MSSM flat direction inflation: slow roll, stability, fine-tuning and reheating

Allahverdi, Rouzbeh; Enqvist, Kari; García-Bellido, J.; Jokinen, Asko; Mazumdar, Anupam

doi:10.1088/1475-7516/2007/06/019

Cited by 206 publications

(414 citation statements)

References 55 publications

(104 reference statements)

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“…In the MSSM case, inflation occurs when the field values are much smaller than the Planck scale [49,50,51]. However, in our case, since we demand two epochs of slow roll, it necessarily requires that the initial values of the field (assuming, say, about 60 e-folds of inflation) be greater than M Pl .…”

Section: Discussionmentioning

confidence: 91%

“…In this work, we have investigated a two stage slow roll inflationary scenario sandwiching an intermediate period of deviation from inflation, driven by potentials that are similar in shape to certain MSSM potentials [49]. In the MSSM case, inflation occurs when the field values are much smaller than the Planck scale [49,50,51].…”

Section: Discussionmentioning

confidence: 99%

“…We had mentioned earlier that potentials of the type (1) are encountered in the Minimal Supersymmetric Standard Model (MSSM) [48], and that their role as an inflaton has been analyzed recently [49,50,51]. At this point it is important that we highlight the differences between MSSM inflation and the scenario we are considering.…”

Section: The Inflaton Potential and The Background Dynamicsmentioning

confidence: 93%

“…We find that the form of the potentials motivated by a class of certain minimal supersymmetric extensions of the standard model provide us with the desired behavior [48,49,50,51]. These large field models allow a period of fast roll sandwiched between two stages of slow roll inflation ‡.…”

Section: Introductionmentioning

confidence: 94%

See 3 more Smart Citations

Punctuated inflation and the low CMB multipoles

Jain

Chingangbam

Gong

et al. 2009

J. Cosmol. Astropart. Phys.

152

172

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Abstract. We investigate inflationary scenarios driven by a class of potentials which are similar in form to those that arise in certain minimal supersymmetric extensions of the standard model. We find that these potentials allow a brief period of departure from inflation sandwiched between two stages of slow roll inflation. We show that such a background behavior leads to a step like feature in the scalar power spectrum. We set the scales such that the drop in the power spectrum occurs at a length scale that corresponds to the Hubble radius today-a feature that seems necessary to explain the lower power observed in the quadrupole moment of the Cosmic Microwave Background (CMB) anisotropies. We perform a Markov Chain Monte Carlo analysis to determine the values of the model parameters that provide the best fit to the recent WMAP 5-year data for the CMB angular power spectrum. We find that an inflationary spectrum with a suppression of power at large scales that we obtain leads to a much better fit (with just one extra parameter, χ 2 eff improves by 6.62) of the observed data when compared to the best fit reference ΛCDM model with a featureless, power law, primordial spectrum.

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Section: Discussionmentioning

confidence: 91%

Section: Discussionmentioning

confidence: 99%

Section: The Inflaton Potential and The Background Dynamicsmentioning

confidence: 93%

Section: Introductionmentioning

confidence: 94%

See 2 more Smart Citations

Punctuated inflation and the low CMB multipoles

Jain

Chingangbam

Gong

et al. 2009

J. Cosmol. Astropart. Phys.

152

172

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“…2 . These models give rise to a wide range of scalar spectral indices [9,[12][13][14], including the whole range allowed by WMAP [2] 3 .…”

Section: Introductionmentioning

confidence: 99%

Nonperturbative production of matter and rapid thermalization after MSSM inflation

et al. 2011

Self Cite

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A gauge invariant combination of LLe sleptons within the Minimal Supersymmetric Standard Model is one of the few inflaton candidates that can naturally explain population of the observable sector and creation of matter after inflation. After the end of inflation, the inflaton oscillates coherently about the minimum of its potential, which is a point of enhanced gauged symmetry. This results in bursts of non-perturbative production of the gauge/gaugino and (s)lepton quanta. The subsequent decay of these quanta is very fast and leads to an extremely efficient transfer of the inflaton energy to (s)quarks via instant preheating. Around 20% of the inflaton energy density is drained during every inflaton oscillation. However, all of the Standard Model degrees of freedom (and their supersymmetric partners) do not thermalize immediately, since the large inflaton vacuum expectation value breaks the electroweak symmetry. After about 100 oscillations -albeit within one Hubble time -the amplitude of inflaton oscillations becomes sufficiently small, and all of the degrees of freedom will thermalize. This provides by far the most efficient reheating of the universe with the observed degrees of freedom.

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Phenomenological aspects of type IIB flux compactifications

Pajer

2009

Fortschritte der Physik

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The purpose of this work is to investigate how phenomenologically successful constructions in the field of high energy physics can be embedded into a fundamental theory, and what we can learn from this procedure. In fact, the synergy of an effective and a fundamental approach might be very fruitful. On the one hand, it poses several theoretical challenges to potential candidates for a fundamental theory, which might be ruled out or restricted in their generality. On the other hand, this mutual interplay can inspire new experiments and observations or suggest correlations which are invisible from an effective point of view. Our starting point is that string theory is entitled to be a valid candidate for a fundamental theory by a series of properties such as the fact that it is a consistent, UV‐finite, anomaly‐free quantum theory and it describes, in appropriate limits, quantum field theory and general relativity, hence providing a unified description of the four known forces. Within string theory, we choose to work in the framework of type IIB flux compactifications where the issue of moduli stabilization can be successfully addressed. On the phenomenological side, we focus on particle physics and cosmology, and in particular on the MSSM and the mechanism of inflation, respectively. We construct and study two different models of inflation in string theory. These are models of brane inflation, i.e. models where the primordial exponential expansion of the universe is driven by a scalar field representing the position of a D3‐brane (a 3+1‐dimensional dynamical object) in a compact space. We show explicitly that, allowing for fine tuning, a prolonged stage of slow‐roll inflation can be achieved during which perturbations are generated in good agreement with the CMB data. In addition, we give an example of the fruitful synergy we mentioned above. One of our two models, namely inflation at the tip, might induce also DBI inflation which produces peculiar features in the spectrum of density perturbations that might be looked for using CMB data. On the particle physics side, we consider a model, the large volume scenario (LVS), which, among other things, provides a rationale for a low scale susy‐breaking. We perform some checks on the consistency of LVS as a string theory model. To this end, we formulate an educated guess for the form of string loop corrections. We then show that physical predictions such as the soft susy‐breaking terms are actually surprisingly robust against the inclusion of these corrections.

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MSSM flat direction inflation: slow roll, stability, fine-tuning and reheating

Cited by 206 publications

References 55 publications

Punctuated inflation and the low CMB multipoles

Punctuated inflation and the low CMB multipoles

Nonperturbative production of matter and rapid thermalization after MSSM inflation

Phenomenological aspects of type IIB flux compactifications

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