000293356 001__ 293356
000293356 005__ 20250717104556.0
000293356 0247_ $$2doi$$a10.1088/1475-7516/2016/01/001
000293356 0247_ $$2arXiv$$aarXiv:1509.00024
000293356 0247_ $$2WOS$$aWOS:000369734300001
000293356 0247_ $$2altmetric$$aaltmetric:4960714
000293356 0247_ $$2inspire$$ainspire:1391259
000293356 0247_ $$2openalex$$aopenalex:W2231561946
000293356 037__ $$aPUBDB-2016-00461
000293356 082__ $$a530
000293356 0881_ $$aDESY-15-166; arXiv: 1509.00024
000293356 088__ $$2DESY$$aDESY-15-166
000293356 088__ $$2arXiv$$aarXiv: 1509.00024
000293356 1001_ $$0P:(DE-H253)PIP1018435$$aBroy, Benedict$$b0$$eCorresponding author
000293356 245__ $$aStarobinsky-type inflation from $\alpha$′-corrections
000293356 260__ $$aLondon$$bIOP$$c2016
000293356 3367_ $$2DRIVER$$aarticle
000293356 3367_ $$2DataCite$$aOutput Types/Journal article
000293356 3367_ $$0PUB:(DE-HGF)29$$2PUB:(DE-HGF)$$aReport$$mreport
000293356 3367_ $$0PUB:(DE-HGF)16$$2PUB:(DE-HGF)$$aJournal Article$$bjournal$$mjournal$$s1482143171_20313
000293356 3367_ $$2BibTeX$$aARTICLE
000293356 3367_ $$2ORCID$$aJOURNAL_ARTICLE
000293356 3367_ $$00$$2EndNote$$aJournal Article
000293356 520__ $$aWorking in the Large Volume Scenario (LVS) of IIB Calabi-Yau flux compactifications, we construct inflationary models from recently computed higher derivative $(\alpha')^3$-corrections. Inflation is driven by a Kaehler modulus whose potential arises from the aforementioned corrections, while we use the inclusion of string loop effects just to ensure the existence of a graceful exit when necessary. The effective inflaton potential takes a Starobinsky-type form $V=V_0(1-e^{-\nu\phi})^2$, where we obtain one set-up with $\nu=-1/\sqrt{3}$ and one with $\nu=2/\sqrt{3}$ corresponding to inflation occurring for increasing or decreasing $\phi$ respectively. The inflationary observables are thus in perfect agreement with PLANCK, while the two scenarios remain observationally distinguishable via slightly varying predictions for the tensor-to-scalar ratio $r$. Both set-ups yield $r\simeq (2\ldots 7)\,\times 10^{-3}$. They hence realise inflation with moderately large fields $\left(\Delta\phi\sim 6\thinspace M_{Pl}\right)$ without saturating the Lyth bound. Control over higher corrections relies in part on tuning underlying microscopic parameters, and in part on intrinsic suppressions. The intrinsic part of control arises as a leftover from an approximate effective shift symmetry at parametrically large volume.
