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 4.3 Theoretical and experimental constraints We discuss the relevant theoretical and experimental constraints in this section. 4.3.1 Vacuum Stability condition The scalar potential 𝑉(𝐻, Φ, 𝜒) must be bounded from below [195] and it can be determined from the following symmetric matrix which comes from the quadratic part of the potential, Above matrix will be positive-definite if following conditions are satisfied, 4.3.2 Invisible Higgs width constraint In our model, ℎ1 scalar is SM Higgs by choice, which is the mixed state of three real scalar fields from eq. 4.6. 4.3.3 Relic density constraint The relic density bound is from Planck satellite data [49]. Any DM candidate must satisfy the relic bound given in equation 4.42. 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 4.3 Theoretical and experimental constraints We discuss the relevant theoretical and experimental constraints in this section. 4.3.1 Vacuum Stability condition The scalar potential 𝑉(𝐻, Φ, 𝜒) must be bounded from below [195] and it can be determined from the following symmetric matrix which comes from the quadratic part of the potential, Above matrix will be positive-definite if following conditions are satisfied, 4.3.2 Invisible Higgs width constraint In our model, ℎ1 scalar is SM Higgs by choice, which is the mixed state of three real scalar fields from eq. 4.6. 4.3.3 Relic density constraint The relic density bound is from Planck satellite data [49]. Any DM candidate must satisfy the relic bound given in equation 4.42. 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.

Part of HackerNoon's growing list of open-source research papers, promoting free access to academic material.

Evidence

Dark Matter Analysis: A Lifetime Study

A Phenomenological Study of WIMP Models: Considering a BSM Framework

PHENOMENOLOGY.tech

Too Long; Didn't Read

Get Free Unlimited IP Geo Data With IPinfo Lite

A Phenomenological Study: Discussing the Relevant Theoretical and Experimental Constraints

About Author

Comments

TOPICS

THIS ARTICLE WAS FEATURED IN

Related Stories

A Phenomenological Study of WIMP Models: A Summary of Everything We Discussed

Extreme Axions Unveiled: A Novel Fluid Approach for Cosmological Modeling - Abstract and Intro

Extreme Axions Unveiled: Conclusion

Extreme Axions Unveiled: Acknowledgments & References

Extreme Axions Unveiled: A Novel Fluid Approach for Cosmological Modeling - Phenomenology

Extreme Axions Unveiled: Discussion and Future Work

A Phenomenological Study of WIMP Models: A Summary of Everything We Discussed

Extreme Axions Unveiled: A Novel Fluid Approach for Cosmological Modeling - Abstract and Intro

Extreme Axions Unveiled: Conclusion

Extreme Axions Unveiled: Acknowledgments & References

Extreme Axions Unveiled: A Novel Fluid Approach for Cosmological Modeling - Phenomenology

Extreme Axions Unveiled: Discussion and Future Work

Light-Mode

Classic

Newspaper

Dark-Mode

Neon Noir

Minty

HN StartUps