Pith. sign in

REVIEW 4 major objections 4 minor 8 cited by

Minimal Dirac seesaw dark matter

T0 review · 4 major / 4 minor · reviewed 2026-08-11 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read The minimal Z4-symmetric Type-I Dirac seesaw can simultaneously supply a stable thermal dark-matter candidate, generate light Dirac neutrino masses, produce the baryon asymmetry through Dirac leptogenesis, and leave gravitational-wave and…

desk verdict Viable Dirac seesaw with DM, but the v1-v3 domain-wall exclusion is a load-bearing gap that leaves the advertised GW signal unsupported. read the letter →

arxiv 2412.12267 v2 pith:3SG5SHZX submitted 2024-12-16 hep-ph astro-ph.CO

Zafri Ahmed Borboruah , Debasish Borah , Lekhika Malhotra , Utkarsh Patel This is my paper · ORCID
classification hep-phastro-ph.CO
keywords DiracseesawscalardarkmatterZ4symmetrydomainwallsgravitationalwavesleptogenesiseffectiveneutrinonumberNeffchargeconjugation
topics Matter-Antimatter AsymmetryDark Matter
open problems Dark MatterMatter-Antimatter Asymmetry
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper tries to establish that one minimal field content—the fields already required for the Type-I Dirac seesaw, arranged under a Z4 symmetry and with lepton number conserved by a global U(1)_L—can explain neutrino mass, dark matter, and the baryon asymmetry together. The imaginary part of the complex scalar ρ is a stable thermal scalar dark-matter candidate protected by an effective dark charge-conjugation symmetry, so no extra dark-sector fields are needed. The same spontaneous Z4 breaking that generates tiny Dirac neutrino masses also produces domain walls, and a small explicit bias term V_bias = -√2 ε $v_ρ^{4}$ cos θ makes those walls annihilate, producing a stochastic gravitational-wave background within reach of planned detectors. The parameter space that fits neutrino oscillations and the observed baryon asymmetry via Dirac leptogenesis also predicts enhanced ΔNeff and resonant dark-matter masses that future dark-matter and CMB experiments can probe.

What carries the argument

The central mechanism is the Z4-symmetric scalar potential with an induced VEV hierarchy, where the coupling λ1 both fixes the dark-matter mass through the resonance condition mχ = mh3/2 and controls the domain-wall profile. The imaginary component χ of ρ is the stable scalar dark matter, and the four degenerate minima of the potential give adjacent and non-adjacent walls with different tensions, σ_adj = mθ $v_ρ^{2}$/2 and σ_non-adj = (2√2/3)√λρ $v_ρ^{3}$. The load-bearing bias term V_bias = -√2 ε $v_ρ^{4}$ cos θ lifts the degeneracy so walls annihilate when vacuum pressure equals tension; its magnitude, together with the wall tensions, sets the gravitational-wave spectrum via the peak formulas of Eqs. (3.10)-(3.11). The same parameter set fixes v_η, the seesaw scale M_1, and the Yukawa couplings Y_L and Y_R that determine the neutrino mass, Dirac leptogenesis, and the right-handed-neutrino decoupling temperature controlling ΔNeff.

What would settle it

A lattice simulation of the Z4-breaking phase transition with the bias term of Eq. (3.6) would settle the claim: if the degenerate v1–v3 wall channel percolates and fails to annihilate, the cosmological history is broken. A null result from planned gravitational-wave observatories in the predicted peak band for the scanned benchmarks vρ ∈ [$10^{5}$, 2×$10^{8}$] GeV and ε ∈ [$10^{-26}$, $10^{-21}$] would exclude the central parameter region.

Watch

Extended reading notes

Core claim

In this model, the neutrino mass formula is mν = Y_L $M_N^{{-1}}$ Y_R v v_η / 2, with the η VEV vη induced by the ρ VEV vρ, while the dark-matter candidate χ is the imaginary component of ρ with mass $mχ^{2}$ ≃ 8λ1 $v_ρ^{2}$ + 2√2 μ1 v_η. The authors show that after spontaneous Z4-breaking there are four degenerate minima and two classes of domain walls; the bias in Eq. (3.6) gives adjacent walls a potential difference √2 ε $v_ρ^{4}$ and non-adjacent walls 2√2 ε $v_ρ^{4}$, making the walls annihilate before BBN and emit gravitational waves whose peak amplitude and frequency are set by wall tensions and δV. A numerical scan restricted to the resonant regime mχ = mh3/2 finds points that simultaneously satisfy relic density, direct and indirect detection bounds, electroweak precision data, and vacuum stability up to the Planck scale, while reproducing neutrino oscillation data and a baryon asymmetry ηB in the observed range. The same scan places the additional relativistic degrees of freedom from right-handed neutrinos at ΔNeff = 0.14 in the thermalized region, and predicts GW signals with SNR > 10 for planned observatories across a range of dark-matter masses and seesaw scales.

Load-bearing premise

The load-bearing premise is that the one domain-wall channel that the bias does not split—the wall between the two opposite minima that remain exactly degenerate—can be safely ignored and will not survive as a percolating network that dominates the universe.

Editorial extensions

If this is right

  • A detection of the predicted gravitational-wave peak would directly measure the Z4-breaking scale vρ and, through the resonance condition, the dark-matter mass mχ.
  • The same parameter space ties the seesaw and leptogenesis scale to vη via M1 ≳ 10^9 GeV (vη/100 GeV), so the mechanism is not pushed to arbitrarily high scales.
  • Regions with thermalized right-handed neutrinos predict ΔNeff = 0.14, which future CMB surveys will be able to confirm or exclude.
  • In the resonant regime, dark-matter masses range from about 10^2 to 10^5 GeV, with direct-detection lower bounds between 161 and 593 GeV for the sampled portal couplings; these are testable by next-generation dark-matter experiments.
  • A future positive signal in neutrinoless double beta decay would falsify the Dirac nature of neutrinos assumed here and break the model's connection to the observed baryon asymmetry.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • An extension the paper leaves implicit is deriving the bias parameter ε from explicit Planck-scale-suppressed operators and checking that the same operators do not make the dark matter decay faster than the age of the Universe.
  • The v1–v3 wall channel is excluded rather than simulated; a dedicated lattice study would either strengthen the model by showing that channel annihilates through neighbouring-wall pressure or overturn the gravitational-wave prediction, so it is the clearest next step.
  • The reported ΔNeff value is 0.14 when right-handed neutrinos thermalize and decouple; coupling the decoupling temperature to leptogenesis efficiency could produce a continuum of smaller values, giving a testable correlation that the paper does not explore.
  • Because the gravitational-wave peak frequency and the dark-matter mass are linked by the resonance condition, a future GW measurement plus a direct scalar mass measurement would overdetermine vρ and λ1, offering a multi-messenger discriminator among models of this type.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

4 major / 4 minor

Summary. The manuscript proposes a minimal Type-I Dirac seesaw extension of the SM containing heavy Dirac fermions N_L,N_R, right-handed neutrinos nu_R, a real scalar eta, and a complex scalar rho, with a global Z4 symmetry and an unbroken U(1)_L. The imaginary component of rho, chi, is a stable scalar dark matter candidate protected by a C_dark/CP symmetry. Spontaneous Z4 breaking generates a Dirac neutrino mass through the induced VEV of eta, and also produces domain walls. A small bias term V_bias = -sqrt(2) epsilon v_rho^4 cos theta (Eq. 3.6) is introduced to make the walls annihilate and emit gravitational waves within reach of LISA, BBO, mu-ARES, and other experiments. The paper studies DM relic density, direct and indirect detection, Dirac leptogenesis, Delta N_eff, and presents numerical scans showing parameter regions consistent with neutrino oscillation data, baryon asymmetry, and DM constraints, together with projected GW sensitivities.

Significance. If valid, the model would be a minimal combined solution to neutrino mass, dark matter, and baryogenesis, with correlated observational signals in gravitational waves, Delta N_eff, neutrinoless double-beta decay, and DM searches. The economy of using the seesaw field content also for DM, stabilized by C_dark, is a genuine virtue. The numerical work uses standard public tools (SARAH, SPheno, micrOMEGAs) with clearly stated scan ranges and benchmark points, making the analysis reproducible in principle. The GW spectra are compared with a broad set of current and future experiments, and the Delta N_eff discussion is quantitative. However, the central GW claim depends on the fate of the zero-bias v1-v3 domain walls, which is not established, and the predictive content of the GW reach is weakened because the bias epsilon is a free parameter scanned over many orders of magnitude.

