Erratum: A Little Inflation in the Early Universe at the QCD Phase Transition [Phys. Rev. Lett.<b>105</b>, 041301 (2010)]

Boeckel, Tillmann; Schaffner-Bielich, J.

doi:10.1103/physrevlett.106.069901

Cited by 37 publications

(36 citation statements)

References 9 publications

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“…We demonstrate that both the extension and mass of the most extended polytropic spheres, when the role of the cosmological constant has to be very important putting even strong limits on the extension of such structures, can be in agreement with the data restricting dark matter halos -their extension and mass have to be ∼ 100 kpc and ∼ 10 12 M ⊙ for galaxies of the type of the Milky Way, going up to ∼ 1 Mpc and ∼ 10 14 M ⊙ for the largest galaxies [145] or even larger radius and mass for galaxy clusters. It is interesting that the polytropic spheres can be relevant also in the framework of the so called little inflation [146] related to the first order phase transition of quark gluon plasma to the hadron phase at non-negligible baryon number [147] that implies existence of dark matter halos of mass M cluster ∼ 10 6 M ⊙ relevant for the physics of globular clusters and emergence of first stars [148].…”

Section: Discussionmentioning

confidence: 99%

General relativistic polytropes with a repulsive cosmological constant

2016

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Spherically symmetric equilibrium configurations of perfect fluid obeying a polytropic equation of state are studied in spacetimes with a repulsive cosmological constant. The configurations are specified in terms of three parameters-the polytropic index n, the ratio of central pressure and central energy density of matter σ, and the ratio of energy density of vacuum and central density of matter λ. The static equilibrium configurations are determined by two coupled first-order nonlinear differential equations that are solved by numerical methods with the exception of polytropes with n = 0 corresponding to the configurations with uniform distribution of energy density, when the solution is given in terms of elementary functions. The geometry of the polytropes is conveniently represented by embedding diagrams of both the ordinary space geometry and the optical reference geometry reflecting some dynamical properties of the geodesic motion. The polytropes are represented by radial profiles of energy density, pressure, mass, and metric coefficients. For all tested values of n > 0, the static equilibrium configurations with fixed parameters n, σ, are allowed only up to a critical value of the cosmological parameter λc = λc(n, σ). In the case of n > 3, the critical value λc tends to zero for special values of σ. The gravitational potential energy and the binding energy of the polytropes are determined and studied by numerical methods. We discuss in detail the polytropes with extension comparable to those of the dark matter halos related to galaxies, i.e., with extension ℓ > 100 kpc and mass M > 10 12 M⊙. For such largely extended polytropes the cosmological parameter relating the vacuum energy to the central density has to be larger than λ = ρvac/ρc ∼ 10 −9 . We demonstrate that extension of the static general relativistic polytropic configurations cannot exceed the so called static radius related to their external spacetime, supporting the idea that the static radius represents a natural limit on extension of gravitationally bound configurations in an expanding universe dominated by the vacuum energy.PACS numbers: 98.80. Es,

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Section: Discussionmentioning

confidence: 99%

General relativistic polytropes with a repulsive cosmological constant

2016

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“…Depending on the order of the transition there might be today several observable relics like quark nuggets, magnetic fields, and the modification of the primordial background of gravitational waves [10,13]. If the transition were of first order, the universe might have undergone a second period of inflation, suggested by [14]. We want to review here our results on the effect of leptons on the transition [3] and show, how they change Fig.…”

Section: The Cosmic Qcd Transitionmentioning

confidence: 94%

Particle asymmetries in the early universe

Stuke

2011

Progress in Particle and Nuclear Physics

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The total lepton asymmetry $l=\sum_f l_f$ in our universe is only poorly constrained by theories and experiments. It might be orders of magnitudes larger than the observed baryon asymmetry $b\simeq {\cal O}(10^{-10})$, $|l|/b \leq {\cal O}(10^{9})$. We found that the dynamics of the cosmic QCD transition changes for large asymmetries. Predictions for asymmetries in a single flavour $l_f$ allow even larger values. We find that asymmetries of $l_f\leq {\cal O}(1)$ in a single or two flavours change the relic abundance of WIMPs. However, large lepton and large individual lepton flavour asymmetries influences significantly the dynamics of the early universe.Comment: 7 pages,8 figures; Proceedings of the Erice workshop on Nuclear Physics 2010 "Particle and Nuclear Astrophysics

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“…On the other hand the cosmological QCD phase transition does not seem to be associated with a key observable in today's universe. In this contribution we revisit the cosmological QCD phase transition and discuss some new cosmological signals in view of the little inflation scenario proposed by us [1,2]. The basic ingredients for a short inflationary period are an Affleck-Dine-type baryogenesis, in order to achieve a large initial baryon-to-photon ratio, and a metastable vacuum due to the nonvanishing vacuum expectation values of QCD at high net baryon densities.…”

Section: Introductionmentioning

confidence: 98%

The cosmological QCD phase transition revisited

Boeckel

Schettler

Schaffner-Bielich

2011

Progress in Particle and Nuclear Physics

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a b s t r a c tThe QCD phase diagram might exhibit a first order phase transition for large baryochemical potentials. We explore the cosmological implications of such a QCD phase transition in the early universe. We propose that the large baryon-asymmetry is diluted by a little inflation where the universe is trapped in a false vacuum state of QCD. The little inflation is stopped by bubble nucleation which leads to primordial production of the seeds of extragalactic magnetic fields, primordial black holes and gravitational waves. In addition the power spectrum of cold dark matter can be affected up to mass scales of 10 9 M ⊙ . The imprints of the cosmological QCD phase transition on the gravitational wave background can be explored with the future gravitational wave detectors LISA and BBO and with pulsar timing.

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Erratum: A Little Inflation in the Early Universe at the QCD Phase Transition [Phys. Rev. Lett.105, 041301 (2010)]

Cited by 37 publications

References 9 publications

General relativistic polytropes with a repulsive cosmological constant

General relativistic polytropes with a repulsive cosmological constant

Particle asymmetries in the early universe

The cosmological QCD phase transition revisited

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