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@ARTICLE{Westphal:172332,
      author       = {Westphal, Alexander},
      title        = {{S}tring {C}osmology - {L}arge-{F}ield {I}nflation in
                      {S}tring {T}heory},
      reportid     = {PUBDB-2014-03682, DESY-14-149},
      year         = {2014},
      note         = {34 pages, 1 figure, LaTeX, to be published in 'Perspectives
                      in String Phenomenology'},
      abstract     = {This 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.},
      keywords     = {inflation: model (autogen) / scale: inflation (autogen) /
                      cosmic background radiation: polarization (autogen) /
                      gravitational radiation: primordial (autogen) / correction:
                      quantum (autogen) / field theory: scalar (autogen) / string
                      model (autogen) / string (autogen) / cosmological model
                      (autogen) / grand unified theory (autogen) / power spectrum
                      (autogen) / fractional (autogen) / monodromy (autogen) /
                      inflaton (autogen) / B-mode (autogen) / axion (autogen)},
      cin          = {T},
      cid          = {I:(DE-H253)T-20120731},
      pnm          = {514 - Theoretical Particle Physics (POF2-514)},
      pid          = {G:(DE-HGF)POF2-514},
      experiment   = {EXP:(DE-MLZ)NOSPEC-20140101},
      typ          = {PUB:(DE-HGF)25 / PUB:(DE-HGF)15},
      eprint       = {1409.5350},
      howpublished = {arXiv:1409.5350},
      archivePrefix = {arXiv},
      SLACcitation = {$\%\%CITATION$ = $arXiv:1409.5350;\%\%$},
      url          = {https://bib-pubdb1.desy.de/record/172332},
}