major comments (4)
  1. [Section 3, Eq. (3.7) and the paragraph following Eq. (3.12)] The paper excludes the domain wall between minima v1 and v3 on the grounds that delta V13 = 0 and that its collapse dynamics is more complex, but no dynamical proof or simulation is provided. Since the bias term in Eq. (3.6) is even under rho -> rho*, the minima v1 and v3 remain exactly degenerate, so a wall separating them has no volume pressure to drive annihilation. If such walls form a percolating network, they would survive and could dominate the universe, invalidating the BBN and Delta N_eff constraints and the GW signal calculation. The authors must either prove by a lattice simulation or a controlled analytic argument that these walls are destabilized by the surrounding network, introduce a small C_dark-breaking bias that lifts delta V13 and show that the DM lifetime constraint (Appendix D) is still satisfied, or demonstrate that v1/v3 regions do not percolate for the relevant initial conditions.
  2. [Section 3, Eqs. (3.10)-(3.12) and Fig. 8] The GW spectrum is computed using the instantaneous-annihilation approximation and formulas calibrated for Z2 domain walls from Ref. [165], while the Z4 network has two distinct wall types with different tensions and biases. The paper acknowledges that delayed annihilation shifts the peak frequency and modifies the spectral shape (Refs. [187-189]) but does not incorporate these effects. Since the peak amplitude scales as sigma^4/delta V^2 and the detectability in Fig. 13 is quantified by SNR > 10, the projected reach could shift substantially; a quantitative estimate of this systematic uncertainty is needed before the GW claims can be considered robust.
  3. [Section 5, Fig. 13] The bias parameter epsilon is treated as a free parameter scanned in the range 10^-26 to 10^-21, and the colored GW-sensitive region is the locus of SNR > 10 for that scan. The QG discussion in Section 3 and Appendix D only establishes that epsilon values of this order can be compatible with DM lifetime; it does not predict epsilon. The abstract's statement that the model generates GWs 'within reach' of future experiments is therefore a conditional projection, not a parameter-free prediction. This should be stated explicitly in the conclusions, and the claim of verifiability should be tempered accordingly.
  4. [Section 2.2, Eqs. (2.23)-(2.24)] The baryon asymmetry is computed with the simplified efficiency kappa_f = 1 for K <= 1 and kappa_f = 0.12/K^1.1 for K > 1. For weak washout with thermal initial abundance, kappa_f is not generally unity but depends on the initial conditions and on washout processes; the adopted approximation can overestimate eta_B. Since the lower bound M1 >~ 1.6 x 10^9 (v_eta/100 GeV) GeV and the colored regions in Fig. 13 depend on this efficiency, a more complete solution of the Boltzmann equations is needed to confirm the claimed parameter space for Dirac leptogenesis.
minor comments (4)
  1. [Throughout] The manuscript contains numerous typos and formatting errors, including 'Additionnaly', 'magnituded', 'mestasble', 'T able 1', 'a-as-well-as', and inconsistent table/figure captions; a careful proofread is needed.
  2. [Section 3, text after Eq. (3.12)] The statement that 'approximately 4/5th of the domain walls evolve under the adjacent bias and 1/5th under the non-adjacent bias' is not derived from the actual population of wall types in the Z4 network; weighting by the number of bias types rather than by the produced wall fractions is an oversimplification that affects the total GW spectrum in Fig. 8.
  3. [Section 5] The scan imposes the resonance condition m_chi = m_h3/2, so the plotted DM mass ranges are projections onto the resonance, not independent predictions of the model; this should be clarified when summarizing the 'predicted' m_chi ranges.
  4. [Fig. 13 caption] The caption does not specify whether the y-axis is epsilon itself or epsilon times v_rho^4; the axis label should be defined explicitly.

Circularity Check

1 steps flagged · score 6.0 of 10

Zero-bias v1–v3 domain walls are excluded after δV13=0, so the central DW-annihilation/GW claim is demonstrated only for the biased 5/6 of walls and reduces to assuming away the one wall the bias does not lift.

  1. self definitional [Section 3, 'Gravitational waves from domain walls', after Eqs. (3.6)–(3.7), paragraph beginning 'Starting from a homogeneous medium'.]
    "The domain wall between v1 and v3 is excluded from our analysis since the associated bias, δV13 = 0, and its collapse dynamics is more complex due to the influence of surrounding domain walls. The remaining biases, δVij, consist of four biases corresponding to adjacent domain walls and one bias for non-adjacent domain walls. As a result, approximately 4/5th of the domain walls evolve under the influence of the adjacent bias, δVadj., while 1/5th experience the non-adjacent bias, δVnon−adj."

    Eq. (3.6) defines Vbias = −√2 ε vρ^4 cosθ, and Eq. (3.7) then gives δV13 = 0 for the minima v1=(0,vρ) and v3=(0,−vρ), which are related by the χ→−χ symmetry that stabilizes the DM. The paper's central cosmological claim — that 'these cosmologically catastrophic walls can be made to annihilate away by introducing bias terms' — is then established only for the five wall types with δV≠0; the sixth, exactly degenerate wall is removed from the analysis by the quoted sentence. Hence the conclusion that the wall network annihilates and produces the advertised GW signal is true by construction only for the subset of walls that the bias term was designed to bias, and the survival/dominance of the non-adjacent v1–v3 network is assumed away rather than derived or simulated.

full rationale

The single reportable circular step is the treatment of the v1–v3 domain walls. The bias term (3.6) is chosen so that, by Eq. (3.7), δV13 = 0; the paper then explicitly excludes that wall type from the annihilation/GW analysis. The central claim that the Z4-breaking walls 'can be made to annihilate away' is therefore verified only for the biased subset, while the zero-bias wall is removed by hand. This is a partial reduction of the main cosmological result to an assumption about which walls exist, rather than a derivation or simulation covering all wall types. The remaining phenomenology is largely self-contained and not circular in the same way: the neutrino mass formula (2.11) follows from the standard Dirac seesaw with VEVs fixed by tadpole equations; the DM relic, direct/indirect detection, and ∆Neff calculations use external codes and data as constraints; and the leptogenesis scan computes ε and K from Casas-Ibarra parameters and then selects points matching the observed ηB, which is a consistency scan rather than a fitted quantity disguised as a prediction. Self-citations to earlier Dirac-seesaw domain-wall papers [80,81] are used for standard formulas and comparison, not to import an unverified uniqueness theorem. Thus the score of 6 reflects the one load-bearing by-construction exclusion in the GW/domain-wall sector, while the model's other advertised connections retain independent content.

Assumptions & free parameters 9 free parameters · 7 assumptions · 5 invented entities

The central derivation rests on a global U(1)_L, the Z4 charge assignments, CP conservation in the scalar sector, a specific vacuum hierarchy, and a QG-origin bias with an effective scale much larger than the Planck scale. The numerical results use many scanned and tuned parameters: m_chi, lambda_rho, lambda_eta, v_rho, mu_1, lambda_H_rho, plus v_eta, M1, and Casas-Ibarra random matrices in the leptogenesis scan, and the DW bias epsilon. The v1-v3 wall exclusion is an unproved dynamical assumption. No new particles with independent evidence appear; all BSM fields are postulates, though motivated by neutrino mass, DM, and leptogenesis.

free parameters (9)
  • bias parameter epsilon = 1e-26 to 1e-21 (benchmarks)
    Free dimensionless parameter controlling wall annihilation and GW peak; chosen so signals fall in LISA, BBO, and micro-ARES bands.
  • DM mass m_chi = 1 to 1e5 GeV (scanned)
    Scanned; only the resonance region m_chi = m_h3 / 2 is kept to avoid overabundant relic density.
  • quartic couplings lambda_rho, lambda_eta = 1e-4 to 1; lambda_rho = 0.1 in GW benchmarks
    Scanned; set DM annihilation rates, scalar masses, and DW tensions.
  • Z4 breaking scale v_rho = 1e3 to 1e8 GeV
    Scanned; controls v_eta, DM mass, DW tension, and GW peak.
  • scalar mass parameter mu_1 = 1e-4 to 1e3 GeV
    Scanned; controls induced VEV v_eta through Eq. (2.5).
  • Higgs portal lambda_H_rho = 0.02 (fiducial); 0.02 to 0.14
    Scanned; sets direct detection cross-section and scalar mixing.
  • induced VEV v_eta = 50 to 1e6 GeV (sampled)
    Sampled with M1 and R to fit neutrino oscillation data and baryon asymmetry.
  • lightest heavy fermion mass M1 = 1e9 to 1e15 GeV (sampled)
    Sampled; values below about 1e9 (v_eta / 100 GeV) GeV cannot produce the observed baryon asymmetry.
  • Casas-Ibarra matrix R elements = random magnitudes 1e-4 to 10
    Random complex matrices reconstructed to reproduce neutrino mixing and CP asymmetry epsilon.
assumptions (7)
  • domain assumption Exact global U(1)_L lepton number symmetry
    Prevents Majorana mass terms for nu_R and N at any order; introduced in Sec. 2 and Table 1 to guarantee pure Dirac neutrinos.
  • domain assumption Z4 symmetry with charges rho -> i rho, eta -> -eta, nu_R odd
    Realizes tree-level Dirac seesaw and prevents direct L-H-nu_R coupling; Sec. 2 and Table 1.
  • domain assumption CP invariance in the scalar sector (rho <-> rho*)
    Makes chi stable via dark charge conjugation C_dark; Sec. 2 and Sec. 2.4.
  • domain assumption Vacuum hierarchy: v_rho >> v, mu_eta, mu_1 << v_rho, lambda_rho_eta = lambda_H_eta ~ 0, lambda_rho / 4 > lambda_1
    Required for the induced VEV v_eta, tadpole solutions Eq. (2.5), and the correct scalar mass spectrum.
  • ad hoc to paper Quantum gravity origin of the bias with effective scale Lambda_QG >= 1e23 GeV
    Appendix D; needed so that chi is long-lived while the bias epsilon is large enough to annihilate walls. Assumes non-perturbative QG effects beyond the Planck scale or additional protecting gauge symmetries.
  • domain assumption Instantaneous scaling-law annihilation of Z4 domain walls
    GW spectrum from Eqs. (3.10)-(3.12) relies on simulations for Z2-like walls; delayed annihilation is acknowledged but not included, and the v1-v3 wall network is excluded.
  • domain assumption Thermal WIMP freeze-out for chi
    Used to compute Omega_chi h^2 via Eq. (2.27); non-thermal DW production is only estimated and not included.
invented entities (5)
  • Right-handed neutrinos nu_R
    purpose: Provide Dirac mass partners for active neutrinos and contribute Delta Neff when thermalized.
    No direct observations; required for the Dirac seesaw.
  • Heavy Dirac fermions N_L, N_R
    purpose: Mediate the Type-I Dirac seesaw and source CP violation for Dirac leptogenesis.
    No direct observations.
  • Real scalar eta
    purpose: Carries the induced VEV v_eta that links nu_R to N; Z4-odd.
    No direct observations; part of the seesaw field content.
  • Complex scalar rho
    purpose: Spontaneous Z4 breaking sets the seesaw scale; its imaginary part chi is the DM candidate.
    No direct observations; the DM sector is observed only gravitationally.
  • Scalar DM chi
    purpose: Thermal scalar dark matter stabilized by C_dark.
    No particle-level evidence; the observed DM abundance is the only independent handle and it is used to constrain parameters.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Minimal Dirac seesaw dark matter." pith.science (2026). https://pith.science/paper/3SG5SHZX

