Cosmic Stability of Dark Matter from Pauli Blocking

Brian Batell; Wen Yin

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Cosmic Stability of Dark Matter from Pauli Blocking

Brian Batell, Wen Yin

High Energy Physics - Phenomenology · Submitted 24 Jun 2024

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim We analyze the stability of the DM condensate against decays, scatterings (i.e., evaporation), and parametric resonance, delineating the viable parameter regions in which DM is cosmologically stable.

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What the abstract itself states, as probabilities: claims first 0.12 · states limitation 0.28 · human participants 0.01 · controlled comparison 0.13 · randomized assignment 0.01 · states quantitative result 0.07 · compares with prior results 0.35 · mentions code or data availability 0.02.

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Why does dark matter (DM) live longer than the age of the Universe? Here we study a novel sub-eV scalar DM candidate whose stability is due to the Pauli exclusion of its fermionic decay products. We analyze the stability of the DM condensate against decays, scatterings (i.e., evaporation), and parametric resonance, delineating the viable parameter regions in which DM is cosmologically stable. In a minimal scenario in which the scalar DM decays to a pair of new exotic fermions, we find that scattering can populate an interacting thermal dark sector component to energies far above the DM mass. This self-interacting dark radiation may potentially alleviate the Hubble tensions. Furthermore, our scenario can be probed through precise measurements of the halo mass function or the masses of dwarf spheroidal galaxies since scattering prevents the DM from becoming too dense. On the other hand, if the lightest neutrino stabilizes the DM, the cosmic neutrino background (C$\nu$B) can be significantly altered from the $\Lambda$CDM prediction and thus be probed in the future by C$\nu$B detection experiments.

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What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	Why does dark matter (DM) live longer than the age of the Universe?	background 0.78	0.03	0.02	unclear 0.63
s1	Here we study a novel sub-eV scalar DM candidate whose stability is due to the Pauli exclusion of its fermionic decay products.	contribution 1.00	0.77	0.43	asserted 0.98
s2	We analyze the stability of the DM condensate against decays, scatterings (i.e., evaporation), and parametric resonance, delineating the viable parameter regions in which DM is cosmologically stable.	contribution 0.91	0.94	0.33	asserted 0.98
s3	In a minimal scenario in which the scalar DM decays to a pair of new exotic fermions, we find that scattering can populate an interacting thermal dark sector component to energies far above the DM mass.	result 1.00	0.95	0.09	asserted 1.00
s4	This self-interacting dark radiation may potentially alleviate the Hubble tensions.	interpretation 0.98	0.33	0.08	hedged possibility 1.00
s5	Furthermore, our scenario can be probed through precise measurements of the halo mass function or the masses of dwarf spheroidal galaxies since scattering prevents the DM from becoming too dense.	interpretation 0.61	0.58	0.08	hedged possibility 0.84
s6	On the other hand, if the lightest neutrino stabilizes the DM, the cosmic neutrino background (C$\nu$B) can be significantly altered from the $\Lambda$CDM prediction and thus be probed in the future by C$\nu$B detection experiments.	interpretation 0.57	0.40	0.08	hedged possibility 0.76

What kind of paper the classifier reports this is: theoretical result 1.00 · evidence from proof or derivation 0.85.

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The paper

Original abstract

Why does dark matter (DM) live longer than the age of the Universe? Here we study a novel sub-eV scalar DM candidate whose stability is due to the Pauli exclusion of its fermionic decay products. We analyze the stability of the DM condensate against decays, scatterings (i.e., evaporation), and parametric resonance, delineating the viable parameter regions in which DM is cosmologically stable. In a minimal scenario in which the scalar DM decays to a pair of new exotic fermions, we find that scattering can populate an interacting thermal dark sector component to energies far above the DM mass. This self-interacting dark radiation may potentially alleviate the Hubble tensions. Furthermore, our scenario can be probed through precise measurements of the halo mass function or the masses of dwarf spheroidal galaxies since scattering prevents the DM from becoming too dense. On the other hand, if the lightest neutrino stabilizes the DM, the cosmic neutrino background (C$\nu$B) can be significantly altered from the $\Lambda$CDM prediction and thus be probed in the future by C$\nu$B detection experiments.

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8 arXiv papers cite this in 11 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 8 sentences without a confident label

Cites it as background 3 papers

In this work, we focus on the invisible decays of massive neutrinos, which are also subject to various observational constraints [ref] .

