Supersymmetric Dark Matter

G. Jungman; K. Griest; M. Kamionkowski

REVIEW

Supersymmetric Dark Matter

G. Jungman, M. Kamionkowski, K. Griest

High Energy Physics - Phenomenology · Submitted 22 Jun 1995 · 14 references

Pith's verdict: A canonical, well-organized synthesis of neutralino dark matter calculations; the stress-test's worry about correlated halo systematics is plausible but unverified from the text I can see, which is only the table of contents.

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arXiv IDhep-ph/9506380 (version 1)

Pith IDJF4WFMIX, Pith's permanent record of this paper and its review

CitationG. Jungman, K. Griest, M. Kamionkowski. "Supersymmetric Dark Matter." arXiv:hep-ph/9506380 (1995). https://pith.science/paper/JF4WFMIX

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Editor's note

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Bottom line: this is the reference synthesis for neutralino dark matter, and it earns that role. It is not a discovery paper and doesn't pretend to be — the abstract says plainly that it reviews the MSSM and the detection prospects (abstract:s5) and that its job is to isolate the particle-physics, nuclear-physics, and astrophysical uncertainties at each step (abstract:s7). What's genuinely useful is the decomposition: relic abundance in section 3, annihilation channels one by one in section 6, axial versus scalar scattering split in 7.2 and 7.3, capture separated from annihilation in 9.3 and 9.4, and a worked MSSM scan in section 11. That structure is the contribution, and it's the reason people cite this paper rather than the individual calculations it draws on. The Neutdriver guide in Appendix B is a real bonus for 1995 — explicit formulas plus documented code is better reproducibility than most of the field managed then or now. Credit where due: the paper is honest about what it inherits and where the numbers come from, and the sample scan varies parameters over ranges rather than tuning them to a target, so I don't see circularity either. On the stress-test: the point that rho_0 and the Maxwellian f(v) are a correlated systematic rather than three independent error bars is a fair physics point, and the observation that v_min samples the high-velocity tail for heavy WIMPs and low thresholds is correct and is exactly where the ansatz is weakest. But the note itself concedes it can't see how sections 2.4 and 8.1 handle the tail, and a review that devotes a section to Galactic dark-matter distribution is likely to say so. I'd treat this as a question to check against the body, not a flaw established. My own caveat is the same one the reader flagged: the text I have is the title page and TOC, so I can't verify a single equation or number. That limits my confidence, not the paper's quality. Who should read it: anyone computing a neutralino rate, anyone converting a direct-detection limit into a SUSY constraint, and any student entering the subfield. It deserves a serious referee, though for a Physics Reports review the referee's job is mostly checking that the uncertainty discussion is as careful as claimed — which is precisely where the stress-test points.

Referee report

Significance

If the programme is carried out as advertised, this is a reference work rather than a single result: it would let every direct-detection and neutrino-telescope limit be read as a constraint on supersymmetric parameter space within one consistent calculational framework. Three things deserve explicit credit. First, the decomposition into independently checkable pieces (annihilation channels in §6, spin-dependent and scalar scattering separated in §7.2 and §7.3, capture separated from annihilation in §9.3 and §9.4) is the right architecture for a review whose selling point is error bookkeeping. Second, §9.6 promises a model-independent analysis, which is exactly the right response to the fact that the underlying particle model is unknown. Third, Appendix B's user's guide to the numerical code is a genuine reproducibility asset, and the event rates and exclusion contours of §11 are falsifiable predictions in the ordinary sense. The paper is also candid about the nuclear-physics inputs, which are the least tractable part of the chain.

Major objections (2)

[§2.4, §8.1, §9.4] The abstract's central methodological claim (abstract:s7) is that the particle-physics, nuclear-physics, and astrophysical uncertainties are isolated at each step. The astrophysical factor is the one place where that isolation is not automatic, and the manuscript should say so explicitly rather than leaving it to the reader. The local density rho_0 and the halo velocity distribution f(v) enter the direct-detection rate of §8.1 and the capture rate of §9.4 with different velocity weightings: the direct rate is an integral from a recoil-dependent minimum velocity v_min, so for heavy neutralinos and low thresholds it samples the high-velocity tail of f(v), whereas capture in the Sun is weighted against the escape velocity and the solar gravitational well. A change in the shape of the tail can therefore move the two rates by different factors even when rho_0 is held fixed, which means the direct-versus-indirect comparison of §9.7 is not a comparison at fixed astrophysics. I would ask the authors to state this correlation explicitly in §2.4 or §8.1 and, if feasible, to add a short table showing how the §11 rates and contours respond to a factor-of-two change in rho_0 and to a non-Maxwellian tail. This is a request to make an existing systematic explicit, not a claim that the calculations are wrong.
[§11.2–§11.5] In the sample MSSM analysis the supersymmetric parameters are scanned while rho_0 = 0.3 GeV/cm^3 and a Maxwellian f(v) are held fixed, so the exclusion contours presented in §11.5 mix a particle-physics scan with a fixed astrophysical prior. Because the direct-detection rate scales as rho_0 times the cross section, the contours shift systematically with the assumed local density, and a reader who wants to re-derive limits under a different halo normalization has no stated prescription for doing so. The manuscript should give that prescription in one or two sentences in §11.2 or §11.5 — for example, that the contours scale as rho_0 sigma and can be rescaled by the ratio of assumed densities — and should flag which of the §11 conclusions are sensitive to the choice and which are not.