@misc{pith2026241212267,
  author       = {Pith},
  title        = {Pith review of: Minimal Dirac seesaw dark matter},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/3SG5SHZX}},
  note         = {Machine review of arXiv:2412.12267}
}
abstract

We propose a minimal Type-I Dirac seesaw which accommodates a thermal scalar dark matter (DM) candidate protected by a charge conjugation symmetry in dark sector $C_{\rm dark}$, without introducing any additional field beyond the ones taking part in the seesaw. A $Z_4$ symmetry is introduced to realise the tree level Dirac seesaw while the Majorana mass terms are prevented by an unbroken global lepton number symmetry. While the spontaneous $Z_4$ breaking together with electroweak symmetry breaking lead to the generation of light Dirac neutrino mass, it also results in the formation of domain walls. These cosmologically catastrophic walls can be made to annihilate away by introducing bias terms while also generating stochastic gravitational waves (GW) within reach of near future experiments like \texttt{LISA}, \texttt{BBO}, $\mu$-\texttt{ARES} etc. The scalar DM parameter space can be probed at direct and indirect search experiments. Light Dirac neutrinos also enhance the relativistic degrees of freedom $N_{\rm eff}$ within reach of future cosmic microwave background (CMB) experiments. The model can also explain the observed baryon asymmetry via Dirac leptogenesis.

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 8 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. $Z^\prime$ Portal Dark Matter with Observable $\Delta N_{\rm eff}$

    hep-ph 2026-07 accept novelty 5.5 of 10

    Dirac right-handed neutrinos in a U(1)_{B-L} Z' portal model produce observable ΔN_eff that, together with direct/indirect detection and collider bounds, carves out testable WIMP and FIMP dark-matter regions.

  2. Sterile neutrino Dark Matter in the minimal Dirac Seesaw

    hep-ph 2026-03 conditional novelty 5.0 of 10

    A minimal Dirac seesaw model yields viable sterile-neutrino dark matter via freeze-in, with the right-handed mixing angle θ_R bypassing X-ray bounds.

  3. Radiative Dirac neutrino masses and dark matter in a $U(1)_{B-L}$ extended model

    hep-ph 2026-01 conditional novelty 5.0 of 10

    A U(1) extension of the Standard Model generates Dirac neutrino masses at one loop and provides a stable dark matter candidate via a residual discrete symmetry.

  4. Gravitational waves from seesaw assisted collapsing domain walls

    hep-ph 2025-12 conditional novelty 5.0 of 10

    Right-handed-neutrino couplings generate the energy bias that collapses Z2 domain walls, linking the type-I seesaw mass scale to observable gravitational-wave peaks and to resonant leptogenesis.

  5. Electromagnetic Dirac Cogenesis

    hep-ph 2025-07 conditional novelty 5.0 of 10

    A single out-of-equilibrium decay chain of heavy vector-like fermions via electromagnetic dipole operators can simultaneously generate the baryon asymmetry and an asymmetric dark matter relic with mass around 1.9 prot...

  6. Seesaw Portal to Super Heavy Dark Matter with $Z_3$ Symmetry

    hep-ph 2025-06 conditional novelty 5.0 of 10

    Adding Z3 symmetry to the seesaw portal allows the dark scalar to decay promptly to dark matter, evading BBN limits for the m_N>m_phi mass ordering.

  7. Gravitational wave signatures of dark sector portal leptogenesis

    hep-ph 2025-04 conditional novelty 5.0 of 10

    A Z2-odd dark sector with a heavy fermion and two scalars enables TeV-scale leptogenesis and produces LISA-visible gravitational waves from a strong electroweak phase transition.

  8. Probing Leptophobic Dark Sectors via Gravitational Wave Signatures

    hep-ph 2025-08 unverdicted novelty 4.0 of 10

    A gauged U(1)_B extension of the Standard Model is claimed to produce observable gravitational waves from a first-order phase transition, with dark matter around 8-12 TeV.

Reference graph

Works this paper leans on

200 extracted references · 11 canonical work pages · cited by 8 Pith papers

  1. [165]

    Hiramatsu, M

    T. Hiramatsu, M. Kawasaki, and K. Saikawa, On the estimation of gravitational wave spectrum from cosmic domain walls , JCAP 02 (2014) 031, [ arXiv:1309.5001]

    arXiv 2014

  2. [1]

    Navas et al

    Particle Data GroupCollaboration, S. Navas et al. , Review of particle physics , Phys. Rev. D 110 (2024), no. 3 030001

    2024

  3. [2]

    M. J. Dolinski, A. W. P. Poon, and W. Rodejohann, Neutrinoless Double-Beta Decay: Status and Prospects, Ann. Rev. Nucl. Part. Sci. 69 (2019) 219–251, [ arXiv:1902.04097]

    arXiv 2019

  4. [3]

    Majorana Collaboration, I. J. Arnquist et al. , Final Result of the Majorana Demonstrator’s Search for Neutrinoless Double- β Decay in Ge76 , Phys. Rev. Lett. 130 (2023), no. 6 062501, [ arXiv:2207.07638]

    arXiv 2023

  5. [4]

    Minkowski, µ → eγ at a Rate of One Out of 109 Muon Decays?, Phys

    P. Minkowski, µ → eγ at a Rate of One Out of 109 Muon Decays?, Phys. Lett. B 67 (1977) 421–428

    1977

  6. [5]

    Gell-Mann, P

    M. Gell-Mann, P. Ramond, and R. Slansky, Complex Spinors and Unified Theories , Conf. Proc. C 790927 (1979) 315–321, [ arXiv:1306.4669]

    arXiv 1979

  7. [6]

    R. N. Mohapatra and G. Senjanovic, Neutrino Mass and Spontaneous Parity Nonconservation, Phys. Rev. Lett. 44 (1980) 912

    1980

  8. [7]

    Sawada and A

    O. Sawada and A. Sugamoto, eds., Proceedings: Workshop on the Unified Theories and the Baryon Number in the Universe: Tsukuba, Japan, February 13-14, 1979 , (Tsukuba, Japan), Natl.Lab.High Energy Phys., 1979

    1979

Show all 200 references
  1. [8]

    Yanagida, Horizontal Symmetry and Masses of Neutrinos , Prog

    T. Yanagida, Horizontal Symmetry and Masses of Neutrinos , Prog. Theor. Phys. 64 (1980) 1103

    1980

  2. [9]

    Schechter and J

    J. Schechter and J. W. F. Valle, Neutrino Masses in SU(2) x U(1) Theories , Phys. Rev. D 22 (1980) 2227

    1980

  3. [10]

    R. N. Mohapatra and G. Senjanovic, Neutrino Masses and Mixings in Gauge Models with Spontaneous Parity Violation , Phys. Rev. D 23 (1981) 165

    1981

  4. [11]

    Schechter and J

    J. Schechter and J. W. F. Valle, Neutrino Decay and Spontaneous Violation of Lepton Number, Phys. Rev. D 25 (1982) 774. – 35 –

    1982

  5. [12]

    Wetterich, Neutrino Masses and the Scale of B-L Violation , Nucl

    C. Wetterich, Neutrino Masses and the Scale of B-L Violation , Nucl. Phys. B 187 (1981) 343–375

    1981

  6. [13]

    Lazarides, Q

    G. Lazarides, Q. Shafi, and C. Wetterich, Proton Lifetime and Fermion Masses in an SO(10) Model, Nucl. Phys. B 181 (1981) 287–300

    1981

  7. [14]

    Brahmachari and R

    B. Brahmachari and R. N. Mohapatra, Unified explanation of the solar and atmospheric neutrino puzzles in a minimal supersymmetric SO(10) model , Phys. Rev. D 58 (1998) 015001, [hep-ph/9710371]

    1998 arXiv

  8. [15]

    R. Foot, H. Lew, X. G. He, and G. C. Joshi, Seesaw Neutrino Masses Induced by a Triplet of Leptons, Z. Phys. C 44 (1989) 441

    1989

  9. [16]

    Roncadelli and D

    M. Roncadelli and D. Wyler, Naturally Light Dirac Neutrinos in Gauge Theories , Phys. Lett. B 133 (1983) 325–329

    1983

  10. [17]

    Roy and O

    P. Roy and O. U. Shanker, Observable Neutrino Dirac Mass and Supergrand Unification , Phys. Rev. Lett. 52 (1984) 713–716. [Erratum: Phys.Rev.Lett. 52, 2190 (1984)]

    1984

  11. [18]

    K. S. Babu and X. G. He, DIRAC NEUTRINO MASSES AS TWO LOOP RADIATIVE CORRECTIONS, Mod. Phys. Lett. A 4 (1989) 61

    1989

  12. [19]

    J. T. Peltoniemi, D. Tommasini, and J. W. F. Valle, Reconciling dark matter and solar neutrinos, Phys. Lett. B 298 (1993) 383–390

    1993

  13. [20]

