Inflation and late-time cosmic acceleration in non-minimal Maxwell-<i>F</i>(<i>R</i>) gravity and the generation of large-scale magnetic fields

Bamba, Kazuharu; Odintsov, Sergei D.

doi:10.1088/1475-7516/2008/04/024

Cited by 196 publications

(173 citation statements)

References 87 publications

(150 reference statements)

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“…[21][22][23][24][25][26][27][42][43][44][45][46][47][48][49][50][51][52], in order to explain the origin of the large-scale magnetic fields in our universe. In such inflationary magnetogenesis scenarios, the magnetic fields are generically accompanied by the production of even larger electric fields.…”

Section: Constraints On Inflationary Magnetogenesismentioning

confidence: 99%

Schwinger effect in 4D de Sitter space and constraints on magnetogenesis in the early universe

Kobayashi

Afshordi

2014

J. High Energ. Phys.

145

229

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We investigate pair creation by an electric field in four-dimensional de Sitter space. The expectation value of the induced current is computed, using the method of adiabatic regularization. Under strong electric fields the behavior of the current is similar to that in flat space, while under weak electric fields the current becomes inversely proportional to the mass squared of the charged field. Thus we find that the de Sitter space obtains a large conductivity under weak electric fields in the presence of a charged field with a tiny mass. We then apply the results to constrain electromagnetic fields in the early universe. In particular, we study cosmological scenarios for generating large-scale magnetic fields during the inflationary era. Electric fields generated along with the magnetic fields can induce sufficiently large conductivity to terminate the phase of magnetogenesis. For inflationary magnetogenesis models with a modified Maxwell kinetic term, the generated magnetic fields cannot exceed 10 −30 G on Mpc scales in the present epoch, when a charged field carrying an elementary charge with mass of order the Hubble scale or smaller exists in the Lagrangian. Similar constraints from the Schwinger effect apply for other magnetogenesis mechanisms.

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Section: Constraints On Inflationary Magnetogenesismentioning

confidence: 99%

Schwinger effect in 4D de Sitter space and constraints on magnetogenesis in the early universe

Kobayashi

Afshordi

2014

J. High Energ. Phys.

145

229

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“…In order to improve EN gravity, one may add a (cosmological) constant to its Lagrangian (Padmanabhan 2003;Frieman 2008). Moreover, we can regard other modifications of Einstein gravity such as Lovelock gravity (Lovelock 1971;Lovelock 1972;Deruelle 1990;, brane world cosmology (Demetrian 2006;Brax 2003;Gergely 2006;Amarilla 2010), scalar-tensor theories (Jordan 1955;Brans 1961;Cai 2007;Fujii 2003;Sotiriou 2006;Giddings 1993;Gregory 1997;Ling 2013;Klepac 2002;Ghodrati 2008) and F (R) gravity (Bamba 2008;Cognola 2008;Corda 2009;Sotiriou 2010;Nojiri 2011;Hendi 2012;Hendi 2014a;Momeni 2014 ).…”

Section: Introductionmentioning

confidence: 99%

Dilatonic equation of hydrostatic equilibrium and neutron star structure

Hendi

Bordbar

Panah

et al. 2015

Astrophys Space Sci

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In this paper, we present a new hydrostatic equilibrium equation related to dilaton gravity. We consider a spherical symmetric metric to obtain the hydrostatic equilibrium equation of stars in 4-dimensions, and generalize TOV equation to the case of regarding a dilaton field. Then, we calculate the structure properties of neutron star using our obtained hydrostatic equilibrium equation employing the modern equations of state of neutron star matter derived from microscopic calculations. We show that the maximum mass of neutron star depends on the parameters of dilaton field and cosmological constant. In other words, by setting the parameters of new hydrostatic equilibrium equation, we calculate the maximum mass of neutron star.

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“…In the evolution of the early Universe, such a kind of coupled terms may result in electromagnetic quantum fluctuations and lead to the inflation [8][9][10][11][12]. Recent investigations also show that these cross-terms have been used as attempts to explain the large scale magnetic fields observed in clusters of galaxies [13][14][15].…”

Section: Introductionmentioning

confidence: 99%

Rotating charged black hole with Weyl corrections

Chen

Jing

2014

Phys. Rev. D

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We present firstly a four-dimensional spherical symmetric black hole with small Weyl corrections and find that with increasing Weyl corrections the region of the event horizon existence for the black hole in the parameter space increases for the negative Weyl coupling parameter and decreases for the positive one. Moreover, we also obtain a rotating charged black hole with weak Weyl corrections by the method of complex coordinate transformation. Our results show that the sign of Weyl coupling parameter α yields the different spatial topology of the event horizons for the black hole with its parameters lied in some special regions in the parameter space. We also analyze the dependence of the ergosphere on the Weyl coupling parameter α and find that with the increase of the Weyl corrections the ergosphere in the equatorial plane becomes thick for a black hole with α > 0, but becomes thin in the case with α < 0, which means that the energy extraction become easier in the background of a black hole with the positive Weyl coupling parameter, but more difficult in the background of a black hole with the negative one.

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Inflation and late-time cosmic acceleration in non-minimal Maxwell-F(R) gravity and the generation of large-scale magnetic fields

Cited by 196 publications

References 87 publications

Schwinger effect in 4D de Sitter space and constraints on magnetogenesis in the early universe

Schwinger effect in 4D de Sitter space and constraints on magnetogenesis in the early universe

Dilatonic equation of hydrostatic equilibrium and neutron star structure

Rotating charged black hole with Weyl corrections

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