N-flation

By S. Dimopoulos, S. Kachru, John McGreevy, J. Wacker. 2005

551 citations recorded by the source corpus.

The presence of many axion fields in four-dimensional string vacua can lead to a simple, radiatively stable realization of chaotic inflation.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c0abec6e8101a568e94fc9547901c33e4e50c63a

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Citations in the corpus

Random matrices and the spectrum of N-flation (2005, methodology): “(The overall mass scale is not determined a priori; as in [1], we fix it by requiring the observed amplitude of density perturbations.”
Weak gravity strongly constrains large-field axion inflation (2015, methodology): “In section 3, we present arguments for how the magnetic form of the Weak Gravity Conjecture excludes the simplest models of N -flation [15] and models based on the Kim–Nilles– Peloso alignment mechanism [14] when it is realized through the structure of kinetic mixing [23].”
Phenomenology of a pseudo-scalar inflaton: naturally large nongaussianity (2011, methodology): “The idea of using a PNGB as inflaton was first put forward in [6]; in this minimal realization a single axion is present; it turns out that this model can produce a sufficiently flat spectrum of perturbations only if the axion decay constant f is above the Planck scale.”
A review of axion inflation in the era of Planck (2013, background): “One point worth stressing is that loop corrections induced by the N fields renormalize the Planck scale [31] in such a way to prevent inflation for very large N .”
The String Landscape and the Swampland (2005, background): “3 In the context of volume of field space for certain axion fields this finiteness was studied recently [2].”
Punctuated inflation and the low CMB multipoles (2008, background): “For example, it is known that the existence of a number of string axion fields can give rise to the following potential describing multi-field chaotic inflation [61]:”
On the possibility of large axion moduli spaces (2014, methodology): “In [12], it was noted that the overall volume of a Calabi-Yau (in string units) must not grow linearly with N , or else the Planck mass would grow as √ N , cancelling the Pythagorean gain from traveling along the diagonal.”
Non-Gaussianities in multi-field inflation (2006, background): “Originally, the axion fields that drive N-flation were assumed to have identical masses [6].”
Primordial black holes and gravitational waves from parametric amplification of curvature perturbations (2019, background): “Such a model can naturally arise from brane inflation and axion inflation [49–53].”
Non-Gaussianities and chiral gravitational waves in natural steep inflation (2012, background): “[5, 6, 7, 8, 9]) that aims at maintaining the properties of radiative stability of the axion-like field while changing the shape of V (Φ) to allow it to support inflation.”
Axion cosmology and the energy scale of inflation (2008, background): “For such models, Ne around 50 or 60 is expected, so any reasonable p is ruled out, including φ2 chaotic inflation [4] and the stringy Nflation [37] and Monodromy [38] models.”
F-term axion monodromy inflation (2014, background): “The first class of ideas involves multiple axions in an intricate way [11–14], while the second can be implemented with a single axion if there is a non-trivial monodromy in field space [15,16].”