    Centelles Chuli´ a, E

    S. Centelles Chuli´ a, E. Ma, R. Srivastava, and J. W. F. Valle, Dirac Neutrinos and Dark Matter Stability from Lepton Quarticity , Phys. Lett. B767 (2017) 209–213, [arXiv:1606.04543]

    2017 arXiv

  14. [21]

    Aranda, C

    A. Aranda, C. Bonilla, S. Morisi, E. Peinado, and J. W. F. Valle, Dirac neutrinos from flavor symmetry , Phys. Rev. D 89 (2014), no. 3 033001, [ arXiv:1307.3553]

    2014 arXiv

  15. [22]

    Chen, G.-J

    P. Chen, G.-J. Ding, A. D. Rojas, C. A. Vaquera-Araujo, and J. W. F. Valle, Warped flavor symmetry predictions for neutrino physics , JHEP 01 (2016) 007, [ arXiv:1509.06683]

    2016 arXiv

  16. [23]

    E. Ma, N. Pollard, R. Srivastava, and M. Zakeri, Gauge B − L Model with Residual Z3 Symmetry, Phys. Lett. B 750 (2015) 135–138, [ arXiv:1507.03943]

    2015 arXiv

  17. [24]

    M. Reig, J. W. F. Valle, and C. A. Vaquera-Araujo, Realistic SU(3)c ⊗ SU(3)L ⊗ U(1)X model with a type II Dirac neutrino seesaw mechanism , Phys. Rev. D 94 (2016), no. 3 033012, [arXiv:1606.08499]

    2016 arXiv

  18. [25]

    Wang and Z.-L

    W. Wang and Z.-L. Han, Naturally Small Dirac Neutrino Mass with Intermediate SU (2)L Multiplet Fields , arXiv:1611.03240. [JHEP04,166(2017)]

    2017 arXiv

  19. [26]

    W. Wang, R. Wang, Z.-L. Han, and J.-Z. Han, The B − L Scotogenic Models for Dirac Neutrino Masses , Eur. Phys. J. C77 (2017), no. 12 889, [ arXiv:1705.00414]

    2017 arXiv

  20. [27]

    F. Wang, W. Wang, and J. M. Yang, Split two-Higgs-doublet model and neutrino condensation, Europhys. Lett. 76 (2006) 388–394, [ hep-ph/0601018]

    2006 arXiv

  21. [28]

    Gabriel and S

    S. Gabriel and S. Nandi, A New two Higgs doublet model , Phys. Lett. B655 (2007) 141–147, [hep-ph/0610253]

    2007 arXiv

  22. [29]

    S. M. Davidson and H. E. Logan, Dirac neutrinos from a second Higgs doublet , Phys. Rev. D 80 (2009) 095008, [ arXiv:0906.3335]

    2009 arXiv

  23. [30]

    S. M. Davidson and H. E. Logan, LHC phenomenology of a two-Higgs-doublet neutrino mass model, Phys. Rev. D82 (2010) 115031, [ arXiv:1009.4413]. – 36 –

    2010 arXiv

  24. [31]

    Bonilla and J

    C. Bonilla and J. W. F. Valle, Naturally light neutrinos in Diracon model, Phys. Lett. B762 (2016) 162–165, [ arXiv:1605.08362]

    2016 arXiv

  25. [32]

    Farzan and E

    Y. Farzan and E. Ma, Dirac neutrino mass generation from dark matter , Phys. Rev. D86 (2012) 033007, [ arXiv:1204.4890]

    2012 arXiv

  26. [33]

    Bonilla, E

    C. Bonilla, E. Ma, E. Peinado, and J. W. F. Valle, Two-loop Dirac neutrino mass and WIMP dark matter , Phys. Lett. B762 (2016) 214–218, [ arXiv:1607.03931]

    2016 arXiv

  27. [34]

    Ma and O

    E. Ma and O. Popov, Pathways to Naturally Small Dirac Neutrino Masses , Phys. Lett. B764 (2017) 142–144, [ arXiv:1609.02538]

    2017 arXiv

  28. [35]

    Ma and U

    E. Ma and U. Sarkar, Radiative Left-Right Dirac Neutrino Mass , Phys. Lett. B776 (2018) 54–57, [arXiv:1707.07698]

    2018 arXiv

  29. [36]

    Borah, Light sterile neutrino and dark matter in left-right symmetric models without a Higgs bidoublet , Phys

    D. Borah, Light sterile neutrino and dark matter in left-right symmetric models without a Higgs bidoublet , Phys. Rev. D94 (2016), no. 7 075024, [ arXiv:1607.00244]

    2016 arXiv

  30. [37]

    Borah and A

    D. Borah and A. Dasgupta, Common Origin of Neutrino Mass, Dark Matter and Dirac Leptogenesis, JCAP 12 (2016), no. 12 034, [ arXiv:1608.03872]

    2016 arXiv

  31. [38]

    Borah and A

    D. Borah and A. Dasgupta, Observable Lepton Number Violation with Predominantly Dirac Nature of Active Neutrinos , JHEP 01 (2017) 072, [ arXiv:1609.04236]

    2017 arXiv

  32. [39]

    Borah and A

    D. Borah and A. Dasgupta, Naturally Light Dirac Neutrino in Left-Right Symmetric Model , JCAP 06 (2017), no. 06 003, [ arXiv:1702.02877]

    2017 arXiv

  33. [40]

    Centelles Chuli´ a, R

    S. Centelles Chuli´ a, R. Srivastava, and J. W. F. Valle,Generalized Bottom-Tau unification, neutrino oscillations and dark matter: predictions from a lepton quarticity flavor approach , Phys. Lett. B 773 (2017) 26–33, [ arXiv:1706.00210]

    2017 arXiv

  34. [41]

    Bonilla, J

    C. Bonilla, J. M. Lamprea, E. Peinado, and J. W. F. Valle, Flavour-symmetric type-II Dirac neutrino seesaw mechanism , Phys. Lett. B 779 (2018) 257–261, [ arXiv:1710.06498]

    2018 arXiv

  35. [42]

    Memenga, W

    N. Memenga, W. Rodejohann, and H. Zhang, A4 flavor symmetry model for Dirac neutrinos and sizable Ue3, Phys. Rev. D 87 (2013), no. 5 053021, [ arXiv:1301.2963]

    2013 arXiv

  36. [43]

    Borah and B

    D. Borah and B. Karmakar, A4 flavour model for Dirac neutrinos: Type I and inverse seesaw, Phys. Lett. B 780 (2018) 461–470, [ arXiv:1712.06407]

    2018 arXiv

  37. [44]

    Centelles Chuli´ a, R

    S. Centelles Chuli´ a, R. Srivastava, and J. W. F. Valle,Seesaw roadmap to neutrino mass and dark matter , Phys. Lett. B 781 (2018) 122–128, [ arXiv:1802.05722]

    2018 arXiv

  38. [45]

    Centelles Chuli´ a, R

    S. Centelles Chuli´ a, R. Srivastava, and J. W. F. Valle,Seesaw Dirac neutrino mass through dimension-six operators, Phys. Rev. D 98 (2018), no. 3 035009, [ arXiv:1804.03181]

    2018 arXiv

  39. [46]

    Han and W

    Z.-L. Han and W. Wang, Z ′ Portal Dark Matter in B − L Scotogenic Dirac Model, arXiv:1805.02025

    arXiv

  40. [47]

    Borah, B

    D. Borah, B. Karmakar, and D. Nanda, Common Origin of Dirac Neutrino Mass and Freeze-in Massive Particle Dark Matter , JCAP 07 (2018) 039, [ arXiv:1805.11115]

    2018 arXiv

  41. [48]

    Borah and B

    D. Borah and B. Karmakar, Linear seesaw for Dirac neutrinos with A4 flavour symmetry , Phys. Lett. B 789 (2019) 59–70, [ arXiv:1806.10685]

    2019 arXiv

  42. [49]

    Borah, D

    D. Borah, D. Nanda, and A. K. Saha, Common origin of modified chaotic inflation, nonthermal dark matter, and Dirac neutrino mass , Phys. Rev. D 101 (2020), no. 7 075006, [arXiv:1904.04840]. – 37 –

    2020 arXiv

  43. [50]

    Centelles Chuli´ a, R

    S. Centelles Chuli´ a, R. Cepedello, E. Peinado, and R. Srivastava, Systematic classification of two loop d = 4 Dirac neutrino mass models and the Diracness-dark matter stability connection, JHEP 10 (2019) 093, [ arXiv:1907.08630]

    2019 arXiv

  44. [51]

    S. Jana, P. K. Vishnu, and S. Saad, Minimal realizations of Dirac neutrino mass from generic one-loop and two-loop topologies at d = 5, JCAP 04 (2020) 018, [arXiv:1910.09537]

    2020 arXiv

  45. [52]

    Nanda and D

    D. Nanda and D. Borah, Connecting Light Dirac Neutrinos to a Multi-component Dark Matter Scenario in Gauged B − L Model, Eur. Phys. J. C 80 (2020), no. 6 557, [arXiv:1911.04703]

    2020 arXiv

  46. [53]

    Guo and Z.-L

    S.-Y. Guo and Z.-L. Han, Observable Signatures of Scotogenic Dirac Model , JHEP 12 (2020) 062, [ arXiv:2005.08287]

    2020 arXiv

  47. [54]

    Bernal, J

    N. Bernal, J. Calle, and D. Restrepo, Anomaly-free Abelian gauge symmetries with Dirac scotogenic models, Phys. Rev. D 103 (2021), no. 9 095032, [ arXiv:2102.06211]

    2021 arXiv

  48. [55]

