Relativistic<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mo stretchy="false">⟨</mml:mo><mml:mi>σ</mml:mi><mml:msub><mml:mrow><mml:mi mathvariant="bold-italic">v</mml:mi></mml:mrow><mml:mrow><mml:mtext mathvariant="bold">rel</mml:mtext></mml:mrow></mml:msub><mml:mo stretchy="false">⟩</mml:mo></mml:mrow></mml:math>in the calculation of relics abundances: A closer look

Cannoni, M.

doi:10.1103/physrevd.89.103533

Cited by 50 publications

(51 citation statements)

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“…In this simple setup the scattering rate s should be s = nσ, where it is taken into account that the relative velocity between particles is close to the speed of light (a calculation using Eq. (52) of [34] gives v rel ≈ 0.98 for our setup), and n is the particle density. From Fig.…”

Section: Elastic Box Testmentioning

confidence: 99%

Particle production and equilibrium properties within a new hadron transport approach for heavy-ion collisions

et al. 2016

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The microscopic description of heavy-ion reactions at low beam energies is achieved within hadronic transport approaches. In this article a new approach SMASH (Simulating Many Accelerated Strongly-interacting Hadrons) is introduced and applied to study the production of non-strange particles in heavy-ion reactions at E kin = 0.4 − 2A GeV. First, the model is described including details about the collision criterion, the initial conditions and the resonance formation and decays. To validate the approach, equilibrium properties such as detailed balance are presented and the results are compared to experimental data for elementary cross sections. Finally results for pion and proton production in C+C and Au+Au collisions is confronted with HADES and FOPI data. Predictions for particle production in π + A collisions are made.

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Section: Elastic Box Testmentioning

confidence: 99%

Particle production and equilibrium properties within a new hadron transport approach for heavy-ion collisions

et al. 2016

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“…is evaluated at T = m χ , with g * defined similarly to (123), but with (T i /T ) 4 instead of (T i /T ) 3 , such that the energy density is ρ = (π 2 /30)g * T 4 . The cross section is thermally averaged, and the v appearing there is usually considered to be the relative velocity between the annihilating particles, but there is some subtlety in this identification that becomes relevant when the annihilations are relativistic [111], which is not the case here. Since the particles are highly nonrelativistic for thermal freezeout, it is a good approximation to use Maxwell-Boltzmann statistics so that…”

Section: B Thermal Freezeoutmentioning

confidence: 99%

TASI Lectures on Early Universe Cosmology: Inflation, Baryogenesis and Dark Matter

Cline¹

2019

Proceedings of Theoretical Advanced Study Institute Summer School 2018 "Theory in an Era of Data" — PoS(TASI2018)

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These lectures, presented at TASI 2018, provide a concise introduction to inflation, baryogenesis, and aspects of dark matter not covered by the other lectures. The emphasis for inflation is an intuitive understanding and techniques for constraining inflationary models. For baryogenesis we focus on two examples, leptogenesis and electroweak baryogenesis, with attention to singlet-assisted two-step phase transitions. Concerning dark matter, we review different classes of models distinguished by their mechanisms for obtaining the observed relic density, including thermal freeze-out, asymmetric dark matter, freeze-in, SIMP dark matter, the misalignment mechanism for ultralight scalars and axions, and production of primordial black holes during inflation. Problem sets are provided.arXiv:1807.08749v4 [hep-ph]

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“…(A8). Thus, taking into account the relation between the average velocity and temperature [41,42], the velocity-averaged cross section is σv conv = σ conv v = σ conv · 2/ √ πx. Finally, we arrive at the following expression…”

Section: A Boltzmann Equationsmentioning

confidence: 99%

Dark matter from CP symmetry of order 4: evolution in the asymmetric regime

Иванов

Laletin

2019

J. Cosmol. Astropart. Phys.

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Multi-Higgs models equipped with global symmetries produce scalar dark matter (DM) candidates stabilized by the unbroken symmetry. It is remarkable that a conserved CP symmetry can also stabilize DM candidates, provided it is a CP symmetry of order higher than two. CP4 3HDM, the three-Higgs-doublet model with CP symmetry of order 4, is the simplest example of this kind. It contains two mass-degenerate scalar DM candidates ϕ andφ, each of them being a CP4 eigenstate and, therefore, its own antiparticle. A novel phenomenological feature of this model is the presence of ϕϕ ↔φφ conversion process, which conserves CP . It offers a rare example of DM models in which self-interaction in the dark sector can significantly affect cosmological and astrophysical observables. Here, we explore the thermal evolution of these DM species in the asymmetric regime. We assume that a mechanism external to CP4 3HDM produces an initial imbalance of the densities of ϕ andφ. As the Universe cools down, we track the evolution of the asymmetry through different stages, and determine how the final asymmetry depends on the interplay between the conversion and annihilation ϕφ → SM and on the initial conditions. We begin with the analytic treatment of Boltzmann equations, present a detailed qualitative description of the process, and then corroborate it with numerical results obtained using a dedicated computer code. Finally, we check if the model can produce an observable indirect detection signal. *

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Relativistic⟨σvrel⟩in the calculation of relics abundances: A closer look

Cited by 50 publications

References 10 publications

Particle production and equilibrium properties within a new hadron transport approach for heavy-ion collisions

Particle production and equilibrium properties within a new hadron transport approach for heavy-ion collisions

TASI Lectures on Early Universe Cosmology: Inflation, Baryogenesis and Dark Matter

Dark matter from CP symmetry of order 4: evolution in the asymmetric regime

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