Minor objections (7)

[Table of contents, §7.4] The entry reads 'General Axial-Vector, Vector, and Scalar Interaction s'; the stray space in 'Interactions' should be corrected.
[Table of contents, §8.2] The page number for 'Detectors' is printed as '1 30'; this should be '130'.
[Table of contents, §9] The heading reads 'Energetic Neutrinos from WIMP Annihilation in the Sun and /or Earth'; the spacing around the slash should be regularized to 'and/or'.
[Abstract] The abstract uses 'WIMPS' in one sentence and 'WIMP' elsewhere; the acronym should be capitalized consistently as 'WIMPs'. The phrase 'a vast experimental effort being surmounted' also reads oddly, since the effort is being mounted or undertaken rather than surmounted.
[Abstract, first sentence] The statement that 'most of the mass in the Universe and most of the mass in the Galactic halo is dark' is loose for the Universe as a whole, where the dark component is constrained by big-bang nucleosynthesis and the microwave background rather than by the same arguments that apply to the halo. A qualifier distinguishing the two cases would be more accurate.
[Appendix B] The user's guide to the numerical code is a valuable part of the review. The manuscript should state plainly whether the code is publicly available, and if so from where, since a user's guide without an availability statement limits the reproducibility benefit.
[§12.1] The subsection title 'The Rise and Fall of Heavy-Neutrino Dark Matter' is more journalistic than the rest of the headings; a descriptive title would fit the surrounding sections better.

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The paper

The paper claims

The neutralino of minimal supersymmetry is a well-motivated dark matter candidate whose relic abundance and direct and indirect detection rates can be computed with particle, nuclear, and astrophysical uncertainties isolated at each step.

The reading

The universe appears to contain far more mass than the stars and gas we can see. One long-standing explanation is that the missing mass is a new kind of particle that interacts weakly with ordinary matter and rarely annihilates or decays. Supersymmetry, a proposed extension of the Standard Model of particle physics, supplies a natural candidate: the neutralino, the lightest of the new electrically neutral particles it predicts. This paper is a long review of that idea. It does four things. First, it summarizes the evidence that dark matter exists and describes how much of it is plausibly ordinary matter. Second, it explains how to compute how many neutralinos would survive from the early universe, a number set by when they stopped annihilating each other. Third, it works out how a neutralino would scatter off a nucleus in a laboratory detector, separating the spin-dependent and spin-independent pieces. Fourth, it works out how neutralinos captured by the Sun or the Earth would annihilate and produce neutrinos that a telescope could see. Throughout, the authors separate the uncertainties into three buckets: particle physics (which supersymmetric model and which parameters), nuclear physics (how quarks and gluons inside a nucleon couple to the neutralino), and astrophysics (how much dark matter sits near the Sun and how fast it moves). The point is to let an experimental result be read as a constraint on particle theory rather than as a single number.

Extended reading notes

Core claim

The neutralino of the minimal supersymmetric Standard Model is a well-motivated WIMP dark matter candidate, and its cosmological relic abundance together with its direct-detection and neutrino-indirect-detection event rates can be computed with the particle-physics, nuclear-physics, and astrophysical uncertainties isolated at each step (abstract s5 and s7; sections 3, 7, 8, 9). If correct, every dark matter search can be read as a constraint on supersymmetric models within one consistent framework.

Load-bearing premise

Every event rate in sections 8 and 9 scales with the local halo dark matter density and the assumed velocity distribution, taken as roughly 0.3 GeV/cm^3 and Maxwellian (section 2.4, section 8.1). If the local density is a factor of two lower, or the velocity distribution has a significant non-Maxwellian component, all quoted rates and all derived exclusion limits shift accordingly, and the direct-versus-indirect comparison in section 9.7 changes.

Original abstract

There is almost universal agreement among astronomers that most of the mass in the Universe and most of the mass in the Galactic halo is dark. Many lines of reasoning suggest that the dark matter consists of some new, as yet undiscovered, weakly-interacting massive particle (WIMP). There is now a vast experimental effort being surmounted to detect WIMPS in the halo. The most promising techniques involve direct detection in low-background laboratory detectors and indirect detection through observation of energetic neutrinos from annihilation of WIMPs that have accumulated in the Sun and/or the Earth. Of the many WIMP candidates, perhaps the best motivated and certainly the most theoretically developed is the neutralino, the lightest superpartner in many supersymmetric theories. We review the minimal supersymmetric extension of the Standard Model and discuss prospects for detection of neutralino dark matter. We review in detail how to calculate the cosmological abundance of the neutralino and the event rates for both direct- and indirect-detection schemes, and we discuss astrophysical and laboratory constraints on supersymmetric models. We isolate and clarify the uncertainties from particle physics, nuclear physics, and astrophysics that enter at each step in the calculation. We briefly review other related dark-matter candidates and detection techniques.

The compiled record

The paper's own sentences, arranged, kept beside the review and separate from it. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 6,934 input tokens, $0.0003 reported.

What the abstract itself states, as probabilities: claims first 0.02 · states limitation 0.36 · human participants 0.02 · controlled comparison 0.02 · randomized assignment 0.01 · states quantitative result 0.04 · compares with prior results 0.08 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; show every role.

