On inflation and axionic dark matter in a scaled gravity

被引：1

作者：

Belhaj, A. ^{[1
]}

Ennadifi, S. E. ^{[2
]}

Lamaaoune, M. ^{[1
]}

机构：

[1] Univ Mohammed V Rabat, Fac Sci, Dept Phys, Equipe Sci Matiere & Rayonnement,ESMaR, Rabat, Morocco

[2] Univ Mohammed V Rabat, Fac Sci, LPHE MS, Rabat, Morocco

来源：

EUROPEAN PHYSICAL JOURNAL PLUS | 2024年 / 139卷 / 02期

基金：

英国科研创新办公室;

关键词：

HUBBLE-SPACE-TELESCOPE; CP CONSERVATION; CONSTRAINTS; CONSTANT; FLATNESS; UNIVERSE; HORIZON;

D O I：

10.1140/epjp/s13360-024-04965-y

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

Motivated by the modified gravity theories F(R)not equal R\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$F(R)\ne R$$\end{document} and inflationary physics, we first propose and investigate an inflation model in a scaled gravity F(R)=R+beta R\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$F(R)=R\,+\beta R$$\end{document}, where beta\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\beta $$\end{document} is a dimensionless scaling parameter. The latter is also implemented in a particular potential V(phi)=M41-cos phi mu beta\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$V(\phi )=M<^>{4}\left[ 1-\cos \left( \frac{\phi }{\mu }\right) <^>{\beta }\right] $$\end{document} being considered to drive the inflation via a parameter coupling scenario. Using the slow-roll approximations, the gravity scale parameter beta\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\beta $$\end{document} is approached with respect to the range of the associated computed cosmological observables ns\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$n_{s}$$\end{document} and r according to the recent Planck and BICEP/Keck data. Then, we discuss the axionic dark matter in the suggested gravity model by considering the case where the inflaton is taken to be identified with an axion-like field phi=fa theta\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\phi =f_{a}\theta $$\end{document} with the decay constant fa=mu\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$f_{a}=\mu $$\end{document}. Referring to the known data, the underlying inflation scale M is constrained to be much lower than the corresponding axion scale MMUCH LESS-THANfa\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$M\ll f_{a}$$\end{document}.

引用

页数：10

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