    Borah, S

    D. Borah, S. Mahapatra, D. Nanda, and N. Sahu, Type II Dirac seesaw with observable ∆Neff in the light of W-mass anomaly , Phys. Lett. B 833 (2022) 137297, [arXiv:2204.08266]

    2022 arXiv

  49. [56]

    Li, X.-Q

    S.-P. Li, X.-Q. Li, X.-S. Yan, and Y.-D. Yang, Scotogenic Dirac neutrino mass models embedded with leptoquarks: one pathway to address the flavor anomalies and the neutrino masses together, Eur. Phys. J. C 82 (2022), no. 11 1078, [ arXiv:2204.09201]

    2022 arXiv

  50. [57]

    Dey and S

    M. Dey and S. Roy, Revisiting the Dirac Nature of Neutrinos , arXiv:2403.12461

    arXiv

  51. [58]

    Singh, M

    L. Singh, M. Kashav, and S. Verma, Minimal type-I Dirac seesaw and leptogenesis under A4 modular invariance , Nucl. Phys. B 1007 (5, 2024) 116666, [ arXiv:2405.07165]

    2024 arXiv

  52. [59]

    Borah, P

    D. Borah, P. Das, B. Karmakar, and S. Mahapatra, Discrete dark matter with light Dirac neutrinos, arXiv:2406.17861

    arXiv

  53. [60]

    K. N. Abazajian and J. Heeck, Observing Dirac neutrinos in the cosmic microwave background, Phys. Rev. D 100 (2019) 075027, [ arXiv:1908.03286]

    2019 arXiv

  54. [61]

    Fileviez P´ erez, C

    P. Fileviez P´ erez, C. Murgui, and A. D. Plascencia, Neutrino-Dark Matter Connections in Gauge Theories, Phys. Rev. D 100 (2019), no. 3 035041, [ arXiv:1905.06344]

    2019 arXiv

  55. [62]

    C. Han, M. L. L´ opez-Ib´ a˜ nez, B. Peng, and J. M. Yang,Dirac dark matter in U (1)B−L with the Stueckelberg mechanism, Nucl. Phys. B 959 (2020) 115154, [ arXiv:2001.04078]

    2020 arXiv

  56. [63]

    X. Luo, W. Rodejohann, and X.-J. Xu, Dirac neutrinos and Neff , JCAP 06 (2020) 058, [arXiv:2005.01629]

    2020 arXiv

  57. [64]

    Borah, A

    D. Borah, A. Dasgupta, C. Majumdar, and D. Nanda, Observing left-right symmetry in the cosmic microwave background, Phys. Rev. D 102 (2020), no. 3 035025, [ arXiv:2005.02343]

    2020 arXiv

  58. [65]

    Adshead, Y

    P. Adshead, Y. Cui, A. J. Long, and M. Shamma, Unraveling the Dirac neutrino with cosmological and terrestrial detectors, Phys. Lett. B 823 (2021) 136736, [arXiv:2009.07852]

    2021 arXiv

  59. [66]

    X. Luo, W. Rodejohann, and X.-J. Xu, Dirac neutrinos and N ef f. Part II. The freeze-in case, JCAP 03 (2021) 082, [ arXiv:2011.13059]

    2021 arXiv

  60. [67]

    Mahanta and D

    D. Mahanta and D. Borah, Low scale Dirac leptogenesis and dark matter with observable ∆Neff , Eur. Phys. J. C 82 (1, 2022) 495, [ arXiv:2101.02092]. – 38 –

    2022 arXiv

  61. [68]

    Du and J.-H

    Y. Du and J.-H. Yu, Neutrino non-standard interactions meet precision measurements of Nef f, JHEP 05 (2021) 058, [ arXiv:2101.10475]

    2021 arXiv

  62. [69]

    Biswas, D

    A. Biswas, D. Borah, and D. Nanda, Light Dirac neutrino portal dark matter with observable ∆Neff, JCAP 10 (3, 2021) 002, [ arXiv:2103.05648]

    2021 arXiv

  63. [70]

    Borah, S

    D. Borah, S. Jyoti Das, and N. Okada, Affleck-Dine cogenesis of baryon and dark matter , JHEP 05 (2023) 004, [ arXiv:2212.04516]

    2023 arXiv

  64. [71]

    Li, X.-Q

    S.-P. Li, X.-Q. Li, X.-S. Yan, and Y.-D. Yang, Cosmological imprints of Dirac neutrinos in a keV-vacuum 2HDM* , Chin. Phys. C 47 (2023), no. 4 043109, [ arXiv:2202.10250]

    2023 arXiv

  65. [72]

    Biswas, D

    A. Biswas, D. K. Ghosh, and D. Nanda, Concealing Dirac neutrinos from cosmic microwave background, JCAP 10 (2022) 006, [ arXiv:2206.13710]

    2022 arXiv

  66. [73]

    Adshead, P

    P. Adshead, P. Ralegankar, and J. Shelton, Dark radiation constraints on portal interactions with hidden sectors , JCAP 09 (2022) 056, [ arXiv:2206.13530]

    2022 arXiv

  67. [74]

    Borah, S

    D. Borah, S. Mahapatra, D. Nanda, S. K. Sahoo, and N. Sahu, Singlet-doublet fermion Dark Matter with Dirac neutrino mass, (g − 2)µ and ∆Nef f, JHEP 05 (2024) 096, [arXiv:2310.03721]

    2024 arXiv

  68. [75]

    Borah, P

    D. Borah, P. Das, and D. Nanda, Observable ∆Neff in Dirac scotogenic model , Eur. Phys. J. C 84 (2024), no. 2 140, [ arXiv:2211.13168]

    2024 arXiv

  69. [76]

    N. Das, S. Jyoti Das, and D. Borah, Thermalized dark radiation in the presence of a PBH: ∆Neff and gravitational waves complementarity , Phys. Rev. D 108 (2023), no. 9 095052, [arXiv:2306.00067]

    2023 arXiv

  70. [77]

    Esseili and G

    H. Esseili and G. D. Kribs, Cosmological implications of gauged U(1) B−L on ∆N ef fin the CMB and BBN , JCAP 05 (2024) 110, [ arXiv:2308.07955]

    2024 arXiv

  71. [78]

    Das and D

    N. Das and D. Borah, Light Dirac neutrino portal dark matter with gauged U(1)B-L symmetry, Phys. Rev. D 109 (2024), no. 7 075045, [ arXiv:2312.06777]

    2024 arXiv

  72. [79]

    Borah, N

    D. Borah, N. Das, S. Jahedi, and B. Thacker, Collider and CMB complementarity of leptophilic dark matter with light Dirac neutrinos , arXiv:2408.14548

  73. [80]

    Barman, D

    B. Barman, D. Borah, A. Dasgupta, and A. Ghoshal, Probing high scale Dirac leptogenesis via gravitational waves from domain walls , Phys. Rev. D 106 (2022), no. 1 015007, [arXiv:2205.03422]

    2022 arXiv

  74. [81]

    Barman, D

    B. Barman, D. Borah, S. Jyoti Das, and I. Saha, Scale of Dirac leptogenesis and left-right symmetry in the light of recent PTA results , JCAP 10 (7, 2023) 053, [ arXiv:2307.00656]

    2023 arXiv

  75. [82]

    Fukugita and T

    M. Fukugita and T. Yanagida, Baryogenesis Without Grand Unification , Phys. Lett. B 174 (1986) 45–47

    1986

  76. [83]

    K. Dick, M. Lindner, M. Ratz, and D. Wright, Leptogenesis with Dirac neutrinos , Phys. Rev. Lett. 84 (2000) 4039–4042, [ hep-ph/9907562]

    2000 arXiv

  77. [84]

    Murayama and A

    H. Murayama and A. Pierce, Realistic Dirac leptogenesis, Phys. Rev. Lett. 89 (2002) 271601, [hep-ph/0206177]

    2002 arXiv

  78. [85]

    Boz and N

    M. Boz and N. K. Pak, Dirac Leptogenesis and anomalous U(1) , Eur. Phys. J. C 37 (2004) 507–510

    2004

  79. [86]

    Thomas and M

    B. Thomas and M. Toharia, Phenomenology of Dirac neutrinogenesis in split supersymmetry, Phys. Rev. D 73 (2006) 063512, [ hep-ph/0511206]. – 39 –

    2006 arXiv

  80. [87]

    Gu and H.-J

    P.-H. Gu and H.-J. He, Neutrino Mass and Baryon Asymmetry from Dirac Seesaw , JCAP 12 (2006) 010, [ hep-ph/0610275]

    2006 arXiv

  81. [88]

    Bechinger and G

    A. Bechinger and G. Seidl, Resonant Dirac leptogenesis on throats , Phys. Rev. D 81 (2010) 065015, [arXiv:0907.4341]

    2010 arXiv

  82. [89]

    M.-C. Chen, J. Huang, and W. Shepherd, Dirac Leptogenesis with a Non-anomalous U (1)′ Family Symmetry, JHEP 11 (2012) 059, [ arXiv:1111.5018]

    2012 arXiv

  83. [90]

    K.-Y. Choi, E. J. Chun, and C. S. Shin, Dark matter asymmetry in supersymmetric Dirac leptogenesis, Phys. Lett. B 723 (2013) 90–94, [ arXiv:1211.5409]

    2013 arXiv

  84. [91]

    Gu, Peccei-Quinn symmetry for Dirac seesaw and leptogenesis , JCAP 07 (2016) 004, [arXiv:1603.05070]

    P.-H. Gu, Peccei-Quinn symmetry for Dirac seesaw and leptogenesis , JCAP 07 (2016) 004, [arXiv:1603.05070]

    2016 arXiv

  85. [92]

