The f(R) gravity function of the Linde quintessence

We calculate the f(R) gravity function in the dual gravity description of the quintessence model with a quadratic (Linde) scalar potential and a positive cosmological constant. We find that in the large curvature regime relevant to chaotic inflation in Early Universe, the dual f(R) gravity is well a...
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Autor*in:	Sergei V. Ketov [verfasserIn] Natsuki Watanabe [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2015

Übergeordnetes Werk:	In: Physics Letters B - Elsevier, 2015, 741(2015), Seite 242-245
Übergeordnetes Werk:	volume:741 ; year:2015 ; pages:242-245

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.1016/j.physletb.2014.12.047

Katalog-ID:	DOAJ066339723

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spelling	10.1016/j.physletb.2014.12.047 doi (DE-627)DOAJ066339723 (DE-599)DOAJc29a6c7d2c7b431684ba993c617a304e DE-627 ger DE-627 rakwb eng QC1-999 Sergei V. Ketov verfasserin aut The f(R) gravity function of the Linde quintessence 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We calculate the f(R) gravity function in the dual gravity description of the quintessence model with a quadratic (Linde) scalar potential and a positive cosmological constant. We find that in the large curvature regime relevant to chaotic inflation in Early Universe, the dual f(R) gravity is well approximated by the (matter) loop-corrected Starobinsky inflationary model. In the small curvature regime relevant to dark energy in the Present Universe, the f(R) gravity function reduces to the Einstein–Hilbert one with a positive cosmological constant. Physics Natsuki Watanabe verfasserin aut In Physics Letters B Elsevier, 2015 741(2015), Seite 242-245 (DE-627)266015360 (DE-600)1466612-1 18732445 nnns volume:741 year:2015 pages:242-245 https://doi.org/10.1016/j.physletb.2014.12.047 kostenfrei https://doaj.org/article/c29a6c7d2c7b431684ba993c617a304e kostenfrei http://www.sciencedirect.com/science/article/pii/S0370269314009289 kostenfrei https://doaj.org/toc/0370-2693 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ SSG-OLC-PHA GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2025 GBV_ILN_2034 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2064 GBV_ILN_2111 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 741 2015 242-245
allfields_unstemmed	10.1016/j.physletb.2014.12.047 doi (DE-627)DOAJ066339723 (DE-599)DOAJc29a6c7d2c7b431684ba993c617a304e DE-627 ger DE-627 rakwb eng QC1-999 Sergei V. Ketov verfasserin aut The f(R) gravity function of the Linde quintessence 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We calculate the f(R) gravity function in the dual gravity description of the quintessence model with a quadratic (Linde) scalar potential and a positive cosmological constant. We find that in the large curvature regime relevant to chaotic inflation in Early Universe, the dual f(R) gravity is well approximated by the (matter) loop-corrected Starobinsky inflationary model. In the small curvature regime relevant to dark energy in the Present Universe, the f(R) gravity function reduces to the Einstein–Hilbert one with a positive cosmological constant. Physics Natsuki Watanabe verfasserin aut In Physics Letters B Elsevier, 2015 741(2015), Seite 242-245 (DE-627)266015360 (DE-600)1466612-1 18732445 nnns volume:741 year:2015 pages:242-245 https://doi.org/10.1016/j.physletb.2014.12.047 kostenfrei https://doaj.org/article/c29a6c7d2c7b431684ba993c617a304e kostenfrei http://www.sciencedirect.com/science/article/pii/S0370269314009289 kostenfrei https://doaj.org/toc/0370-2693 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ SSG-OLC-PHA GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2025 GBV_ILN_2034 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2064 GBV_ILN_2111 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 741 2015 242-245
allfieldsGer	10.1016/j.physletb.2014.12.047 doi (DE-627)DOAJ066339723 (DE-599)DOAJc29a6c7d2c7b431684ba993c617a304e DE-627 ger DE-627 rakwb eng QC1-999 Sergei V. Ketov verfasserin aut The f(R) gravity function of the Linde quintessence 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We calculate the f(R) gravity function in the dual gravity description of the quintessence model with a quadratic (Linde) scalar potential and a positive cosmological constant. We find that in the large curvature regime relevant to chaotic inflation in Early Universe, the dual f(R) gravity is well approximated by the (matter) loop-corrected Starobinsky inflationary model. In the small curvature regime relevant to dark energy in the Present Universe, the f(R) gravity function reduces to the Einstein–Hilbert one with a positive cosmological constant. Physics Natsuki Watanabe verfasserin aut In Physics Letters B Elsevier, 2015 741(2015), Seite 242-245 (DE-627)266015360 (DE-600)1466612-1 18732445 nnns volume:741 year:2015 pages:242-245 https://doi.org/10.1016/j.physletb.2014.12.047 kostenfrei https://doaj.org/article/c29a6c7d2c7b431684ba993c617a304e kostenfrei http://www.sciencedirect.com/science/article/pii/S0370269314009289 kostenfrei https://doaj.org/toc/0370-2693 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ SSG-OLC-PHA GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2025 GBV_ILN_2034 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2064 GBV_ILN_2111 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 741 2015 242-245