Helicity-changing Decays of Cosmological Relic Neutrinos · Observational Constraints · 0.83
Decaying neutrinos [ref] or the presence of flavor-nonuniversal nonstandard interactions [ref] would need special treatment.] where $V_ν=G_F n_ν/√(2)$, with $n_ν$ being the C$ν$B number density and $G_F$ being the Fermi constant.

Pseudo-Dirac Neutrinos and Relic Neutrino Matter Effect on the High-energy Neutrino Flavor Composition · Pseudo-Dirac Case · 0.88
Degenerate systems with large $μ/T$ have been considered in the context of early universe cosmology [ref] and astrophysics [ref] .

Plasma heating during the chiral plasma instability · Conclusion · 0.89

What it cites · 75 sentences without a confident label

Uses the method or tool of 1 paper

Here we follow the analytical discussion for preheating given in [ref] to quantify and describe the dynamics.

Towards the Theory of Reheating After Inflation · Parametric resonance and DM production · 0.97

Uses data or values from 8 papers

By taking $_̊=ρ_DM ≃(2 meV)^4,$ which is the DM energy density today [ref] , we obtain the following constraint on the DM mass in our scenario: massbound m_≪0.01.

Planck 2018 results. VI. Cosmological parameters · Introduction · 1.00
Here we adopt the bound [ref] (see also [ref] )[This is the case with a generic flavor violation for the $ϕ$ coupling.

Updated constraints on non-standard neutrino interactions from Planck · C$ν$B free-streaming and DM stabilized by neutrino sea · 0.87
Here we adopt the bound [ref] (see also [ref] )[This is the case with a generic flavor violation for the $ϕ$ coupling.

Are cosmological neutrinos free-streaming? · C$ν$B free-streaming and DM stabilized by neutrino sea · 0.87

Compares with 2 papers

In other words, our findings may be considered as a different parameter region of the models of the decaying DM into fermions.] We note that the decaying DM case is close to the bound on the decay width given in [ref] .

Constraints on decaying dark matter from weak lensing and cluster counts · Case without chirality suppression · 0.96
In other words, our findings may be considered as a different parameter region of the models of the decaying DM into fermions.] We note that the decaying DM case is close to the bound on the decay width given in [ref] .

Converting non-relativistic dark matter to radiation · Case without chirality suppression · 0.96

Cites as support 4 papers

Still, the energy density of the $$ condensate dominates over $ρ_ψ$, and $$ is stable [ref] .

On the Theory of Fermionic Preheating · Cosmology and summary · 0.98
Still, the energy density of the $$ condensate dominates over $ρ_ψ$, and $$ is stable [ref] .

Preheating of Fermions · Cosmology and summary · 0.98
Still, the energy density of the $$ condensate dominates over $ρ_ψ$, and $$ is stable [ref] .

Nonequilibrium dynamics of fermions in a spatially homogeneous scalar background field · Cosmology and summary · 0.98

Cites as background 12 papers

The interaction Lagrangian is given as [Neutrino couplings to scalar dark matter have been investigated in various other contexts, see, e.g., Refs. [ref] . ] lagnu L⊃-1/2 y_ij (^c_L)_i (_L)_j+h.c., where $i=1,2,3$ is the index in the mass eigenbasis, e.g., in the normal ordering case, the lightest, heavier, and heaviest neutrinos, respectively.

Distorted Neutrino Oscillations From Ultralight Scalar Dark Matter · DM stabilized by C$ν$B · 1.00
The interaction Lagrangian is given as [Neutrino couplings to scalar dark matter have been investigated in various other contexts, see, e.g., Refs. [ref] . ] lagnu L⊃-1/2 y_ij (^c_L)_i (_L)_j+h.c., where $i=1,2,3$ is the index in the mass eigenbasis, e.g., in the normal ordering case, the lightest, heavier, and heaviest neutrinos, respectively.

Neutrino Oscillations as a Probe of Light Scalar Dark Matter · DM stabilized by C$ν$B · 1.00
The interaction Lagrangian is given as [Neutrino couplings to scalar dark matter have been investigated in various other contexts, see, e.g., Refs. [ref] . ] lagnu L⊃-1/2 y_ij (^c_L)_i (_L)_j+h.c., where $i=1,2,3$ is the index in the mass eigenbasis, e.g., in the normal ordering case, the lightest, heavier, and heaviest neutrinos, respectively.

Fuzzy Dark Matter and Non-Standard Neutrino Interactions · DM stabilized by C$ν$B · 1.00

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