Finite density aspects of leptogenesis [Elektronische Ressource] / put forward by Andreas Hohenegger

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• Physik

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• Publié par: ruprecht-karls-universitat_heidelberg
• Publié le: 01 janvier 2010
• Nombre de lectures: 34
• Langue: Deutsch
• Poids de l'ouvrage: 1 Mo

Extrait

Dissertation
submitted to the
Combined Faculties of the Natural Sciences and Mathematics
of the Ruperto-Carola-University of Heidelberg, Germany
for the degree of
Doctor of Natural Sciences
Put forward by
Andreas Hohenegger
Born in Munich
Oral examination: 8 February 2010Finite Density Aspects of Leptogenesis
Referees: Prof. Dr. Manfred Lindner
Prof. Dr. Salmhofer...Zuerst entwickeln sich majestätisch die Variationen der Geschwindigkeiten,
dann setzen von der einen Seite die Zustands-Gleichungen, von der anderen
die Gleichungen der Centralbewegung ein, immer höher wogt das Chaos der
Formeln; plötzlich ertönen die vier Worte: “Putn = 5.” Der böse DämonV
verschwindet, wie in der Musik eine wilde, bisher alles unterwühlende Figur
der Bässe plötzlich verstummt; wie mit einem Zauberschlage ordnet sich, was
früher unbezwingbar schien...
(Ludwig Boltzmann, 1887)Aspekte der Leptogenese bei endlichen Dichten
Leptogenese ist ein Modell zur dynamischen Erklärung der Materie-Antimaterie Asymmetrie.
Dieser Prozess findet im frühen Universum bei hohen Temperaturen statt und eine Abweichung
vom Gleichgewicht ist fundamentale Voraussetzung für die Erzeugung der Asymmetrie. Die
Beschreibung dieses Prozesses basiert auf klassischen Boltzmann Gleichungen (BGn). Diese wur-
den durch die Verwendung thermaler Propagatoren verfeinert. In Anbetracht der grundlegenden
Beschränkungen dieser Gleichungen erscheint es wünschenswert einen systematischen Ansatz zu
entwickeln der auf Nicht-Gleichgewichts QFT beruht. In dieser Arbeit werden modifizierte BGn
verwendet die aus ersten Prinzipien innerhalb des Kadanoff–Baym Formalismus hergeleitet wer-
den. Dies wird für ein einfaches Toy-Modell durchgeführt welches ausreichend komplex ist um
populäre Szenarien wie das der thermalen Leptogenese in Analogie untersuchen zu können. Dieser
Ansatz legt die Struktur der korrigierten BGn offen und führt zu einem neuen Ergebnis für die
thermalen Beiträge zum CP-verletzenden Parameter, sodass die gängige Form überdacht werden
muss. Es stellt sich heraus, dass die verschiedenen Ansätze in Einklang gebracht werden können.
Die neuen Ergebnisse sagen eine Verstärkung der Asymmetrie vorher. Die Grösse der Korrekturen
innerhalb des Toy-Modells wird durch numerische Lösung der vollen BGn bestimmt.
Finite Density Aspects of Leptogenesis
Leptogenesis is a model for the dynamical generation of the matter-antimatter asymmetry. This
process takes place in the early universe at very high temperatures and a deviation from equilib-
rium is a fundamental requirement for the formation of the asymmetry. The equations used for its
description originate from classical Boltzmann equations (BEs), which were refined using ther-
mal propagators. In view of the basic restrictions of BEs, it is desirable to develop a systematic
approach which uses non-equilibrium QFT as starting point. In this thesis modified BEs are used
which are derived from first principles in the Kadanoff–Baym formalism. This is done for a simple
toy model which is sufficiently intricate to study popular scenarios such as thermal leptogenesis
in analogy to the phenomenological theory. This approach uncovers the structure of the corrected
BEs and leads to a new result for the form of the thermal contributions to the CP-violating param-
eter, so that the established one must be reconsidered. It turns out that the different approaches
can be reconciled. The new form predicts an enhancement of the asymmetry. The quantitative
implications of the medium corrections within the toy model are studied numerically in terms of
the full BEs.Contents
1 Introduction 7
1.1 Overview . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7
1.2 General considerations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 11
1.3 Thermal leptogenesis . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 13
2 Bottom-up approach 19
2.1 Toy model . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 19
2.2 S-matrix elements . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 20
2.3 Kinetic theory . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 22
2.4 Rate equations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 26
2.5 CP-violating parameter . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 32
3 Top-down approach 37
3.1 Schwinger–Keldysh formalism in curved space-time . . . . . . . . . . . . . . . 37
