Large Scale Structure and Supersymmetric Inflation without Fine Tuning

Details Large Scale Structure and Supersymmetric Inflation without Fine Tuning Large Scale Structure and Supersymmetric Inflation without Fine Tuning

1994-06-15

arxiv.org/abs/hep-ph/9406319v1

Phys.Rev.Lett.73:1886-1889,1994

Physics

High Energy Physics

High Energy Physics - Phenomenology

LaTEX, 14 pp. + 1 postscript figure appended

Scientific paper

10.1103/PhysRevLett.73.1886

We explore constraints on the spectral index $n$ of density fluctuations and the neutrino energy density fraction $\Omega_{HDM}$, employing data from a variety of large scale observations. The best fits occur for $n\approx 1$ and $\Omega_{HDM} \approx 0.15 - 0.30$, over a range of Hubble constants $40-60$ km s$^{-1}$ Mpc$^{-1}$. 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 $(M_X /M_P)^2$, where $M_X (M_P)$ denote the GUT (Planck) scale, which is reminiscent of cosmic strings! The spectral index $n = 0.98$, in excellent agreement with the observations provided the dark matter is a mixture of `cold' and `hot' components.

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