There is almost universal agreement among astronomers that most of the mass in the Universe and most of the mass in the Galactic halo is dark. Many lines of reasoning suggest that the dark matter consists of some new, as yet undiscovered, weakly-interacting massive particle (WIMP). There is now a vast experimental effort being surmounted to detect WIMPS in the halo. The most promising techniques involve direct detection in low-background laboratory detectors and indirect detection through observation of energetic neutrinos from annihilation of WIMPs that have accumulated in the Sun and/or the Earth. Of the many WIMP candidates, perhaps the best motivated and certainly the most theoretically developed is the neutralino, the lightest superpartner in many supersymmetric theories. We review the minimal supersymmetric extension of the Standard Model and discuss prospects for detection of neutralino dark matter. We review in detail how to calculate the cosmological abundance of the neutralino and the event rates for both direct- and indirect-detection schemes, and we discuss astrophysical and laboratory constraints on supersymmetric models. We isolate and clarify the uncertainties from particle physics, nuclear physics, and astrophysics that enter at each step in the calculation. We briefly review other related dark-matter candidates and detection techniques.

background contribution method result interpretation main claim

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	There is almost universal agreement among astronomers that most of the mass in the Universe and most of the mass in the Galactic halo is dark.	background 1.00	0.03	0.04	asserted 0.93
s1	Many lines of reasoning suggest that the dark matter consists of some new, as yet undiscovered, weakly-interacting massive particle (WIMP).	background 0.99	0.04	0.06	hedged possibility 0.99
s2	There is now a vast experimental effort being surmounted to detect WIMPS in the halo.	background 1.00	0.05	0.03	asserted 1.00
s3	The most promising techniques involve direct detection in low-background laboratory detectors and indirect detection through observation of energetic neutrinos from annihilation of WIMPs that have accumulated in the Sun and/or the Earth.	background 0.86	0.05	0.04	asserted 0.89
s4	Of the many WIMP candidates, perhaps the best motivated and certainly the most theoretically developed is the neutralino, the lightest superpartner in many supersymmetric theories.	background 0.96	0.06	0.08	hedged possibility 0.64
s5	We review the minimal supersymmetric extension of the Standard Model and discuss prospects for detection of neutralino dark matter.	contribution 0.99	0.58	0.08	unclear 0.51
s6	We review in detail how to calculate the cosmological abundance of the neutralino and the event rates for both direct- and indirect-detection schemes, and we discuss astrophysical and laboratory constraints on supersymmetric models.	contribution 0.68	0.59	0.08	asserted 0.77
s7	We isolate and clarify the uncertainties from particle physics, nuclear physics, and astrophysics that enter at each step in the calculation.	contribution 0.80	0.83	0.05	asserted 0.85
s8	We briefly review other related dark-matter candidates and detection techniques.	contribution 0.86	0.59	0.03	unclear 0.54

What kind of paper the classifier reports this is: review 1.00 · evidence from literature 0.86.

What was examined, and what was not

sources read

arXiv listing abstract v1

not examined

full text
figures and tables
references and citing sentences
relations to other papers

levels run

P abstract

not run

S sections
T body sentences
C citations
R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

References

Works cited (14)

[1]

Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2

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[2]

Dark Matter in the Universe . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 14 2.1. Inventory of Dark Matter . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 14 2.2. Theoretical arguments . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 20 2.3. Baryonic Content of the Universe . . . . . . . . . . . . . . . . . . . . . ....

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[3]

Cosmological Abundance of a WIMP . . . . . . . . . . . . . . . . . . . . . . . . . . . 32 3.1. Simple Estimates . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 34 3.2. Why WIMPs? . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 38 3.3. Standard Calculation of Relic Abundance . . . . . . . . . . . . . . . . . . . . ...

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[4]

Supersymmetric Models . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 46 4.1. Motivation, Goals, and Some Formalities . . . . . . . . . . . . . . . . . . . . . . . 46 4.2. Minimal Supersymmetric Standard Model . . . . . . . . . . . . . . . . . . . . . . . 52 4.3. SUSY-GUT and Supergravity Models . . . . . . . . . . . . . . . . . . . . . . . . . 60

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[5]

Laboratory Constraints . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 62 5.1. Remarks . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 62 5.2. Constraints on the Higgs Sector . . . . . . . . . . . . . . . . . . . . . . . . . . . 62 5.3. Constraints on the Chargino/Neutralino Sector . . . . . . . . . . . . . . . ...

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[6]

Neutralino Annihilation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 72 6.1. Remarks . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 72 6.2. Weak–Gauge-Boson Final States . . . . . . . . . . . . . . . . . . . . . . . . . . . 74 6.3. Final States Containing Higgs Bosons . . . . . . . . . . . . . . . . . . . . . ...

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[7]

Elastic-Scattering Cross Sections . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 96 7.1. The Basic Ingredients . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 96 7.2. Axial-Vector (spin) Interaction . . . . . . . . . . . . . . . . . . . . . . . . . . . . 98 7.3. Scalar Interaction . . . . . . . . . . . . . . . . . . . . . . . . ...

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[8]

Direct Detection of Neutralinos . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 120 8.1. Theory . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 120 8.2. Detectors . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1 30 8.3. Inelastic-Scattering Techniques . . . . . . . . . . . . . . . . . . . . ...