000293356 536__ $$0G:(DE-HGF)POF3-611$$a611 - Fundamental Particles and Forces (POF3-611)$$cPOF3-611$$fPOF III$$x0
000293356 536__ $$0G:(DE-HGF)2015_IFV-HZ-NG-603$$aHZ-NG-603 - Strings and Cosmology - an Interface for Testing fundamental Theories (2015_IFV-HZ-NG-603)$$c2015_IFV-HZ-NG-603$$x1
000293356 536__ $$0G:(EU-Grant)320421$$aSPLE - String Phenomenology in the LHC Era (320421)$$c320421$$fERC-2012-ADG_20120216$$x2
000293356 588__ $$aDataset connected to CrossRef
000293356 693__ $$0EXP:(DE-MLZ)NOSPEC-20140101$$5EXP:(DE-MLZ)NOSPEC-20140101$$eNo specific instrument$$x0
000293356 7001_ $$0P:(DE-H253)PIP1017434$$aCiupke, David$$b1
000293356 7001_ $$aPedro, Francisco G.$$b2
000293356 7001_ $$0P:(DE-H253)PIP1013212$$aWestphal, Alexander$$b3
000293356 773__ $$0PERI:(DE-600)2104147-7$$a10.1088/1475-7516/2016/01/001$$gVol. 2016, no. 01, p. 001 - 001$$n01$$p001 -$$tJournal of cosmology and astroparticle physics$$v2016$$x1475-7516$$y2016
000293356 7870_ $$0PUBDB-2015-03906$$aBroy, Benedict et.al.$$d2015$$iIsParent$$rIFT-UAM/CSIC-15-093, DESY-15-166$$tStarobinsky-Type Inflation from $\alpha'$-Corrections
000293356 8564_ $$uhttps://bib-pubdb1.desy.de/record/293356/files/pdf-2.pdf$$yOpenAccess
000293356 8564_ $$uhttps://bib-pubdb1.desy.de/record/293356/files/pdf-2.pdf?subformat=pdfa$$xpdfa$$yOpenAccess
000293356 909CO $$ooai:bib-pubdb1.desy.de:293356$$pdnbdelivery$$pec_fundedresources$$pVDB$$pdriver$$popen_access$$popenaire
000293356 9101_ $$0I:(DE-588b)2008985-5$$6P:(DE-H253)PIP1018435$$aDeutsches Elektronen-Synchrotron$$b0$$kDESY
000293356 9101_ $$0I:(DE-588b)2008985-5$$6P:(DE-H253)PIP1017434$$aDeutsches Elektronen-Synchrotron$$b1$$kDESY
000293356 9101_ $$0I:(DE-588b)2008985-5$$6P:(DE-H253)PIP1013212$$aDeutsches Elektronen-Synchrotron$$b3$$kDESY
000293356 9131_ $$0G:(DE-HGF)POF3-611$$1G:(DE-HGF)POF3-610$$2G:(DE-HGF)POF3-600$$3G:(DE-HGF)POF3$$4G:(DE-HGF)POF$$aDE-HGF$$bForschungsbereich Materie$$lMaterie und Universum$$vFundamental Particles and Forces$$x0
000293356 9141_ $$y2016
000293356 915__ $$0LIC:(DE-HGF)CCBY3$$2HGFVOC$$aCreative Commons Attribution CC BY 3.0
000293356 915__ $$0StatID:(DE-HGF)0200$$2StatID$$aDBCoverage$$bSCOPUS
000293356 915__ $$0StatID:(DE-HGF)0100$$2StatID$$aJCR$$bJ COSMOL ASTROPART P : 2014
000293356 915__ $$0StatID:(DE-HGF)9905$$2StatID$$aIF >= 5$$bJ COSMOL ASTROPART P : 2014
000293356 915__ $$0StatID:(DE-HGF)0150$$2StatID$$aDBCoverage$$bWeb of Science Core Collection
000293356 915__ $$0StatID:(DE-HGF)0111$$2StatID$$aWoS$$bScience Citation Index Expanded
000293356 915__ $$0StatID:(DE-HGF)0510$$2StatID$$aOpenAccess
000293356 915__ $$0StatID:(DE-HGF)1150$$2StatID$$aDBCoverage$$bCurrent Contents - Physical, Chemical and Earth Sciences
000293356 915__ $$0StatID:(DE-HGF)0420$$2StatID$$aNationallizenz
000293356 915__ $$0StatID:(DE-HGF)0199$$2StatID$$aDBCoverage$$bThomson Reuters Master Journal List
000293356 915__ $$0StatID:(DE-HGF)0570$$2StatID$$aSCOAP3
000293356 9201_ $$0I:(DE-H253)T-20120731$$kT$$lTheorie-Gruppe$$x0
000293356 980__ $$ajournal
000293356 980__ $$aVDB
000293356 980__ $$areport
000293356 980__ $$aI:(DE-H253)T-20120731
000293356 980__ $$aUNRESTRICTED
000293356 9801_ $$aUNRESTRICTED
000293356 9801_ $$aFullTexts