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Neutrinos and Dark Matter: Unseen Forces in the Universe

Discover the roles of neutrinos and dark matter in our cosmos.

Anirban Majumdar, Dimitrios K. Papoulias, Hemant Prajapati, Rahul Srivastava

― 4 min read


Neutrinos and Dark Matter Neutrinos and Dark Matter Explained particles and cosmic forces. Uncovering the mysteries of fundamental
Table of Contents

Neutrinos are tiny particles that are everywhere. They come from the sun, stars, and even from Earth’s own radioactive materials. They are so small that they can pass through just about anything without touching it. Imagine trying to catch a leaf falling from a tree in a strong wind - it's that hard to catch neutrinos.

The Mystery of Dark Matter

Now, let’s talk about dark matter. This is a bit of a mystery. Scientists can't see dark matter, but they know it’s there because of how it affects things we can see, like galaxies. It's like that sneaky friend who pulls the chair out from under you just before you sit down; you can't see them doing it, but you certainly feel their effects.

What is Neutrinoless Double Beta Decay?

Neutrinoless double beta decay sounds fancy, but it's quite simple. Usually, in a beta decay, neutrinos are emitted. In neutrinoless double beta decay, they are not. This could mean something interesting about particles called Majorana particles, which don't have an anti-version of themselves. If we find this decay, it would be a big deal in particle physics.

Lepton Flavor and Number Violations

Leptons are a group of particles that includes electrons and neutrinos. Lepton Flavor Violation means that, under certain conditions, one type of lepton can turn into another type. This is a bit like if your cat suddenly grew wings and started flying - it's not supposed to happen, but some strange things have been spotted.

Similarly, lepton number violation means that the total number of leptons can change. Imagine a room full of apples (leptons). If apples start turning into oranges (or other types of particles), you’ve got a violation.

What’s Up with Coherent Elastic Neutrino-Nucleus Scattering?

Coherent elastic neutrino-nucleus scattering, or CE NS for short, is when neutrinos hit a nucleus without losing a lot of energy. It’s like a soft touch on your arm; you know something is there, but it doesn’t knock you over. This process helps scientists learn more about both neutrinos and the nuclei they interact with.

The Importance of Chiral Gauge Models

Chiral gauge models are theories that describe how particles like neutrinos behave under certain conditions. These models help us understand why particles interact the way they do. It’s like having a map while hiking; it helps you find the best path.

The Role of Dark Hypercharge Symmetries

Dark Hypercharge Symmetries (DHC) are a set of rules about how particles interact under certain new symmetries. They add a twist to the game of particle physics. You could think of it like changing the rules of Monopoly mid-game; it changes everything.

Experimental Data from COHERENT

The COHERENT experiment is like a big science party where researchers collect data about how neutrinos interact with different materials. The data from this experiment helps tighten the constraints on our theories about particles, just like telling your friends they can’t bring snacks to your house party helps keep it clean.

The Search for Dark Matter

Scientists have many tools to search for dark matter, including experiments like XENONnT and PandaX-4T. These experiments aim to directly detect dark matter by looking for unusual interactions between dark matter particles and normal matter. It's like trying to find a specific grain of sand on a beach; it takes time and patience.

The Future: DARWIN Experiment

The DARWIN experiment promises to be a major player in the hunt for dark matter. It aims to improve our understanding of dark matter significantly. You can think of it as the upgrade to your favorite video game. With better graphics and more features, it can uncover secrets that the previous version couldn’t.

Why Does This Matter?

Understanding neutrinos and dark matter can tell us about the universe's beginnings and how it all works. These particles play a role in the fundamental structure of everything, from the smallest atoms to the biggest galaxies. Grasping these concepts helps us understand our place in the universe.

Conclusion

In summary, the world of neutrinos and dark matter is complex but fascinating. Every piece of information we uncover helps us fit together the puzzle of the universe. So, even if you can’t see these particles, you can certainly appreciate the role they play in our cosmic playground!

Original Source

Title: Constraining low scale Dark Hypercharge symmetry at spallation, reactor and Dark Matter direct detection experiments

Abstract: Coherent Elastic Neutrino-Nucleus (CE$\nu$NS) and Elastic Neutrino-Electron Scattering (E$\nu$ES) data are exploited to constrain "chiral" $U(1)_{X}$ gauged models with light vector mediator mass. These models fall under a distinct class of new symmetries called Dark Hypercharge Symmetries. A key feature is the fact that the $Z'$ boson can couple to all Standard Model fermions at tree level, with the $U(1)_X$ charges determined by the requirement of anomaly cancellation. Notably, the charges of leptons and quarks can differ significantly depending on the specific anomaly cancellation solution. As a result, different models exhibit distinct phenomenological signatures and can be constrained through various experiments. In this work, we analyze the recent data from the COHERENT experiment, along with results from Dark Matter (DM) direct detection experiments such as XENONnT, LUX-ZEPLIN, and PandaX-4T, and place new constraints on three benchmark models. Additionally, we set constraints from a performed analysis of TEXONO data and discuss the prospects of improvement in view of the next-generation DM direct detection DARWIN experiment.

Authors: Anirban Majumdar, Dimitrios K. Papoulias, Hemant Prajapati, Rahul Srivastava

Last Update: 2024-11-06 00:00:00

Language: English

Source URL: https://arxiv.org/abs/2411.04197

Source PDF: https://arxiv.org/pdf/2411.04197

Licence: https://creativecommons.org/licenses/by/4.0/

Changes: This summary was created with assistance from AI and may have inaccuracies. For accurate information, please refer to the original source documents linked here.

Thank you to arxiv for use of its open access interoperability.

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