, V.F. Mukhanov, and G. Veneziano, Phys. Rev. D 51, 6744 (1995).
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(1995)
Phys. Rev. D
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Brustein, R.1
Gasperini, M.2
Giovannini, M.3
Mukhanov, V.F.4
Veneziano, G.5
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10
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85038278781
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J. Khoury, B.A. Ovrut, P.J. Steinhardt, and N. Turok, Phys. Rev. D 64, 123522 (2001);
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(2001)
Phys. Rev. D
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, pp. 123522
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Khoury, J.1
Ovrut, B.A.2
Steinhardt, P.J.3
Turok, N.4
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12
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0037104498
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J. Khoury, B.A. Ovrut, P.J. Steinhardt, and N. Turok, Phys. Rev. D 66, 046005 (2002);
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(2002)
Phys. Rev. D
, vol.66
, pp. 046005
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Khoury, J.1
Ovrut, B.A.2
Steinhardt, P.J.3
Turok, N.4
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15
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33845792251
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H. Liu, G. Moore, and N. Seiberg, gr-qc/0301001
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H. Liu, G. Moore, and N. Seiberg, gr-qc/0301001.
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16
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4744339397
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P. Crotty, J. García-Bellido, J. Lesgourgues, and A. Riazuelo, Phys. Rev. Lett. 91, 171301 (2003).
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Phys. Rev. Lett.
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, pp. 171301
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Crotty, P.1
García-Bellido, J.2
Lesgourgues, J.3
Riazuelo, A.4
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18
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0043077843
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hep-ph/0204294; hep-ph/9904502
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G. Lazarides, Lect. Notes Phys. 592, 351 (2002); hep-ph/0204294; hep-ph/9904502.
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(2002)
Lect. Notes Phys.
, vol.592
, pp. 351
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Lazarides, G.1
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22
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33845776859
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K. Dimopoulos and D.H. Lyth, hep-ph/0209180
-
K. Dimopoulos and D.H. Lyth, hep-ph/0209180.
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29
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33845725842
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R. Hofmann, hep-ph/0208267
-
R. Hofmann, hep-ph/0208267.
-
-
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38
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33845777312
-
-
(to be published), astro-ph/0212264
-
K. Dimopoulos, Phys. Rev. D (to be published), astro-ph/0212264.
-
Phys. Rev. D
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Dimopoulos, K.1
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40
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33845736679
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A.R. Liddle and L.A. Urena-López, astro-ph/0302054
-
A.R. Liddle and L.A. Urena-López, astro-ph/0302054.
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42
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85038980644
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K. Enqvist, A. Jokinen, S. Kasuya, and A. Mazumdar, Phys. Rev. D 68, 103507 (2003).
-
(2003)
Phys. Rev. D
, vol.68
, pp. 103507
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Enqvist, K.1
Jokinen, A.2
Kasuya, S.3
Mazumdar, A.4
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43
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23144438732
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K. Dimopoulos, D.H. Lyth, A. Notari, and A. Riotto, J. High Energy Phys. 07, 053 (2003).
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(2003)
J. High Energy Phys.
, vol.7
, pp. 053
-
-
Dimopoulos, K.1
Lyth, D.H.2
Notari, A.3
Riotto, A.4
-
45
-
-
33845808063
-
-
M. Postma and A. Mazumdar, hep-ph/0304246
-
M. Postma and A. Mazumdar, hep-ph/0304246.
-
-
-
-
46
-
-
33845790846
-
-
S. Kasuya, M. Kawasaki, and F. Takahashi, hep-ph/0305134
-
S. Kasuya, M. Kawasaki, and F. Takahashi, hep-ph/0305134.
-
-
-
-
48
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-
33845778685
-
-
D.H. Lyth and D. Wands, astro-ph/0306500
-
D.H. Lyth and D. Wands, astro-ph/0306500.
-
-
-
-
49
-
-
33845739061
-
-
D. H. Lyth and K. Malik (in preparation)
-
D. H. Lyth and K. Malik (in preparation).
-
-
-
-
50
-
-
33845730138
-
-
note
-
Recently, a different alternative to the inflaton scenario has been proposed in Refs. [49-51], in which some "modulating" field perturbs the inflaton decay rate without ever contributing significantly to the energy density. The properties of the modulating field have to be much more special than those of the curvaton field.
-
-
-
-
51
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-
33845731987
-
-
G. Dvali, A. Gruzinov, and M. Zaldarriaga, astro-ph/0303591
-
G. Dvali, A. Gruzinov, and M. Zaldarriaga, astro-ph/0303591.
-
-
-
-
52
-
-
33845801859
-
-
L. Kofman, astro-ph/0303614
-
L. Kofman, astro-ph/0303614.
-
-
-
-
56
-
-
0000638026
-
-
Phys. Rev. Lett. 75, 398 (1995).
-
(1995)
Phys. Rev. Lett.
, vol.75
, pp. 398
-
-
-
58
-
-
33845794624
-
-
note
-
Note that, in view of Eq. (11), wσ may be in principle time dependent.
-
-
-
-
60
-
-
33845751781
-
-
We ignore cubic A-terms
-
We ignore cubic A-terms.
-
-
-
-
61
-
-
33845744596
-
-
note
-
Here, g may also include loop factors or number of degrees of freedom, etc.
-
-
-
-
62
-
-
85107713965
-
-
note
-
2.
-
-
-
-
63
-
-
85107714003
-
-
note
-
0.
-
-
-
-
64
-
-
85107713097
-
-
note
-
0)], which means that the rapid roll due to the kinetic energy ceases in less than a Hubble time.
-
-
-
-
67
-
-
85107715413
-
-
note
-
-1.
-
-
-
-
68
-
-
33845787733
-
-
note
-
kin of the rolling scalar field. If one adopted such a view then there would be no quantum regime on top of local maxima (e.g. in the case of eternal inflation) or at inflection points, where V = 0, as long as V is large enough. Moreover, the fact that one can always add a cosmological constant would have really caused confusion since a change of V would have affected the location of the borders of the quantum regime.
-
-
-
-
69
-
-
85107713033
-
-
note
-
σ both in the oscillating case and in the case of the scaling solution.
-
-
-
-
70
-
-
85107714165
-
-
note
-
-1, at the end of inflation the field may find itself in the quasi-quadratic regime instead.
-
-
-
-
72
-
-
85107714094
-
-
note
-
2, during this time interval, which would lead to substantial roll that reduces the perturbation.
-
-
-
-
73
-
-
85107714867
-
-
note
-
end and so, for the amplitude of the oscillating field, Eq. (71) is valid.
-
-
-
-
74
-
-
85107711944
-
-
note
-
0o →m
-
-
-
-
76
-
-
85107712121
-
-
note
-
reh may be substantially relaxed by the extra entropy production if the curvaton decays after it dominates the Universe.
-
-
-
|