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[9]

Energetic Neutrinos from WIMP Annihilation in the Sun and /or Earth . . . . . . . . . . . . 136 9.1. General Description . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 136 9.2. Detectors and Atmospheric-Neutrino Background . . . . . . . . . . . . . . . . . . . 142 9.3. Annihilation Rate in the Sun and Earth . . . . . . . . . . . . . . . ....

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[10]

Cosmic Rays from WIMP Annihilation in the Halo . . . . . . . . . . . . . . . . . . . . 178 10.1. Cosmic-Ray Antiprotons . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 180 10.2. Cosmic-Ray Positrons . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 182 10.3. Cosmic Gamma Rays . . . . . . . . . . . . . . . . . . . . . . . . . . . . ...

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[11]

Sample Analysis of the MSSM . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 188 11.1. Orientation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 188 11.2. SUSY Parameter Space . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 190 11.3. Relic Density . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . ...

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[12]

Other Particle Dark-Matter Candidates . . . . . . . . . . . . . . . . . . . . . . . . . 208 12.1. The Rise and Fall of Heavy-Neutrino Dark Matter . . . . . . . . . . . . . . . . . . . 210 12.2. Sneutrinos . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 214 12.3. Other Supersymmetric Dark-Matter Candidates . . . . . . . . . . . . . ...

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[13]

Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 216 13.1. Summary of Calculations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 218 13.2. Central Results . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 220 13.3. Concluding Remarks . . . . . . . . . . . . . . . . . . . . . . . . . . . ...

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[14]

Acknowledgments . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 224 Appendix A. Construction of the MSSM . . . . . . . . . . . . . . . . . . . . . . . . . . 224 A.1. Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 224 A.2. Superﬁeld Formalism . . . . . . . . . . . . . . . . . . . . . . . . . . . . ....

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hep-th 2009-06 conditional novelty 7.0 of 10

Quark and lepton flavor hierarchies in F-theory GUTs require a single E8 enhancement point, which simultaneously fixes the messenger sector to 10 plus 10-bar of SU(5) and eliminates all TeV-scale dark matter candidate...
Bosonic super-WIMPs as keV-scale dark matter
hep-ph 2008-07 accept novelty 7.0 of 10

KeV-scale bosonic dark matter can be probed by absorption in direct-detection experiments, with the vector (dark photon) model offering sensitivity beyond existing indirect constraints.
Thermal decoupling of WIMPs from first principles
hep-ph 2006-12 conditional novelty 7.0 of 10

A first-principles analytic solution of the WIMP kinetic decoupling equation yields the decoupling temperature, and hence the small-scale cutoff of the matter power spectrum, for any WIMP candidate given its scatterin...
Largest temperature of the radiation era and its cosmological implications
hep-ph 2000-05 accept novelty 7.0 of 10

If the reheat temperature was as low as 0.7 MeV, WIMPs, neutrinos, and axions can be far heavier or more weakly coupled than standard cosmology allows, and the usual dark-matter mass bounds dissolve.
Vanilla Scotogenic Model at the future Muon Collider
hep-ph 2026-09 conditional novelty 6.5 of 10

The Vanilla Scotogenic Model with enhanced second-generation Yukawa couplings lowers the leptogenesis scale to ~1 TeV and can be probed via long-lived charged scalar disappearing tracks at future muon colliders.
Light top-flavoured dark matter in dark SMEFT: one-loop matching and phenomenology
hep-ph 2026-10 accept novelty 6.0 of 10

In dark SMEFT, one-loop matching of top-flavoured dark matter shows that only tree-level operators can explain the Belle II B+→K+ννbar excess with O(1) couplings at Λ=1 TeV, with B0→K*0+inv giving the strongest constraint.
Solar Neutrino Signals and Capture-Annihilation Equilibrium of SU(5) Neutralino Dark Matter
hep-ph 2026-10 conditional novelty 6.0 of 10

For subdominant neutralinos, the solar annihilation signal interpolates between linear and quadratic abundance scaling, so linear rescaling overestimates the signal in many SU(5) models.
One-loop mixing matrix of the N=1 SYM Supercurrent operator upon renormalization on the Lattice using stout-smeared Links
hep-lat 2026-10 accept novelty 6.0 of 10

The one-loop mixing matrix of the supercurrent operator is calculated analytically for stout-smeared links and three Symanzik-improved gauge actions.
Is the Light Neutralino Dark Matter Still Viable in the MSSM After the LZ-2024 Results?
hep-ph 2026-10 conditional novelty 6.0 of 10

Radiative corrections, conservative hadronic inputs, and a likelihood-based recast of LZ-2024 close the h- and Z-resonant annihilation windows for light Bino-like neutralino dark matter in the MSSM.
Environment-Dependent Annihilation of Axion-Coupled Higgsino Dark Matter
hep-ph 2026-10 conditional novelty 6.0 of 10

A subthreshold axion mediator plus a change in the annihilating Higgsino population makes annihilation environment-dependent, decoupling the solar-neutrino bound from Galactic and terrestrial signals for a few-percent...
Anomalous Dimensions, Matching, and Phenomenology of Dirac Fermionic Dark Matter Effective Interactions
hep-ph 2026-09 accept novelty 6.0 of 10

This paper computes the complete renormalization-group evolution and matching for Dirac fermionic dark matter effective operators and derives constraints from precision measurements.
Connecting Vector-like Muons, pNGB Dark Matter and Electroweak Phase Transition through Collider and Gravitational Wave
hep-ph 2026-09 conditional novelty 6.0 of 10

