Table of Links Acknowledgements 1 Introduction to thesis 1.1 History and Evidence 1.2 Facts on dark matter 1.3 Candidates to dark matter 1.4 Dark matter detection 1.5 Outline of the thesis 2 Dark matter through ALP portal and 2.1 Introduction 2.2 Model 2.3 Existing constraints on ALP parameter space 2.4 Dark matter analysis 2.5 Summary 3 A two component dark matter model in a generic 𝑈(1)𝑋 extension of SM and 3.1 Introduction 3.2 Model 3.3 Theoretical and experimental constraints 3.4 Phenomenology of dark matter 3.5 Relic density dependence on 𝑈(1)𝑋 charge 𝑥𝐻 3.6 Summary 4 A pseudo-scalar dark matter case in 𝑈(1)𝑋 extension of SM and 4.1 Introduction 4.2 Model 4.3 Theoretical and experimental constraints 4.4 Dark Matter analysis 4.5 Summary 5 Summary Appendices A Standard model B Friedmann equations C Type I seasaw mechanism D Feynman diagrams in two-component DM model Bibliography 1.5 Outline of the thesis To explain DM, we introduce a few simple WIMP models that can bypass present constraints and have observable signatures in the future. The main challenge in any WIMP-like DM model is to explain relic density and stringent direct detection bounds simultaneously. In later chapters, we describe a few models to counter these challenges. In this chapter 4, we have the particle and symmetry content similar to our previous model described in chapter 3, but with no Z2 symmetry. The U(1)𝑋 symmetry breaking results in a massive pseudo-scalar particle, which is the proposed candidate for dark matter. We study the parameter space where this massive pseudo-scalar particle has a lifetime much larger than the age of the universe. We constrain the allowed parameter space by the lifetime bound using perturbative unitarity, invisible Higgs width, and relic density bounds. The main advantage of having a pseudo-scalar DM is that it implies a vanishing scattering amplitude for direct detection at tree level in a non-relativistic limit. However, the one-loop level contribution could be finite, which we have studied and plotted against the current direct detection bounds. This paper is available on arxiv under CC BY 4.0 DEED license. Author:
(1) Shivam Gola, The Institute of Mathematical Sciences, Chennai. Table of Links Acknowledgements Acknowledgements 1 Introduction to thesis 1 Introduction to thesis 1.1 History and Evidence 1.1 History and Evidence 1.2 Facts on dark matter 1.2 Facts on dark matter 1.3 Candidates to dark matter 1.3 Candidates to dark matter 1.4 Dark matter detection 1.4 Dark matter detection 1.5 Outline of the thesis 1.5 Outline of the thesis 2 Dark matter through ALP portal and 2.1 Introduction 2 Dark matter through ALP portal and 2.1 Introduction 2.2 Model 2.2 Model 2.3 Existing constraints on ALP parameter space 2.3 Existing constraints on ALP parameter space 2.4 Dark matter analysis 2.4 Dark matter analysis 2.5 Summary 2.5 Summary 3 A two component dark matter model in a generic 𝑈(1)𝑋 extension of SM and 3.1 Introduction 3 A two component dark matter model in a generic 𝑈(1)𝑋 extension of SM and 3.1 Introduction 3.2 Model 3.2 Model 3.3 Theoretical and experimental constraints 3.3 Theoretical and experimental constraints 3.4 Phenomenology of dark matter 3.4 Phenomenology of dark matter 3.5 Relic density dependence on 𝑈(1)𝑋 charge 𝑥𝐻 3.5 Relic density dependence on 𝑈(1)𝑋 charge 𝑥𝐻 3.6 Summary 3.6 Summary 4 A pseudo-scalar dark matter case in 𝑈(1)𝑋 extension of SM and 4.1 Introduction 4 A pseudo-scalar dark matter case in 𝑈(1)𝑋 extension of SM and 4.1 Introduction 4.2 Model 4.2 Model 4.3 Theoretical and experimental constraints 4.3 Theoretical and experimental constraints 4.4 Dark Matter analysis 4.4 Dark Matter analysis 4.5 Summary 4.5 Summary 5 Summary 5 Summary Appendices Appendices A Standard model A Standard model B Friedmann equations B Friedmann equations C Type I seasaw mechanism C Type I seasaw mechanism D Feynman diagrams in two-component DM model D Feynman diagrams in two-component DM model Bibliography Bibliography 1.5 Outline of the thesis To explain DM, we introduce a few simple WIMP models that can bypass present constraints and have observable signatures in the future. The main challenge in any WIMP-like DM model is to explain relic density and stringent direct detection bounds simultaneously. In later chapters, we describe a few models to counter these challenges. In this chapter 4, we have the particle and symmetry content similar to our previous model described in chapter 3, but with no Z2 symmetry. The U(1)𝑋 symmetry breaking results in a massive pseudo-scalar particle, which is the proposed candidate for dark matter. We study the parameter space where this massive pseudo-scalar particle has a lifetime much larger than the age of the universe. We constrain the allowed parameter space by the lifetime bound using perturbative unitarity, invisible Higgs width, and relic density bounds. The main advantage of having a pseudo-scalar DM is that it implies a vanishing scattering amplitude for direct detection at tree level in a non-relativistic limit. However, the one-loop level contribution could be finite, which we have studied and plotted against the current direct detection bounds. This paper is available on arxiv under CC BY 4.0 DEED license. This paper is available on arxiv under CC BY 4.0 DEED license. available on arxiv Author: (1) Shivam Gola, The Institute of Mathematical Sciences, Chennai. Author: Author: (1) Shivam Gola, The Institute of Mathematical Sciences, Chennai.

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