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CosmoLattice
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abstract
This is the user manual for CosmoLattice, a modern package for lattice simulations of the dynamics of interacting scalar and gauge fields in an expanding universe. CosmoLattice incorporates a series of features that makes it very versatile and powerful: $i)$ it is written in C++ fully exploiting the object oriented programming paradigm, with a modular structure and a clear separation between the physics and the technical details, $ii)$ it is MPI-based and uses a discrete Fourier transform parallelized in multiple spatial dimensions, which makes it specially appropriate for probing scenarios with well-separated scales, running very high resolution simulations, or simply very long ones, $iii)$ it introduces its own symbolic language, defining field variables and operations over them, so that one can introduce differential equations and operators in a manner as close as possible to the continuum, $iv)$ it includes a library of numerical algorithms, ranging from $O(\delta t^2)$ to $O(\delta t^{10})$ methods, suitable for simulating global and gauge theories in an expanding grid, including the case of `self-consistent' expansion sourced by the fields themselves. Relevant observables are provided for each algorithm (e.g.~energy densities, field spectra, lattice snapshots) and we note that remarkably all our algorithms for gauge theories always respect the Gauss constraint to machine precision. In this manual we explain how to obtain and run CosmoLattice in a computer (let it be your laptop, desktop or a cluster). We introduce the general structure of the code and describe in detail the basic files that any user needs to handle. We explain how to implement any model characterized by a scalar potential and a set of scalar fields, either singlets or interacting with $U(1)$ and/or $SU(2)$ gauge fields. CosmoLattice is publicly available at www.cosmolattice.net.
Forward citations
Cited by 13 Pith papers
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Nonlinear Lattice Framework for Inflation: Bridging stochastic inflation and the $\delta{N}$ formalism
A shear-free locally FLRW lattice framework for single-field inflation captures spatially varying expansion, curvature corrections, and nonlinear δN observables at a fraction of the cost of full numerical relativity.
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Constant Scaling Fails for Global Monopole Networks
Global monopole networks exhibit logarithmic growth in the number-density parameter ξ rather than constant scaling, with fractional response γ ≈ 0.5 for blue-tilted initial spectra.
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Self-Tracking Solutions for Asymptotic Scalar Fields
The self-perturbations of a scalar field on an exponential potential can act as an effective radiation background, producing a self-tracking solution with the familiar radiation tracker fixed point.
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Domain walls through different cosmologies
Domain-wall network area scales as S ≈ 2ξV/τ with ξ≈1.2 across cosmologies from dust to near-Minkowski, so the particle horizon—not H⁻¹—sets the correlation length and GW peak.
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Fixing IR tail of gravitational waves from domain walls
Per-mode time averaging after source shutdown removes nonphysical IR wiggles in simulated GW spectra from domain walls; PRS scaling yields incorrect spectra even with rescaled sources.
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CosmoLattice 2.0
CosmoLattice v2.0 extends lattice cosmology simulations with non-minimal scalars, ALP–gauge couplings, defect networks, low-storage RK integrators, optimized GWs, and O(10) GPU speedups.
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TempLat: a versatile C++ engine for lattice field theories
TempLat and ParaFaFT deliver a performance-portable, expression-template lattice engine and arbitrary-dimension parallel FFTs with demonstrated multi-node CPU/GPU scaling and open-source release.
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Gravitational waves from self-resonance during reheating with a quantum-corrected inflaton potential
A Coleman-Weinberg correction that cancels the inflaton's quadratic term at the potential minimum triggers quartic self-resonance and a peaked GW background at 10^8-10^10 Hz; a negative quadratic term instead gives a ...
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Biased Domain Wall Networks and their Gravitational Waves
Population-biased domain wall networks annihilate at T_ann ~ T_s B_s^0.8 and emit a single-broken-power-law gravitational-wave spectrum peaking near twice the Hubble scale.
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Phase Transitions and Gravitational Wave Production at the End of Thermal Inflation
The end of thermal inflation proceeds by nucleating true-vacuum bubbles rather than by global phase mixing, and the resulting gravitational-wave background can reach BBO and DECIGO sensitivities for low flaton mass sc...
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Fermion (non)reheating with a quartic inflaton potential
In the quartic T-model, inflaton decay to fermions is strongly suppressed by Pauli blocking and parametric resonance, so fermion-only reheating is effectively impossible unless y ≳ 0.2 or a scalar channel is added.
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The art of simulating the early Universe. Part III: Scalar-Gauge-Fluid Dynamics
Detailed continuum-to-lattice schemes are given for perfect/imperfect fluids alone or coupled to scalars/gauges in FLRW, enabling self-consistent CosmoLattice simulations of early-Universe plasma dynamics and GWs.
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Comparative study of the strong backreaction regime in axion inflation: the effect of the potential
In lattice simulations of axion inflation, the strong-backreaction stage that lengthens inflation occurs for all seven tested potentials, but its duration varies strongly with the potential.
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