    Narendra, N

    N. Narendra, N. Sahoo, and N. Sahu, Dark matter assisted Dirac leptogenesis and neutrino mass, Nucl. Phys. B 936 (2018) 76–90, [ arXiv:1712.02960]

    2018 arXiv

  86. [93]

    Zwicky, Die Rotverschiebung von extragalaktischen Nebeln , Helv

    F. Zwicky, Die Rotverschiebung von extragalaktischen Nebeln , Helv. Phys. Acta 6 (1933) 110–127. [Gen. Rel. Grav.41,207(2009)]

    1933

  87. [94]

    V. C. Rubin and W. K. Ford, Jr., Rotation of the Andromeda Nebula from a Spectroscopic Survey of Emission Regions , Astrophys. J. 159 (1970) 379–403

    1970

  88. [95]

    Clowe, M

    D. Clowe, M. Bradac, A. H. Gonzalez, M. Markevitch, S. W. Randall, C. Jones, and D. Zaritsky, A direct empirical proof of the existence of dark matter , Astrophys. J. Lett. 648 (2006) L109–L113, [ astro-ph/0608407]

    2006 arXiv

  89. [96]

    Aghanim et al

    Planck Collaboration, N. Aghanim et al. , Planck 2018 results. VI. Cosmological parameters, Astron. Astrophys. 641 (2020) A6, [ arXiv:1807.06209]. [Erratum: Astron.Astrophys. 652, C4 (2021)]

    2020 arXiv

  90. [97]

    Arcadi, M

    G. Arcadi, M. Dutra, P. Ghosh, M. Lindner, Y. Mambrini, M. Pierre, S. Profumo, and F. S. Queiroz, The waning of the WIMP? A review of models, searches, and constraints , Eur. Phys. J. C 78 (2018), no. 3 203, [ arXiv:1703.07364]

    2018 arXiv

  91. [98]

    Arcadi, D

    G. Arcadi, D. Cabo-Almeida, M. Dutra, P. Ghosh, M. Lindner, Y. Mambrini, J. P. Neto, M. Pierre, S. Profumo, and F. S. Queiroz, The Waning of the WIMP: Endgame? , arXiv:2403.15860

    arXiv

  92. [99]

    Aalbers et al

    LZ Collaboration, J. Aalbers et al. , First Dark Matter Search Results from the LUX-ZEPLIN (LZ) Experiment , Phys. Rev. Lett. 131 (2023), no. 4 041002, [arXiv:2207.03764]

    2023 arXiv

  93. [100]

    Craig, Naturalness: past, present, and future , Eur

    N. Craig, Naturalness: past, present, and future , Eur. Phys. J. C 83 (2023), no. 9 825, [arXiv:2205.05708]

    2023 arXiv

  94. [101]

    Wu, K.-P

    Y. Wu, K.-P. Xie, and Y.-L. Zhou, Classification of Abelian domain walls , Phys. Rev. D 106 (2022), no. 7 075019, [ arXiv:2205.11529]

    2022 arXiv

  95. [102]

    Coito, C

    L. Coito, C. Faubel, J. Herrero-Garcia, and A. Santamaria, Dark matter from a complex scalar singlet: the role of dark CP and other discrete symmetries , JHEP 11 (2021) 202, [arXiv:2106.05289]

    2021 arXiv

  96. [103]

    H. T. Pham and E. Senaha, Gravitational waves from domain wall collapses and dark matter in the SM with a complex scalar , arXiv:2403.16568

    arXiv

  97. [104]

    Sakurai and W

    K. Sakurai and W. Yin, Phenomenology of CP-even ALP , JHEP 04 (2022) 113, [arXiv:2111.03653]. – 40 –

    2022 arXiv

  98. [105]

    M. E. Peskin and T. Takeuchi, A New constraint on a strongly interacting Higgs sector , Phys. Rev. Lett. 65 (1990) 964–967

    1990

  99. [106]

    M. E. Peskin and T. Takeuchi, Estimation of oblique electroweak corrections , Phys. Rev. D 46 (1992) 381–409

    1992

  100. [107]

    D. C. Kennedy and P. Langacker, Precision electroweak experiments and heavy physics: A Global analysis, Phys. Rev. Lett. 65 (1990) 2967–2970. [Erratum: Phys.Rev.Lett. 66, 395 (1991)]

    1990

  101. [108]

    T. Han, D. Marfatia, and R.-J. Zhang, Oblique parameter constraints on large extra dimensions, Phys. Rev. D 62 (2000) 125018, [ hep-ph/0001320]

    2000 arXiv

  102. [109]

    Porod, SPheno, a program for calculating supersymmetric spectra, SUSY particle decays and SUSY particle production at e+ e- colliders , Comput

    W. Porod, SPheno, a program for calculating supersymmetric spectra, SUSY particle decays and SUSY particle production at e+ e- colliders , Comput. Phys. Commun. 153 (2003) 275–315, [hep-ph/0301101]

    2003 arXiv

  103. [110]

    Thomas and M

    B. Thomas and M. Toharia, Lepton flavor violation and supersymmetric Dirac leptogenesis , Phys. Rev. D 75 (2007) 013013, [ hep-ph/0607285]

    2007 arXiv

  104. [111]

    D. G. Cerdeno, A. Dedes, and T. E. J. Underwood, The Minimal Phantom Sector of the Standard Model: Higgs Phenomenology and Dirac Leptogenesis , JHEP 09 (2006) 067, [hep-ph/0607157]

    2006 arXiv

  105. [112]

    Gu, H.-J

    P.-H. Gu, H.-J. He, and U. Sarkar, Realistic neutrinogenesis with radiative vertex correction, Phys. Lett. B 659 (2008) 634–639, [ arXiv:0709.1019]

    2008 arXiv

  106. [113]

    E. J. Chun and P. Roy, Dirac Leptogenesis in extended nMSSM , JHEP 06 (2008) 089, [arXiv:0803.1720]

    2008 arXiv

  107. [114]

    K. S. Babu and A. Kaladharan, Dirac Leptogenesis in Left-Right Symmetric Models , arXiv:2410.24125

    arXiv

  108. [115]

    Heeck, Leptogenesis with Lepton-Number-Violating Dirac Neutrinos , Phys

    J. Heeck, Leptogenesis with Lepton-Number-Violating Dirac Neutrinos , Phys. Rev. D 88 (2013) 076004, [ arXiv:1307.2241]

    2013 arXiv

  109. [116]

    Gu, Leptogenesis with testable Dirac neutrino mass generation , Phys

    P.-H. Gu, Leptogenesis with testable Dirac neutrino mass generation , Phys. Lett. B 805 (2020) 135411, [ arXiv:1907.09443]

    2020 arXiv

  110. [117]

    J. A. Casas and A. Ibarra, Oscillating neutrinos and µ → e, γ, Nucl. Phys. B 618 (2001) 171–204, [hep-ph/0103065]

    2001 arXiv

  111. [118]

    Esteban, M

    I. Esteban, M. C. Gonzalez-Garcia, M. Maltoni, I. Martinez-Soler, J. a. P. Pinheiro, and T. Schwetz, NuFit-6.0: updated global analysis of three-flavor neutrino oscillations , JHEP 12 (2024) 216, [ arXiv:2410.05380]

    2024 arXiv

  112. [119]

    Buchmuller, P

    W. Buchmuller, P. Di Bari, and M. Plumacher, Leptogenesis for pedestrians, Annals Phys. 315 (2005) 305–351, [ hep-ph/0401240]

    2005 arXiv

  113. [120]

    Davidson and A

    S. Davidson and A. Ibarra, A Lower bound on the right-handed neutrino mass from leptogenesis, Phys. Lett. B 535 (2002) 25–32, [ hep-ph/0202239]

    2002 arXiv

  114. [121]

    Degrassi, S

    G. Degrassi, S. Di Vita, J. Elias-Miro, J. R. Espinosa, G. F. Giudice, G. Isidori, and A. Strumia, Higgs mass and vacuum stability in the Standard Model at NNLO , JHEP 08 (2012) 098, [ arXiv:1205.6497]

    2012 arXiv

  115. [122]

    Gonderinger, Y

    M. Gonderinger, Y. Li, H. Patel, and M. J. Ramsey-Musolf, Vacuum Stability, Perturbativity, and Scalar Singlet Dark Matter , JHEP 01 (2010) 053, [ arXiv:0910.3167]. – 41 –

    2010 arXiv

  116. [123]

    Gondolo and G

    P. Gondolo and G. Gelmini, Cosmic abundances of stable particles: Improved analysis , Nucl. Phys. B360 (1991) 145–179

    1991

  117. [124]

    Duerr, P

    M. Duerr, P. Fileviez P´ erez, and J. Smirnov, Scalar Dark Matter: Direct vs. Indirect Detection, JHEP 06 (2016) 152, [ arXiv:1509.04282]

    2016 arXiv

  118. [125]

    Binder, T

    T. Binder, T. Bringmann, M. Gustafsson, and A. Hryczuk, Dark matter relic abundance beyond kinetic equilibrium , Eur. Phys. J. C 81 (2021) 577, [ arXiv:2103.01944]

    2021 arXiv

  119. [126]

    Staub, Exploring new models in all detail with SARAH , Adv

    F. Staub, Exploring new models in all detail with SARAH , Adv. High Energy Phys. 2015 (2015) 840780, [ arXiv:1503.04200]

    2015 arXiv

  120. [127]

    Belyaev, N

    A. Belyaev, N. D. Christensen, and A. Pukhov, CalcHEP 3.4 for collider physics within and beyond the Standard Model , Comput. Phys. Commun. 184 (2013) 1729–1769, [arXiv:1207.6082]

    2013 arXiv

  121. [128]

    Belanger, F

    G. Belanger, F. Boudjema, and A. Pukhov, micrOMEGAs : a code for the calculation of Dark Matter properties in generic models of particle interaction , in Theoretical Advanced Study Institute in Elementary Particle Physics: The Dark Secrets of the Terascale , pp. 739–790, 2013....