A model with pNGB dark matter and a vector-like muon can simultaneously satisfy all current constraints and produce detectable signals at muon colliders and gravitational-wave detectors.
Generalized Chiral $U(1)_{B-L}$ with Inelastic Scalar Dark Matter for the LZ 248 keV Event
hep-ph 2026-09 conditional novelty 6.0 of 10

A generalized chiral $U(1)_{B-L}$ framework with inelastic scalar dark matter can account for the LZ 248 keV event.
Solar Capture Tests of Inelastic Dark Matter after the LZ High-Recoil Event
hep-ph 2026-09 conditional novelty 6.0 of 10

Solar capture and IceCube neutrino limits exclude the thermal Higgsino interpretation of the LZ 248 keV event but leave pseudo-Dirac and neutron-philic spin-dependent inelastic dark matter benchmarks viable.
Strong Constraints on Line Signals from Dark Matter Annihilation in a Nearby Subhalo
hep-ph 2026-09 conditional novelty 6.0 of 10

A 15-year Fermi-LAT search for gamma-ray lines toward a proposed nearby dark matter subhalo finds no significant signal and sets 95% CL cross-section limits stronger than Galactic Center line limits over most of the 1...
Strong Constraints on Higgsino Dark Matter from Solar Capture
hep-ph 2026-09 accept novelty 6.0 of 10

Solar capture and IceCube neutrino limits constrain the Higgsino mass splitting to be greater than 566 keV, excluding a previously proposed explanation of an LZ event.
Taming lepton portal dark matter by a non-invertible selection rule
hep-ph 2026-08 conditional novelty 6.0 of 10

A non-invertible selection rule from Z2 gauging of Z5 enforces one-flavor dominance of lepton portal dark matter couplings while leaving the PMNS matrix unrestricted.
Modelling electroweak interactions at lepton colliders - from the Z pole to the highest energies
hep-ph 2026-08 conditional novelty 6.0 of 10

A thesis that shows how to measure light-quark Z couplings to sub-percent precision at future colliders, revalidates the Equivalent Vector Boson Approximation at TeV energies, and implements Electroweak Parton Distrib...
Probing Sub-GeV Dark Matter with the Migdal Effect at JUNO
hep-ph 2026-08 conditional novelty 6.0 of 10

JUNO's 20 kton liquid scintillator could use annual modulation of Migdal ionization to achieve world-leading sensitivity to spin-dependent sub-GeV dark matter in the 50 MeV to 2 GeV mass range.
Singlet-Doublet fermion origin of dark matter, neutrino mass and inverse first-order electroweak phase transition
hep-ph 2026-08 conditional novelty 6.0 of 10

New singlet and doublet fermions, a scalar singlet, and right-handed neutrinos can simultaneously explain Dirac neutrino masses, dark matter, and a two-step inverse electroweak phase transition with observable gravita...
Fine-tuning in mixed Dark Matter models with Primordial Black Hole relics
astro-ph.CO 2026-08 conditional novelty 6.0 of 10

In mixed dark matter models combining Planck-mass black hole relics, Hawking-evaporated particles, and a WIMP, freeze-in, or axion component, the total abundance's fine-tuning is dominated by the primordial power spec...
Thermal Evolution and Hydrodynamic Filtering of Pseudoscalar Dark Matter
hep-ph 2026-08 conditional novelty 6.0 of 10

Hydrodynamic shock heating in a deflagration phase transition enhances the filtered dark matter abundance by factors of 4.3, 5.8, and 32 for benchmark masses of 1.78, 2.30, and 5.03 TeV.
Unveiling the Vanishing Higgsino-Nucleon Scattering in the MSSM at Next-to-Leading Order
hep-ph 2026-07 conditional novelty 6.0 of 10

Near the stop-top kinematic threshold, next-to-leading-order corrections cancel the leading Higgsino-nucleon scattering amplitude, pushing the spin-independent cross section below the neutrino floor in parts of the MS...
Extreme mass-ratio inspirals into Newtonian Proca stars
gr-qc 2026-07 accept novelty 6.0 of 10

For Newtonian Proca stars, a perturbing object on a circular orbit loses nearly the same energy in the vector ground state as in the scalar boson-star ground state (within ~20%), while the spherical excited Proca stat...
Vortex-reconnection energy bounds in Bose-Einstein-condensed and superfluid dark matter halos
astro-ph.GA 2026-07 conditional novelty 6.0 of 10

Vortex reconnections in BEC/superfluid dark matter halos produce dark-sector heating at a rate that is secular but sub-virial for relaxed non-interacting soliton cores, with the dominant uncertainty being the true vor...
Radiative Neutrino Mass in a Nonholomorphic $T'$ Modular Invariant Model
hep-ph 2026-06 unverdicted novelty 6.0 of 10

A nonholomorphic T' modular model realizes the T4-2-i one-loop topology for radiative Majorana neutrino masses, forbids tree-level seesaws via modular assignments, stabilizes DM with residual Z2, and fits oscillation ...
Light rings, gravitational lensing, and ISCOs of exotic compact objects in Einstein-scalar-Maxwell theories
gr-qc 2026-02 conditional novelty 6.0 of 10

