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Constraining decaying dark matter with neutron stars
Solar and Stellar Astrophysics · Submitted 24 Mar 2014
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find that in the range of uncertainties intrinsic to such a scenario, masses $(m_{\chi}/ \rm TeV) \gtrsim 9 \times 10^{-4}$ or $(m_{\chi}/ \rm TeV) \gtrsim 5 \times 10^{-2}$ and lifetimes ${\tau_{\chi}}\lesssim 10^{55}$ s and ${\tau_{\chi}}\lesssim 10^{53}$ s can be excluded in the bosonic or fermionic decay cases, respectively, in an optimistic estimate, while more conservatively, it decreases $\tau_{\chi}$ by a factor $\gtrsim10^{20}$.
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The abstract, sentence by sentence
The amount of decaying dark matter, accumulated in the central regions in neutron stars together with the energy deposition rate from decays, may set a limit on the neutron star survival rate against transitions to more compact objects provided nuclear matter is not the ultimate stable state of matter and that dark matter indeed is unstable. More generally, this limit sets constraints on the dark matter particle decay time, $\tau_{\chi}$. We find that in the range of uncertainties intrinsic to such a scenario, masses $(m_{\chi}/ \rm TeV) \gtrsim 9 \times 10^{-4}$ or $(m_{\chi}/ \rm TeV) \gtrsim 5 \times 10^{-2}$ and lifetimes ${\tau_{\chi}}\lesssim 10^{55}$ s and ${\tau_{\chi}}\lesssim 10^{53}$ s can be excluded in the bosonic or fermionic decay cases, respectively, in an optimistic estimate, while more conservatively, it decreases $\tau_{\chi}$ by a factor $\gtrsim10^{20}$. We discuss the validity under which these results may improve with other current constraints.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The amount of decaying dark matter, accumulated in the central regions in neutron stars together with the energy deposition rate from decays, may set a limit on the neutron star survival rate against transitions to more compact objects provided nuclear matter is not the ultimate stable state of matter and that dark matter indeed is unstable. | background 0.59 | 0.15 | 0.30 | hedged possibility 1.00 |
| s1 | More generally, this limit sets constraints on the dark matter particle decay time, $\tau_{\chi}$. | interpretation 0.81 | 0.29 | 0.27 | asserted 0.97 |
| s2 | We find that in the range of uncertainties intrinsic to such a scenario, masses $(m_{\chi}/ \rm TeV) \gtrsim 9 \times 10^{-4}$ or $(m_{\chi}/ \rm TeV) \gtrsim 5 \times 10^{-2}$ and lifetimes ${\tau_{\chi}}\lesssim 10^{55}$ s and ${\tau_{\chi}}\lesssim 10^{53}$ s can be excluded in the bosonic or fermionic decay cases, respectively, in an optimistic estimate, while more conservatively, it decreases $\tau_{\chi}$ by a factor $\gtrsim10^{20}$. | result 1.00 | 0.95 | 0.85 | asserted 0.99 |
| s3 | We discuss the validity under which these results may improve with other current constraints. | interpretation 0.41 | 0.54 | 0.03 | hedged possibility 0.52 |
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The paper
Original abstract
The amount of decaying dark matter, accumulated in the central regions in neutron stars together with the energy deposition rate from decays, may set a limit on the neutron star survival rate against transitions to more compact objects provided nuclear matter is not the ultimate stable state of matter and that dark matter indeed is unstable. More generally, this limit sets constraints on the dark matter particle decay time, $\tau_{\chi}$. We find that in the range of uncertainties intrinsic to such a scenario, masses $(m_{\chi}/ \rm TeV) \gtrsim 9 \times 10^{-4}$ or $(m_{\chi}/ \rm TeV) \gtrsim 5 \times 10^{-2}$ and lifetimes ${\tau_{\chi}}\lesssim 10^{55}$ s and ${\tau_{\chi}}\lesssim 10^{53}$ s can be excluded in the bosonic or fermionic decay cases, respectively, in an optimistic estimate, while more conservatively, it decreases $\tau_{\chi}$ by a factor $\gtrsim10^{20}$. We discuss the validity under which these results may improve with other current constraints.