    2013 arXiv

  122. [129]

    Aprile et al

    XENON Collaboration, E. Aprile et al. , Dark Matter Search Results from a One Ton-Year Exposure of XENON1T , Phys. Rev. Lett. 121 (2018), no. 11 111302, [ arXiv:1805.12562]

    2018 arXiv

  123. [130]

    Aprile et al

    XENON Collaboration, E. Aprile et al. , Projected WIMP sensitivity of the XENONnT dark matter experiment , JCAP 11 (2020) 031, [ arXiv:2007.08796]

    2020 arXiv

  124. [131]

    M. W. Goodman and E. Witten, Detectability of Certain Dark Matter Candidates , Phys. Rev. D 31 (1985) 3059

    1985

  125. [132]

    Conrad, Indirect Detection of WIMP Dark Matter: a compact review , in Interplay between Particle and Astroparticle physics , 11, 2014

    J. Conrad, Indirect Detection of WIMP Dark Matter: a compact review , in Interplay between Particle and Astroparticle physics , 11, 2014. arXiv:1411.1925

    2014 arXiv

  126. [133]

    Acero et al

    F ermi-LA TCollaboration, F. Acero et al. , Fermi Large Area Telescope Third Source Catalog, Astrophys. J. Suppl. 218 (2015), no. 2 23, [ arXiv:1501.02003]

    2015 arXiv

  127. [134]

    Ackermann et al

    F ermi-LA TCollaboration, M. Ackermann et al. , Updated search for spectral lines from Galactic dark matter interactions with pass 8 data from the Fermi Large Area Telescope , Phys. Rev. D 91 (2015), no. 12 122002, [ arXiv:1506.00013]

    2015 arXiv

  128. [135]

    J. W. Foster, Y. Park, B. R. Safdi, Y. Soreq, and W. L. Xu, Search for dark matter lines at the Galactic Center with 14 years of Fermi data , Phys. Rev. D 107 (2023), no. 10 103047, [arXiv:2212.07435]

    2023 arXiv

  129. [136]

    Collaboration, H

    H.E.S.S. Collaboration, H. Abdallah et al. , Search for dark matter annihilations towards the inner Galactic halo from 10 years of observations with H.E.S.S , Phys. Rev. Lett. 117 (2016), no. 11 111301, [ arXiv:1607.08142]

    2016 arXiv

  130. [137]

    Abdallah et al

    HESS Collaboration, H. Abdallah et al. , Search for γ-Ray Line Signals from Dark Matter Annihilations in the Inner Galactic Halo from 10 Years of Observations with H.E.S.S. , Phys. Rev. Lett. 120 (2018), no. 20 201101, [ arXiv:1805.05741]

    2018 arXiv

  131. [138]

    CT A ConsortiumCollaboration, B. S. Acharya et al. , Science with the Cherenkov Telescope Array. WSP, 11, 2018

    2018

  132. [139]

    Abe et al

    CT AOCollaboration, S. Abe et al. , Dark matter line searches with the Cherenkov Telescope Array, JCAP 07 (2024) 047, [ arXiv:2403.04857]. – 42 –

    2024 arXiv

  133. [140]

    Ackermann et al

    F ermi-LA TCollaboration, M. Ackermann et al. , Constraining Dark Matter Models from a Combined Analysis of Milky Way Satellites with the Fermi Large Area Telescope , Phys. Rev. Lett. 107 (2011) 241302, [ arXiv:1108.3546]

    2011 arXiv

  134. [141]

    Y. B. Zeldovich, I. Y. Kobzarev, and L. B. Okun, Cosmological Consequences of the Spontaneous Breakdown of Discrete Symmetry , Zh. Eksp. Teor. Fiz. 67 (1974) 3–11

    1974

  135. [142]

    T. W. B. Kibble, Topology of Cosmic Domains and Strings , J. Phys. A 9 (1976) 1387–1398

    1976

  136. [143]

    Vilenkin, Gravitational Field of Vacuum Domain Walls and Strings , Phys

    A. Vilenkin, Gravitational Field of Vacuum Domain Walls and Strings , Phys. Rev. D 23 (1981) 852–857

    1981

  137. [144]

    Coulson, Z

    D. Coulson, Z. Lalak, and B. A. Ovrut, Biased domain walls , Phys. Rev. D 53 (1996) 4237–4246

    1996

  138. [145]

    Krajewski, J

    T. Krajewski, J. H. Kwapisz, Z. Lalak, and M. Lewicki, Stability of domain walls in models with asymmetric potentials , Phys. Rev. D 104 (2021), no. 12 123522, [ arXiv:2103.03225]

    2021 arXiv

  139. [146]

    Z. A. Borboruah and U. A. Yajnik, Left-right symmetry breaking and gravitational waves: A tale of two phase transitions , Phys. Rev. D 110 (2024), no. 4 043016, [ arXiv:2212.05829]

    2024 arXiv

  140. [147]

    U. A. Yajnik, H. Widyan, D. Choudhari, S. Mahajan, and A. Mukherjee, Topological defects in the left-right symmetric model and their relevance to cosmology , Phys. Rev. D 59 (1999) 103508, [hep-ph/9812406]

    1999 arXiv

  141. [148]

    Hiramatsu, M

    T. Hiramatsu, M. Kawasaki, K. Saikawa, and T. Sekiguchi, Axion cosmology with long-lived domain walls , JCAP 01 (2013) 001, [ arXiv:1207.3166]

    2013 arXiv

  142. [149]

    Borah and A

    D. Borah and A. Dasgupta, Probing left-right symmetry via gravitational waves from domain walls , Phys. Rev. D 106 (2022), no. 3 035016, [ arXiv:2205.12220]

    2022 arXiv

  143. [150]

    Sikivie, Of Axions, Domain Walls and the Early Universe , Phys

    P. Sikivie, Of Axions, Domain Walls and the Early Universe , Phys. Rev. Lett. 48 (1982) 1156–1159

    1982

  144. [151]

    G. B. Gelmini, M. Gleiser, and E. W. Kolb, Cosmology of Biased Discrete Symmetry Breaking, Phys. Rev. D 39 (1989) 1558

    1989

  145. [152]

    S. E. Larsson, S. Sarkar, and P. L. White, Evading the cosmological domain wall problem , Phys. Rev. D 55 (1997) 5129–5135, [ hep-ph/9608319]

    1997 arXiv

  146. [153]

    Bai, T.-K

    Y. Bai, T.-K. Chen, and M. Korwar, QCD-collapsed domain walls: QCD phase transition and gravitational wave spectroscopy, JHEP 12 (6, 2023) 194, [ arXiv:2306.17160]

    2023 arXiv

  147. [154]

    Kallosh, A

    R. Kallosh, A. D. Linde, D. A. Linde, and L. Susskind, Gravity and global symmetries , Phys. Rev. D 52 (1995) 912–935, [ hep-th/9502069]

    1995 arXiv

  148. [155]

    Witten, Symmetry and Emergence , Nature Phys

    E. Witten, Symmetry and Emergence , Nature Phys. 14 (2018), no. 2 116–119, [arXiv:1710.01791]

    2018 arXiv

  149. [156]

    Rai and G

    B. Rai and G. Senjanovic, Gravity and domain wall problem , Phys. Rev. D 49 (1994) 2729–2733, [hep-ph/9301240]

    1994 arXiv

  150. [157]

    S. F. King, R. Roshan, X. Wang, G. White, and M. Yamazaki, Quantum gravity effects on dark matter and gravitational waves , Phys. Rev. D 109 (8, 2024) 024057, [arXiv:2308.03724]

    2024 arXiv

  151. [158]

    S. F. King, R. Roshan, X. Wang, G. White, and M. Yamazaki, Quantum Gravity Effects on Fermionic Dark Matter and Gravitational Waves , arXiv:2311.12487. – 43 –

    arXiv

  152. [159]

    Borah, N

    D. Borah, N. Das, and R. Roshan, Observable gravitational waves and ∆Neff with global lepton number symmetry and dark matter , Phys. Rev. D 110 (6, 2024) 075042, [arXiv:2406.04404]

    2024 arXiv

  153. [160]

    Gouttenoire, S

    Y. Gouttenoire, S. F. King, R. Roshan, X. Wang, G. White, and M. Yamazaki, Cosmological Consequences of Domain Walls Biased by Quantum Gravity , arXiv:2501.16414

  154. [161]

    S. M. Barr and D. Seckel, Planck scale corrections to axion models , Phys. Rev. D 46 (1992) 539–549

    1992

  155. [162]

    A. G. Dias, V. Pleitez, and M. D. Tonasse, Naturally light invisible axion in models with large local discrete symmetries , Phys. Rev. D 67 (2003) 095008, [ hep-ph/0211107]

    2003 arXiv

  156. [163]

    L. M. Carpenter, M. Dine, and G. Festuccia, Dynamics of the Peccei Quinn Scale , Phys. Rev. D 80 (2009) 125017, [ arXiv:0906.1273]

    2009 arXiv

  157. [164]

    Hiramatsu, M

    T. Hiramatsu, M. Kawasaki, and K. Saikawa, Gravitational Waves from Collapsing Domain Walls, JCAP 05 (2010) 032, [ arXiv:1002.1555]

    2010 arXiv

  158. [166]