A new family of shell-like, charged, horizonless compact objects is constructed in Einstein-scalar-Maxwell theory, with photon-ring, lensing, and ISCO predictions.
Mixed Freeze-In and Freeze-Out Histories and Dark-Sector Decays in a $\mathbb{Z}_4$ Two-Scalar Model
hep-ph 2026-02 conditional novelty 6.0 of 10

A Z4 two-scalar Higgs-portal dark matter model stays viable under LZ exclusions when one or both scalars are produced via freeze-in, and late dark-sector decays generate SuperWIMP, injection-assisted freeze-out, and s...
Light Dark Matter Search with 7.8 Tonne-Year of Ionization-Only Data in XENONnT
hep-ex 2026-01 conditional novelty 6.0 of 10

An S2-only analysis of 7.83 tonne-years of XENONnT data finds no dark matter excess and sets 90% CL limits, e.g. 6.0e-45 cm^2 for spin-independent scattering at 5 GeV/c^2.
Physical implications of a double right-handed gauge symmetry
hep-ph 2026-01 unverdicted novelty 6.0 of 10

A double right-handed U(1) gauge extension generates the Standard Model fermion mass hierarchy at tree and loop levels and stabilizes a viable scalar singlet dark matter particle consistent with relic density and dire...
BinaryGFH-v2: Improved method to search for gravitational waves from sub-solar-mass, ultra-compact binaries using the Generalized Frequency-Hough Transform
gr-qc 2025-12 conditional novelty 6.0 of 10

BinaryGFH-v2 is a modified GFH method that can search for inspiraling binaries with chirp masses 0.01–0.1 solar masses, validated in Gaussian noise and projected to constrain PBH dark matter.
Ultralight Dark Matter from the Edge of Field Space
hep-ph 2025-11 conditional novelty 6.0 of 10

A scalar with hard field-space boundaries — a 'wallion' — is a viable ultralight dark-matter candidate whose exponentially small, radiatively stable mass and saturated relic density at large misalignment also suppress...
Reviving WIMP dark matter with temperature-dependent couplings
hep-ph 2025-09 unverdicted novelty 6.0 of 10

Temperature-dependent DM couplings mediated by a scalar field's VEV that drops after a first-order phase transition allow sufficient early-universe annihilations for the observed relic density while evading current di...
Amplified capture rate of dark matter in compact binaries and constraints on bosonic dark matter from GW170817
astro-ph.HE 2025-09 conditional novelty 6.0 of 10

Dark matter capture onto neutron stars is amplified by about 4-5 times in circular binaries, tightening cross-section limits from GW170817 and capping the accreted DM fraction near 1e-3.
Novel probes for electron-muon flavor violation from exotic Higgs decays
hep-ph 2025-08 unverdicted novelty 6.0 of 10

Novel multilepton signatures from Higgs decays to a light pseudoscalar decaying to e-mu pairs in type-III 2HDM can set stronger limits on LFV couplings than low-energy experiments.

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How later papers used it

1,269 later papers cite it

Evidence: substantial. 1,257 of the citing papers share no author with it, and 88 of those carry a confident label from Pith's citation classifier.

Pith read 40 of the 1,791 citing sentences, choosing only those whose citation markers point at this paper alone, and wrote the paraphrases from them. The summary, the counts, the evidence level, the links and the quotes come from code; the summary counts the papers listed below. A later paper is listed under a label when Pith's citation classifier gives one of its sentences that label at probability 0.8 or more (0.95 for support), Pith's reading finds that the citing paper itself did it, and a second check confirms the paraphrase against the sentence. This section lists uses only. It does not list criticism or disagreement, so their absence here says nothing about how the paper has been received. Papers that share an author with this one are listed apart, under "By the same authors". A quote is the citing authors' own sentence, shown when their paper's licence is CC BY, CC BY-SA or CC0. JSON

10 later papers by other authors are listed below: 6 used its method or tool and 4 used its data or values.

Uses its method or tool 6 of 55 papers with this label

Employed an exponential (Helm) form factor following this paper to describe nuclear scattering.

A Solar System Test of Self-Interacting Dark Matter (2018) · 1.00 · paraphrased: the licence does not allow quoting
Estimated the scattering cross section between dark matter and a target of N nucleons according to the method used in this paper's direct WIMP detection.

Direct Detection of Ultralight Dark Matter via Astronomical Ephemeris (2018) · 0.98 · paraphrased: the licence does not allow quoting
Used this paper's calculation to compute the capture rate for its cross section.

Search for High-Energy Neutrinos From the Sun Using Ten Years of IceCube Data (2025) · 0.96 · paraphrased: the licence does not allow quoting
Followed the formalism described in this paper for the higgsino-nucleon scattering cross section.

The Race to Find Split Higgsino Dark Matter (2021) · 0.96 · paraphrased: the licence does not allow quoting
Followed this paper to give the SI and SD cross sections.

Dark Matter and the Higgs in Natural SUSY (2016) · 0.86 · paraphrased: the licence does not allow quoting
Calculated the relic abundance following this paper.

The Galactic Center Region Gamma Ray Excess from A Supersymmetric Leptophilic Higgs Model (2011) · 0.90 · paraphrased: the licence does not allow quoting

Uses its data or values 4 of 30 papers with this label

Used the canonical value sigma = 270 km/s from this paper.

