12 December 2024
University of Oslo, Oslo, Norway
Europe/Oslo timezone

Dark Matter from Inflaton Field Perturbations and Primordial Spacetime Cavitation

Not scheduled
20m
Kristan Birkeland auditorium, Department of Physics, University of Oslo, Oslo, Norway. (University of Oslo, Oslo, Norway)

Kristan Birkeland auditorium, Department of Physics, University of Oslo, Oslo, Norway.

University of Oslo, Oslo, Norway

Speaker

Mr Swapnil Singh

Description

This study examines the formation of dark matter as a result of Primordial Spacetime Cavitation, driven by Inflaton Field Perturbations. Our theoretical framework integrates early universe dynamics with quantum field theory to explain the emergence of subatomic voids within the spacetime fabric. These cavitated regions, resulting from perturbations in the inflaton field, persist as stable or metastable vacua after inflation, affecting large-scale structure formation, contributing to the formation of dark matter.

We derive the stress-energy tensor ( T_{\mu\nu}^{\text{cav}} ) for these cavitated regions, incorporate them into the Einstein field equations, and calculate the resulting gravitational effects. Quantum fluctuations during inflation, described by the Klein-Gordon equation, induce variations in the potential energy landscape, leading to distinct vacuum states in spacetime. This process modifies the power spectrum of density fluctuations, which we compute using the slow-roll approximation and inflationary potential.

[
T_{\mu\nu}^{\text{cav}} = \rho_{\text{cav}} c^2 u_\mu u_\nu + p_{\text{cav}} g_{\mu\nu}
]

where ( \rho_{\text{cav}} ) is the energy density, ( p_{\text{cav}} ) is the pressure within cavitated regions, and ( u^\mu ) is the four-velocity of the cavitated fluid element.

The energy density ( \rho_{\text{cav}} ) in these regions, derived from the Friedmann equation, aligns with observations of the primordial power spectrum of density fluctuations indicating consistency with cosmological observations on large scales. The power spectrum ( P(k) ) of density fluctuations from cavitated regions matches the nearly scale-invariant nature observed in the Cosmic Microwave Background (CMB) data, validating our theoretical model within current observational constraints.

Using parameters such as ( A_s \approx 2.2 \times 10^{-9} ), ( n_s \approx 0.96 ), ( \frac{d n_s}{d \ln k} \approx -0.03 ), and ( k_{\text{pivot}} = 0.05 \text{ Mpc}^{-1} ), our theoretical model predicts ( P(0.1) \approx 2.25 \times 10^{-9} ), aligning closely with observational constraints.

Details

Swapnil Singh, Student, B.M.S College of Engineering, Bangalore, India - 560019

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Author

Mr Swapnil Singh

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