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000172332 0247_ $$2arXiv$$aarXiv:1409.5350
000172332 0247_ $$2altmetric$$aaltmetric:2696251
000172332 0247_ $$2inspire$$ainspire:1317862
000172332 037__ $$aPUBDB-2014-03682
000172332 041__ $$aEnglish
000172332 0881_ $$aDESY-14-149
000172332 088__ $$2DESY$$aDESY-14-149
000172332 1001_ $$0P:(DE-H253)PIP1013212$$aWestphal, Alexander$$b0$$eCorresponding Author$$udesy
000172332 245__ $$aString Cosmology - Large-Field Inflation in String Theory
000172332 260__ $$c2014
000172332 3367_ $$2DRIVER$$apreprint
000172332 3367_ $$028$$2EndNote$$aElectronic Article
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000172332 500__ $$a34 pages, 1 figure, LaTeX, to be published in 'Perspectives in String Phenomenology'
000172332 520__ $$aThis is a short review of string cosmology. We wish to connect string-scale physics as closely as possible to observables accessible to current or near-future experiments. Our possible best hope to do so is a description of inflation in string theory. The energy scale of inflation can be as high as that of Grand Unification (GUT). If this is the case, this is the closest we can possibly get in energy scales to string-scale physics. Hence, GUT-scale inflation may be our best candidate phenomenon to preserve traces of string-scale dynamics. Our chance to look for such traces is the primordial gravitational wave, or tensor mode signal produced during inflation. For GUT-scale inflation this is strong enough to be potentially visible as a B-mode polarization of the cosmic microwave background (CMB). Moreover, a GUT-scale inflation model has a trans-Planckian excursion of the inflaton scalar field during the observable amount of inflation. Such large-field models of inflation have a clear need for symmetry protection against quantum corrections. This makes them ideal candidates for a description in a candidate fundamental theory like string theory. At the same time the need of large-field inflation models for UV completion makes them particularly susceptible to preserve imprints of their string-scale dynamics in the inflationary observables, the spectral index $n_s$ and the fractional tensor mode power $r$. Hence, we will focus this review on axion monodromy inflation as a mechanism of large-field inflation in string theory.
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000172332 650_7 $$2autogen$$ainflation: model
000172332 650_7 $$2autogen$$ascale: inflation
000172332 650_7 $$2autogen$$acosmic background radiation: polarization
000172332 650_7 $$2autogen$$agravitational radiation: primordial
000172332 650_7 $$2autogen$$acorrection: quantum
000172332 650_7 $$2autogen$$afield theory: scalar
000172332 650_7 $$2autogen$$astring model
000172332 650_7 $$2autogen$$astring
000172332 650_7 $$2autogen$$acosmological model
000172332 650_7 $$2autogen$$agrand unified theory
000172332 650_7 $$2autogen$$apower spectrum
000172332 650_7 $$2autogen$$afractional
000172332 650_7 $$2autogen$$amonodromy
000172332 650_7 $$2autogen$$ainflaton
000172332 650_7 $$2autogen$$aB-mode
000172332 650_7 $$2autogen$$aaxion
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000172332 9141_ $$y2014
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