New Limits on Charged Dark Matter from Large-Scale Coherent Magnetic Fields (2019) · 1.00 · paraphrased: the licence does not allow quoting
Used the values listed in Tables 8 and 9 of this paper for these parameters.

Light mixed sneutrinos as thermal dark matter (2010) · 1.00 · paraphrased: the licence does not allow quoting
Used the values given in this paper for the mass fraction and distribution of element i.

Neutrinos from Inert Doublet Dark Matter (2009) · 1.00 · paraphrased: the licence does not allow quoting
Used the same values for the parameters taken from this paper.

General Neutrino Interactions from an Effective Field Theory Perspective (2019) · 0.99 · paraphrased: the licence does not allow quoting

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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

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Contests it 1 paper

In the notation of [ref] , the signs before $x^2$ and $y^2$ in the respective formulas there should be altered in order to be correct.

Muon Flux Limits for Majorana Dark Matter Particles · Muon flux from the captured 2 · contest 0.88

Builds on it 2 papers

In Ref. [ref] we enlarged each simplified wino model by introducing a minimal set of parameters belonging to the EW sector (like $μ$ and $tanβ$) and tried to scrutinize the pMSSM thus obtained by considering three major constraints, namely, the LHC mass limits on the chargino-neutralino and the slepton sectors, measured dark matter (DM) [ref] relic density of the universe from the WMAP [ref] /PLANCK [ref] [A partial list of works on SUSY DM may be seen in Ref. [ref] .] and the precisely measured value of $2$ [ref] .

Reduced LHC constraints for higgsino-like heavier electroweakinos · Introduction · 0.80
We note that our results for annihilations into a pair of fermions include the case of flavour-off-diagonal sfermion mixing as well, which is covered in [ref] and [ref] , but was not yet included in [ref] , wherein only flavour-diagonal right-left sfermion mixing was taken into account, although it is straightforward to extend these results to the general flavour-off-diagonal case.

Non-relativistic pair annihilation of nearly mass degenerate neutralinos and charginos I. General framework and S-wave annihilation · Analytic checks · 0.85

Uses its method or tool 51 papers

In this approximation the capture rate can be written in an analytical form [ref] C = M_⊙ρ_χv̅/4√(6)m_χ^2η ∑_if_iσ_i(m_χ+m_i)^2/m_i^2a

Annihilation of NMSSM neutralinos in the Sun and neutrino telescope limits · Neutralino capture rate in the Sun · 0.94
Assuming only $s$-wave annihilations, one can obtain the $x_f=m_2/T_f$ [We use $m_2$ as the mass of the neutral scalar component of $Φ_2$ because there are no mass corrections which occur only after EW symmetry breaking] at freeze-out where $T_f$ is the freeze-out temperature, and the relic abundance $Ω_dm h^2$ to be [ref] : [equation] where $m_P$ is the Planck mass (not the reduced Planck mass which we have denoted as $M_Pl$), $g$ and $g_*$ are the number of degrees of freedom in the plasma and the entropic number of degrees of freedom respectively and $⟨σ v⟩$ is taken from Eq. ([ref]).

Inflation and Dark Matter in the Inert Doublet Model · Dark matter · 0.95
Finally, the $ψ$-nucleon elastic scattering cross section is given by [ref] : [equation] where $μ_n,p$ is the DM–nucleon reduced mass.

Dark matter and a new gauge boson through kinetic mixing · Direct detection of dark matter · 0.93

Uses its data or values 27 papers

It was found that wino masses up to about $1060 GeV$ for $m_χ̃_1^0 ≲400 GeV$ and higgsino masses up to $900 GeV$ for $m_χ̃_1^0 ≲240 GeV$ have been excluded in the simplified model of SUSY [ref] , where $χ̃_1^0$ denotes the lightest neutralino, acting as the lightest supersymmetric particle (LSP) and thus a DM candidate under the assumption of $R$-parity conservation [ref] , and $m_χ̃_1^0$ is its mass.

Impact of recent measurement of $(g-2)_\mu$, LHC search for supersymmetry, and LZ experiment on Minimal Supersymmetric Standard Model · Introduction · 0.96
Since we would like to consider the results of [ref] , we use the same values for the parameters [equation] taken from [ref] .

General Neutrino Interactions from an Effective Field Theory Perspective · Exotic interactions in coherent scattering and beta decay · 0.99
The DM mass density, $ρ_χ= n_χm_χ$, in the neighborhood of the solar system is about 0.3 GeV/cm$^3$ [ref] .

Towards Closing the Window on Strongly Interacting Dark Matter: Far-Reaching Constraints from Earth's Heat Flow · Dark Matter Capture Rate of Earth · 0.99

Compares with it 4 papers

Eq. ([ref]) agrees numerically within $20÷40$% with the respective formula of [ref] .

Muon Flux Limits for Majorana Dark Matter Particles · Muon flux from the captured 2 · 1.00
Rather than being associated to supersymmetry [ref] , WIMP dark-matter emerges here as a neutrino mass mediator, in a manner distinct from scotogenic approaches [ref] , and also inequivalent to the dark inverse-seesaw realization [ref] .

Linear seesaw mechanism from dark sector · Introduction · 0.93
The value of $$ is about 3 orders larger than that of thermal DM [ref] .