allfieldsSound	10.1016/j.physletb.2014.12.047 doi (DE-627)DOAJ066339723 (DE-599)DOAJc29a6c7d2c7b431684ba993c617a304e DE-627 ger DE-627 rakwb eng QC1-999 Sergei V. Ketov verfasserin aut The f(R) gravity function of the Linde quintessence 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We calculate the f(R) gravity function in the dual gravity description of the quintessence model with a quadratic (Linde) scalar potential and a positive cosmological constant. We find that in the large curvature regime relevant to chaotic inflation in Early Universe, the dual f(R) gravity is well approximated by the (matter) loop-corrected Starobinsky inflationary model. In the small curvature regime relevant to dark energy in the Present Universe, the f(R) gravity function reduces to the Einstein–Hilbert one with a positive cosmological constant. Physics Natsuki Watanabe verfasserin aut In Physics Letters B Elsevier, 2015 741(2015), Seite 242-245 (DE-627)266015360 (DE-600)1466612-1 18732445 nnns volume:741 year:2015 pages:242-245 https://doi.org/10.1016/j.physletb.2014.12.047 kostenfrei https://doaj.org/article/c29a6c7d2c7b431684ba993c617a304e kostenfrei http://www.sciencedirect.com/science/article/pii/S0370269314009289 kostenfrei https://doaj.org/toc/0370-2693 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ SSG-OLC-PHA GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2025 GBV_ILN_2034 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2064 GBV_ILN_2111 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 741 2015 242-245
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author	Sergei V. Ketov
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title	The f(R) gravity function of the Linde quintessence
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title_full	The f(R) gravity function of the Linde quintessence
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title_sort	f(r) gravity function of the linde quintessence
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title_auth	The f(R) gravity function of the Linde quintessence
abstract	We calculate the f(R) gravity function in the dual gravity description of the quintessence model with a quadratic (Linde) scalar potential and a positive cosmological constant. We find that in the large curvature regime relevant to chaotic inflation in Early Universe, the dual f(R) gravity is well approximated by the (matter) loop-corrected Starobinsky inflationary model. In the small curvature regime relevant to dark energy in the Present Universe, the f(R) gravity function reduces to the Einstein–Hilbert one with a positive cosmological constant.
abstractGer	We calculate the f(R) gravity function in the dual gravity description of the quintessence model with a quadratic (Linde) scalar potential and a positive cosmological constant. We find that in the large curvature regime relevant to chaotic inflation in Early Universe, the dual f(R) gravity is well approximated by the (matter) loop-corrected Starobinsky inflationary model. In the small curvature regime relevant to dark energy in the Present Universe, the f(R) gravity function reduces to the Einstein–Hilbert one with a positive cosmological constant.
abstract_unstemmed	We calculate the f(R) gravity function in the dual gravity description of the quintessence model with a quadratic (Linde) scalar potential and a positive cosmological constant. We find that in the large curvature regime relevant to chaotic inflation in Early Universe, the dual f(R) gravity is well approximated by the (matter) loop-corrected Starobinsky inflationary model. In the small curvature regime relevant to dark energy in the Present Universe, the f(R) gravity function reduces to the Einstein–Hilbert one with a positive cosmological constant.
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title_short	The f(R) gravity function of the Linde quintessence
url	https://doi.org/10.1016/j.physletb.2014.12.047 https://doaj.org/article/c29a6c7d2c7b431684ba993c617a304e http://www.sciencedirect.com/science/article/pii/S0370269314009289 https://doaj.org/toc/0370-2693
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score	7.401078

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The f(R) gravity function of the Linde quintessence

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Zugang & Verfügbarkeit

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