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References
How the literature uses it
25 arXiv papers cite this in 27 sentences
Papers citing it · 11 sentences without a confident label
Compares with it 1 paper
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Note also that the cross-sections we consider are smaller than those relevant for other stellar probes of DM (e.g. main-sequence [ref] , astroseismic [ref] , cooling [ref] , and pulsar phase [ref] constraints).
Dark matter ignition of type Ia supernovae · Introduction · 0.92
Cites it as support 1 paper
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DM population in the NS (after the supernova explosion) should not be negligible since the massive progenitor $8M_⊙≲M_progenitor≲15 M_⊙$ can be efficient in the DM accretion process [ref] .
Diffusion of dark matter in a hot and dense nuclear environment · Dark Matter model and cross sections · 0.99
Cites it as background 14 papers
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In the search for this ellusive substance a number of studies have considered DM capture in celestial object ranging from solar system objects such as the Earth, Sun [ref] , Jupiter [ref] , and Uranus [ref] , to Brown Dwarfs [ref] , White Dwarfs [ref] , Neutron Stars [ref] , and other stars [ref] , as well as recently Exoplanets [ref] .
Dark Matter (H)eats Young Planets · Introduction · 0.96
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There has been growing interest in signals of DM capture in compact stars [ref] .
Relativistic capture of dark matter by electrons in neutron stars · Introduction · 0.97
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In particular, the production of sterile neutrinos $ν_s$, through collisions with standard matter or flavor oscillations has important implications in particle physics [ref] .
Production of unstable heavy neutrinos in proto-neutron stars · Introduction · 0.89
What it cites · 11 sentences without a confident label
Builds on 4 papers
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In previous works we have considered the effect of a self-annihilating DM particle on the internal NS dynamics [ref] but here we will focus on the possibility that the only process depleting DM is decay.
Dark Matter Seeding in Neutron Stars · Introduction · 0.87
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In previous works we have considered the effect of a self-annihilating DM particle on the internal NS dynamics [ref] but here we will focus on the possibility that the only process depleting DM is decay.
Dark matter seeding and the kinematics and rotation of neutron stars · Introduction · 0.87
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In previous works we have considered the effect of a self-annihilating DM particle on the internal NS dynamics [ref] but here we will focus on the possibility that the only process depleting DM is decay.
Strangelets and the TeV-PeV cosmic-ray anisotropies · Introduction · 0.87
Uses data or values from 3 papers
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Using the photon spectrum $dN_γ/dE$ from [ref] , we estimate the injection rate per unit volume and unit energy from the contribution of each channel with corresponding decay rate $Γ_i$ at stellar radial location $r$ as $Q(E, r)=n_χ(r) ∑_i Γ_i dN^i_γ/dE$.
Gamma Ray Spectra from Dark Matter Annihilation and Decay · Introduction · 0.87
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Linked to this argument, we have considered an average-sized massive NS, however, variations in mass and radius in current surveys are of the order of $30%$ [ref] and the capture rate would be affected in a similar fashion, resulting in a moderately reduced capture efficiency.
The Neutron Star Mass Distribution · Introduction · 0.87
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Compilation of the latest results in direct detection searches [ref] allows analysis to set limits at a level of $σ_χn ≃10^-44 cm^2$ in the $m_χ∼(10-10^4)$ GeV range.
Snowmass CF1 Summary: WIMP Dark Matter Direct Detection · Introduction · 0.89
Compares with 1 paper
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Our optimistic limits are considerably stronger than earlier results, including the CMB constraints [ref] .
Constraining dark matter late-time energy injection: decays and p-wave annihilations · Introduction · 1.00
Cites as background 2 papers
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Some attemps to computationally model progression of seeds of quark matter inside NSs have been recently performed in [ref] .
Three-dimensional hydrodynamic simulations of the combustion of a neutron star into a quark star · Introduction · 0.82
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It is usually assumed that the decay daughter particles are (nearly) massless although a more generic situation with arbitrary non-zero masses, $m_D$, may also occur [ref] .
Formulation and constraints on decaying dark matter with finite mass daughter particles · Introduction · 0.80
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