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research
Cosmological Density Perturbations From A Quantum Gravitational Model Of Inflation
Authors
L. R. Abramo
N. C. Tsamis
R. P. Woodard
Publication date
25 April 1996
Publisher
'Wiley'
Doi
View
on
arXiv
Abstract
We derive the implications for anisotropies in the cosmic microwave background following from a model of inflation in which a bare cosmological constant is gradually screened by an infrared process in quantum gravity. The model predicts that the amplitude of scalar perturbations is
A
S
=
(
2.0
Β±
.
2
)
Γ
1
0
β
5
A_S = (2.0 \pm .2) \times 10^{-5}
A
S
β
=
(
2.0
Β±
.2
)
Γ
1
0
β
5
, that the tensor-to-scalar ratio is
r
β
1.7
Γ
1
0
β
3
r \approx 1.7 \times 10^{-3}
r
β
1.7
Γ
1
0
β
3
, and that the scalar and tensor spectral indices are
n
β
.
97
n \approx .97
n
β
.97
and
n
T
β
β
2.8
Γ
1
0
β
4
n_T \approx -2.8 \times 10^{-4}
n
T
β
β
β
2.8
Γ
1
0
β
4
, respectively. By comparing the model's power spectrum with the COBE 4-year RMS quadrupole, the mass scale of inflation is determined to be
M
=
(
.
72
Β±
.
03
)
Γ
1
0
16
Β
G
e
V
M = (.72 \pm .03) \times 10^{16}~{\rm GeV}
M
=
(
.72
Β±
.03
)
Γ
1
0
16
Β
GeV
. At this scale the model produces about
1
0
8
10^8
1
0
8
e-foldings of inflation, so another prediction is
Ξ©
=
1
\Omega = 1
Ξ©
=
1
.Comment: 18 pages, LaTeX 2 epsilon, 1 eps file, uses epsfi
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Last time updated on 24/08/2020