3.1.1 Schwinger–Dyson equations . . . . . . . . . . . . . . . . . . . . . . . . 38
3.1.2 2PI effective action . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 41
3.1.3 Kadanoff–Baym equations . . . . . . . . . . . . . . . . . . . . . . . . . 42
3.1.4 Quantum kinetic . . . . . . . . . . . . . . . . . . . . . . . . . 44
3.1.5 Boltzmann kinetic equations . . . . . . . . . . . . . . . . . . . . . . . . 51
3.2 Quantum corrected Boltzmann equations . . . . . . . . . . . . . . . . . . . . . . 56
3.2.1 Kadanoff–Baym equations . . . . . . . . . . . . . . . . . . . . . . . . . 56
3.2.2 Boltzmann kinetic . . . . . . . . . . . . . . . . . . . . . . . . 60
3.2.3 CP-violating parameter . . . . . . . . . . . . . . . . . . . . . . . . . . . 64
4 Finite temperature field theory approach 71
4.1 Physical and ghost fields . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 73
4.2 Causal n-point functions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 77
5 Numerical results 81
5.1 Numerical method . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 82
5.2 results . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 90
56 Conclusion 95
A Kadanoff–Baym formalism for complex scalars 99
B Calculation of the self-energies 107
C Generalized optical theorem and cutting rules 111
D Reduction of the collision integral 113
6Chapter 1
Introduction
1.1 Overview
While the standard model of particle physics combined with the big-bang theory for the forma-
tion of the universe predicts an approximate symmetry between matter and antimatter, the latter is
almost completely absent on earth and in the solar system. The obvious conclusion that the uni-
verse is baryonically asymmetric is confirmed by experimental data on the abundances of the light
elements predicted by primordial nucleosynthesis [5–7] and precise measurements of the cosmic
microwave background anisotropies [8, 9] by the WMAP satellite experiment. As it is somewhat
unsatisfactory and insufficient to assume that this asymmetry comes as an initial condition of the
universe, many possible mechanisms have been proposed to generate the asymmetry in a dynamic
way. It has been shown that this possibility exists if three conditions are met. Two of these directly
address extensions of the standard model and since 1967, when Sakharov found these require-
ments [10], numerous possible scenarios have been invented which can rather satisfactorily fulfill
them. Some of these became disfavoured or were ruled out later.
A viable class of models which has attracted a lot of attention in recent years is known as leptoge-
nesis [11]. Here the asymmetry is initially produced in the lepton sector and (partially) converted
to the baryon sector subsequently [12, 13]. The success of this scenario is partly due to the fact
that the required extension of the standard model, through the implementation of Majorana mass
terms, is relatively moderate and tightly linked to a favored mechanism for the generation of the
neutrino masses. Another advantage is that a non-vanishingB L asymmetry is produced which
survives the conversion process to baryons, in contrast to aB andL asymmetry withB L = 0.
Many aspects of leptogenesis have been extensively investigated. In particular, it has been studied
in the context of supersymmetry and it has been shown that the CP-violating parameter and the
efficiency of leptogenesis are affected by the flavor structure of the neutrino Yukawa couplings
[14–20]. It has also been shown that the creation of the asymmetry may be resonantly enhanced if
the Majorana neutrino masses are quasi-degenerate [21–24].
Comparatively few progress has been made towards a better understanding of the underlying ki-
netic equations which are needed to implement the third Sakharov condition, namely the necessity
of a deviation from thermal equilibrium. In most of the models it is realized with help of a standard
out-of-equilibrium decay scenario. This scenario is based on the fact that, because of the rapid ex-
pansion of the universe, a relatively weakly interacting massive particle species (heavy Majorana
neutrinos in the case of leptogenesis) may fail to follow its equilibrium abundance while it decays.
71.1. Overview Chapter 1. Introduction
This process takes place at high temperatures which approximately correspond to the mass of the
9heavy Majorana neutrinos, in the simplest case of thermal leptogenesis aboveT& 10 GeV. In
practice, the detailed time evolution of the abundances of the different species in this scenario is
investigated by solving rate equations, as in many cases in cosmology. These phenomenological
equations are usually constructed from generalized Boltzmann equations [25–29] in a bottom-up
appr