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Large Scale Structure and Supersymmetric Inflation without Fine Tuning
Authors
A. Dekel
A. Nusser
+28Β more
A.D. Linde
A.D. Linde
A.D. Linde
A.R. Liddle
A.R. Liddle
C.L. Bennett
D. Yu. Pogosyan
D.H. Lyth
E. Witten
E.J. Copeland
E.L. Wright
E.W. Kolb
G. Dvali
H. Feldman
M.G. Haehnelt
M.G. Haehnelt
M.S. Smith
Q. Shafi
Q. Shafi
R. Schaefer
R. Schaefer
R.K. Schaefer
S. Coleman
S. Mollerach
S.D.M. White
T.P. Walker
W.H. Press
Y. Avni
Publication date
1 January 1994
Publisher
'American Physical Society (APS)'
Doi
Cite
View
on
arXiv
Abstract
We explore constraints on the spectral index
n
n
n
of density fluctuations and the neutrino energy density fraction
Ξ©
H
D
M
\Omega_{HDM}
Ξ©
HD
M
β
, employing data from a variety of large scale observations. The best fits occur for
n
β
1
n\approx 1
n
β
1
and
Ξ©
H
D
M
β
0.15
β
0.30
\Omega_{HDM} \approx 0.15 - 0.30
Ξ©
HD
M
β
β
0.15
β
0.30
, over a range of Hubble constants
40
β
60
40-60
40
β
60
km s
β
1
^{-1}
β
1
Mpc
β
1
^{-1}
β
1
. We present a new class of inflationary models based on realistic supersymmetric grand unified theories which do not have the usual `fine tuning' problems. The amplitude of primordial density fluctuations, in particular, is found to be proportional to
(
M
X
/
M
P
)
2
(M_X /M_P)^2
(
M
X
β
/
M
P
β
)
2
, where
M
X
(
M
P
)
M_X (M_P)
M
X
β
(
M
P
β
)
denote the GUT (Planck) scale, which is reminiscent of cosmic strings! The spectral index
n
=
0.98
n = 0.98
n
=
0.98
, in excellent agreement with the observations provided the dark matter is a mixture of `cold' and `hot' components.Comment: LaTEX, 14 pp. + 1 postscript figure appende
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Last time updated on 26/03/2019