A simple and natural interpretations of the DAMPE cosmic-ray electron/positron spectrum within two sigma deviations · Extra Sources · 0.98

Cites it as background 746 papers

where $h^0$ and $H^0$ are the SM-like Higgs and heavy Higgs, respectively, $C_h χ̃χ̃$ ($C_H χ̃χ̃$) stands for the $h^0$($H^0$)-$χ̃^0$-$χ̃^0$ coupling, $C_hqq$ ($C_Hqq$) is the $h^0$($H^0$)-quark-quark Yukawa coupling, explicit expressions of them are given in literatures [ref] .

Implications of CDMS II result on Higgs sector in the MSSM · Introduction · 0.83
In scenarios of dark matter (DM) for the weakly-interacting massive particle (WIMP) [ref] , a DM particle with mass of the weak scale should have a thermally-averaged annihilation cross section of the order of $⟨σv ⟩= 2 ×10^26 cm^3/sec$ [ref] .

Impacts of new small-scale N-body simulations on dark matter annihilations constrained from cosmological 21cm line observations · Introduction · 0.81
Several facilities were aimed to detect it directly [ref] , mainly when it lies in the range of hundreds of GeV mass scale, characterizing what is known as a weakly interacting massive particle (WIMP) [ref] .

Higgs mass and right-handed sneutrino WIMP in a supersymmetric 3-3-1 model · Introduction · 0.84

Discussion

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[1] [1]

Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2

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[2] [2]

Dark Matter in the Universe . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 14 2.1. Inventory of Dark Matter . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 14 2.2. Theoretical arguments . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 20 2.3. Baryonic Content of the Universe . . . . . . . . . . . . . . . . . . . . . ....

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[3] [3]

Cosmological Abundance of a WIMP . . . . . . . . . . . . . . . . . . . . . . . . . . . 32 3.1. Simple Estimates . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 34 3.2. Why WIMPs? . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 38 3.3. Standard Calculation of Relic Abundance . . . . . . . . . . . . . . . . . . . . ...

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[4] [4]

Supersymmetric Models . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 46 4.1. Motivation, Goals, and Some Formalities . . . . . . . . . . . . . . . . . . . . . . . 46 4.2. Minimal Supersymmetric Standard Model . . . . . . . . . . . . . . . . . . . . . . . 52 4.3. SUSY-GUT and Supergravity Models . . . . . . . . . . . . . . . . . . . . . . . . . 60

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[5] [5]

Laboratory Constraints . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 62 5.1. Remarks . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 62 5.2. Constraints on the Higgs Sector . . . . . . . . . . . . . . . . . . . . . . . . . . . 62 5.3. Constraints on the Chargino/Neutralino Sector . . . . . . . . . . . . . . . ...

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[6] [6]

Neutralino Annihilation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 72 6.1. Remarks . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 72 6.2. Weak–Gauge-Boson Final States . . . . . . . . . . . . . . . . . . . . . . . . . . . 74 6.3. Final States Containing Higgs Bosons . . . . . . . . . . . . . . . . . . . . . ...

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[7] [7]

Elastic-Scattering Cross Sections . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 96 7.1. The Basic Ingredients . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 96 7.2. Axial-Vector (spin) Interaction . . . . . . . . . . . . . . . . . . . . . . . . . . . . 98 7.3. Scalar Interaction . . . . . . . . . . . . . . . . . . . . . . . . ...

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[8] [8]

Direct Detection of Neutralinos . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 120 8.1. Theory . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 120 8.2. Detectors . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1 30 8.3. Inelastic-Scattering Techniques . . . . . . . . . . . . . . . . . . . . ...

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[9] [9]

Energetic Neutrinos from WIMP Annihilation in the Sun and /or Earth . . . . . . . . . . . . 136 9.1. General Description . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 136 9.2. Detectors and Atmospheric-Neutrino Background . . . . . . . . . . . . . . . . . . . 142 9.3. Annihilation Rate in the Sun and Earth . . . . . . . . . . . . . . . ....

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[10] [10]

Cosmic Rays from WIMP Annihilation in the Halo . . . . . . . . . . . . . . . . . . . . 178 10.1. Cosmic-Ray Antiprotons . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 180 10.2. Cosmic-Ray Positrons . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 182 10.3. Cosmic Gamma Rays . . . . . . . . . . . . . . . . . . . . . . . . . . . . ...

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[11] [11]

Sample Analysis of the MSSM . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 188 11.1. Orientation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 188 11.2. SUSY Parameter Space . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 190 11.3. Relic Density . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . ...

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[12] [12]

Other Particle Dark-Matter Candidates . . . . . . . . . . . . . . . . . . . . . . . . . 208 12.1. The Rise and Fall of Heavy-Neutrino Dark Matter . . . . . . . . . . . . . . . . . . . 210 12.2. Sneutrinos . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 214 12.3. Other Supersymmetric Dark-Matter Candidates . . . . . . . . . . . . . ...

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[13] [13]

Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 216 13.1. Summary of Calculations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 218 13.2. Central Results . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 220 13.3. Concluding Remarks . . . . . . . . . . . . . . . . . . . . . . . . . . . ...

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[14] [14]

Acknowledgments . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 224 Appendix A. Construction of the MSSM . . . . . . . . . . . . . . . . . . . . . . . . . . 224 A.1. Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 224 A.2. Superﬁeld Formalism . . . . . . . . . . . . . . . . . . . . . . . . . . . . ....

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