    Kadota, M

    K. Kadota, M. Kawasaki, and K. Saikawa, Gravitational waves from domain walls in the next-to-minimal supersymmetric standard model , JCAP 10 (2015) 041, [arXiv:1503.06998]

    2015 arXiv

  159. [167]

    A. Paul, U. Mukhopadhyay, and D. Majumdar, Gravitational Wave Signatures from Domain Wall and Strong First-Order Phase Transitions in a Two Complex Scalar extension of the Standard Model , JHEP 05 (10, 2021) 223, [ arXiv:2010.03439]

    2021 arXiv

  160. [168]

    Maggiore, Gravitational wave experiments and early universe cosmology , Phys

    M. Maggiore, Gravitational wave experiments and early universe cosmology , Phys. Rept. 331 (2000) 283–367, [ gr-qc/9909001]

    2000 arXiv

  161. [169]

    R. H. Cyburt, B. D. Fields, K. A. Olive, and T.-H. Yeh, Big Bang Nucleosynthesis: 2015 , Rev. Mod. Phys. 88 (2016) 015004, [ arXiv:1505.01076]

    2016 arXiv

  162. [170]

    Aiola et al

    CMB-HD Collaboration, S. Aiola et al. , Snowmass2021 CMB-HD White Paper , arXiv:2203.05728

    arXiv

  163. [171]

    CMB-Bharat Collaboration Collaboration, C.-B. A. I. C. Consortium, Exploring Cosmic History and Origin: A proposal for a next generation space mission for near-ultimate measurements of the Cosmic Microwave Background (CMB) polarization and discovery of global CMB spectral dist...

  164. [172]

    K. N. Abazajian and M. Kaplinghat, Neutrino physics from the cosmic microwave background and large-scale structure, Annual Review of Nuclear and Particle Science 66 (2016), no. 1 401–420, [ https://doi.org/10.1146/annurev-nucl-102014-021908]

    2016 doi

  165. [173]

    Alvarez et al

    M. Alvarez et al. , PICO: Probe of Inflation and Cosmic Origins , Bull. Am. Astron. Soc. 51 (2019), no. 7 194, [ arXiv:1908.07495]

    2019 arXiv

  166. [174]

    Delabrouille et al

    CORE Collaboration, J. Delabrouille et al. , Exploring cosmic origins with CORE: Survey requirements and mission design , JCAP 04 (2018) 014, [ arXiv:1706.04516]

    2018 arXiv

  167. [175]

    SPT-3G Collaboration, B. A. Benson et al. , SPT-3G: A Next-Generation Cosmic Microwave Background Polarization Experiment on the South Pole Telescope , Proc. SPIE Int. Soc. Opt. Eng. 9153 (2014) 91531P, [arXiv:1407.2973]. – 44 –

    2014 arXiv

  168. [176]

    Ade et al

    Simons ObservatoryCollaboration, P. Ade et al. , The Simons Observatory: Science goals and forecasts, JCAP 02 (2019) 056, [ arXiv:1808.07445]

    2019 arXiv

  169. [177]

    Yagi and N

    K. Yagi and N. Seto, Detector configuration of DECIGO/BBO and identification of cosmological neutron-star binaries, Phys. Rev. D 83 (2011) 044011, [ arXiv:1101.3940]. [Erratum: Phys.Rev.D 95, 109901 (2017)]

    2011 arXiv

  170. [178]

    Amaro-Seoane et al, Laser Interferometer Space Antenna, arXiv e-prints (feb, 2017) arXiv:1702.00786, [ arXiv:1702.00786]

    LISA Collaboration, P. Amaro-Seoane et al, Laser Interferometer Space Antenna, arXiv e-prints (feb, 2017) arXiv:1702.00786, [ arXiv:1702.00786]

    2017 arXiv

  171. [179]

    Punturo et al, The einstein telescope: a third-generation gravitational wave observatory , Classical and Quantum Gravity 27 (sep,

    ET Collaboration Collaboration, M. Punturo et al, The einstein telescope: a third-generation gravitational wave observatory , Classical and Quantum Gravity 27 (sep,

  172. [180]

    Garcia-Bellido, H

    J. Garcia-Bellido, H. Murayama, and G. White, Exploring the early Universe with Gaia and Theia, JCAP 12 (4, 2021) 023, [ arXiv:2104.04778]

    2021 arXiv

  173. [181]

    Sesana et al

    A. Sesana et al. , Unveiling the gravitational universe at µ-Hz frequencies, Exper. Astron. 51 (2021), no. 3 1333–1383, [ arXiv:1908.11391]

    2021 arXiv

  174. [182]

    Antoniadis et al

    J. Antoniadis et al. , The second data release from the European Pulsar Timing Array III. Search for gravitational wave signals , arXiv:2306.16214

    arXiv

  175. [183]

    Weltman et al

    A. Weltman et al. , Fundamental physics with the Square Kilometre Array , Publ. Astron. Soc. Austral. 37 (2020) e002, [ arXiv:1810.02680]

    2020 arXiv

  176. [184]

    Agazie et al

    NANOGrav Collaboration, G. Agazie et al. , The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background , Astrophys. J. Lett. 951 (2023), no. 1 L8, [arXiv:2306.16213]

    2023 arXiv

  177. [185]

    Kogut et al

    A. Kogut et al. , The Primordial Inflation Explorer (PIXIE): Mission Design and Science Goals, arXiv:2405.20403

    arXiv

  178. [186]

    Basu et al

    K. Basu et al. , A space mission to map the entire observable universe using the CMB as a backlight: Voyage 2050 science white paper , Exper. Astron. 51 (2021), no. 3 1555–1591, [arXiv:1909.01592]

    2021

  179. [187]

    Kitajima, J

    N. Kitajima, J. Lee, K. Murai, F. Takahashi, and W. Yin, Gravitational waves from domain wall collapse, and application to nanohertz signals with QCD-coupled axions , Phys. Lett. B 851 (6, 2024) 138586, [ arXiv:2306.17146]

    2024 arXiv

  180. [188]

    R. Z. Ferreira, S. Gasparotto, T. Hiramatsu, I. Obata, and O. Pujolas, Axionic defects in the CMB: birefringence and gravitational waves , JCAP 05 (2024) 066, [arXiv:2312.14104]

    2024 arXiv

  181. [189]

    Dankovsky, E

    I. Dankovsky, E. Babichev, D. Gorbunov, S. Ramazanov, and A. Vikman, Revisiting evolution of domain walls and their gravitational radiation with CosmoLattice , JCAP 09 (2024) 047, [ arXiv:2406.17053]

    2024 arXiv

  182. [190]

    D. I. Dunsky, A. Ghoshal, H. Murayama, Y. Sakakihara, and G. White, Gravitational Wave Gastronomy, Phys. Rev. D 106 (11, 2021) 075030, [ arXiv:2111.08750]

    2021 arXiv

  183. [191]

    Schmitz, New Sensitivity Curves for Gravitational-Wave Signals from Cosmological Phase Transitions, JHEP 01 (2, 2021) 097, [ arXiv:2002.04615]

    K. Schmitz, New Sensitivity Curves for Gravitational-Wave Signals from Cosmological Phase Transitions, JHEP 01 (2, 2021) 097, [ arXiv:2002.04615]

    2021 arXiv

  184. [192]

    Heeck, J

    J. Heeck, J. Heisig, and A. Thapa, Testing Dirac leptogenesis with the cosmic microwave background and proton decay, Phys. Rev. D 108 (2023), no. 3 035014, [ arXiv:2304.09893]

    2023 arXiv

  185. [193]

    Griest and M

    K. Griest and M. Kamionkowski, Unitarity Limits on the Mass and Radius of Dark Matter Particles, Phys. Rev. Lett. 64 (1990) 615. – 45 –

    1990

  186. [194]

    Hattori, T

    H. Hattori, T. Kobayashi, N. Omoto, and O. Seto, Entropy production by domain wall decay in the NMSSM , Phys. Rev. D 92 (2015), no. 10 103518, [ arXiv:1510.03595]

    2015 arXiv

  187. [195]

    Kawasaki and F

    M. Kawasaki and F. Takahashi, Late-time entropy production due to the decay of domain walls, Phys. Lett. B 618 (2005) 1–6, [ hep-ph/0410158]

    2005 arXiv

  188. [196]

    Sato et al

    S. Sato et al. , The status of DECIGO , J. Phys. Conf. Ser. 840 (2017), no. 1 012010

    2017

  189. [197]

    Ishikawa et al

    T. Ishikawa et al. , Improvement of the target sensitivity in DECIGO by optimizing its parameters for quantum noise including the effect of diffraction loss , Galaxies 9 (2021), no. 1 14, [ arXiv:2012.11859]

    2021 arXiv

  190. [198]

    Kannike, Vacuum Stability Conditions From Copositivity Criteria , Eur

    K. Kannike, Vacuum Stability Conditions From Copositivity Criteria , Eur. Phys. J. C 72 (2012) 2093, [ arXiv:1205.3781]

    2012 arXiv

  191. [199]

    Antusch, J

    S. Antusch, J. Kersten, M. Lindner, and M. Ratz, Neutrino mass matrix running for nondegenerate seesaw scales, Phys. Lett. B 538 (2002) 87–95, [ hep-ph/0203233]

    2002 arXiv

  192. [200]

    Brdar, A

    V. Brdar, A. J. Helmboldt, S. Iwamoto, and K. Schmitz, Type-I Seesaw as the Common Origin of Neutrino Mass, Baryon Asymmetry, and the Electroweak Scale , Phys. Rev. D 100 (2019) 075029, [ arXiv:1905.12634]. – 46 –

    2019 arXiv

Pith tools

Reviewed August 11, 2026 · model on record in the stance chip above.