Pith. sign in

REVIEW 3 major objections 3 minor 134 references

Flavoured leptogenesis and ${\rm CP}^{\mu\tau}$ symmetry

T0 review · 3 major / 3 minor · reviewed 2026-08-14 · deepseek-v4-flash

Pith's one-line read In a CP$\mu\tau$-symmetric minimal seesaw model, the observed baryon asymmetry can be produced with a right-handed neutrino mass hierarchy as mild as $M_2/M_1 \simeq 4.7$, lowering the lightest mass bound to about $7.5\times 10^9$ GeV.

desk verdict Relaxing the strong hierarchy in CPμτ leptogenesis is a genuine extension, and the numbers are usable as estimates, but the decoherence-derived upper bound and scan fractions need verification before being treated as precise. read the letter →

arxiv 1908.08126 v2 pith:2VFRYY5L submitted 2019-08-21 hep-ph

classification hep-ph
keywords leptogenesisCPmu-tausymmetryreflectionminimalseesawtworight-handedneutrinosflavouredN2baryonasymmetry
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 asks whether the CP$\mu\tau$-symmetric minimal seesaw model, a neutrino mass model with a $\mu$-$\tau$ exchanging CP symmetry, can account for the observed baryon asymmetry using only two right-handed neutrinos once realistic flavour effects are included. The authors establish that the heavy neutrino mass hierarchy need not be extreme: a ratio as mild as $M_2/M_1 \simeq 4.7$ still supports a standard $N_1$-dominated leptogenesis scenario, lowering the lower bound on the lightest right-handed mass from about $6\times 10^{10}$ GeV to about $7.5\times 10^{9}$ GeV. They further show that $N_1$-domination is confined to a window $7.5\times 10^{9}\,\mathrm{GeV} < M_1 < 4\times 10^{10}\,\mathrm{GeV}$, fixed by tau-lepton flavoured decoherence, and that beyond this window the second right-handed neutrino $N_2$ can dominate the final asymmetry over a substantial fraction of the parameter space. When $N_2$ produces the asymmetry in the two-flavour regime and $N_1$ washes it out in the three-flavour regime, the surviving asymmetry is essentially electron-flavoured, and roughly 33% of the parameter space is consistent with pure $N_2$ leptogenesis.

What carries the argument

The argument is carried by the CP$\mu\tau$ ($\mu\tau$-reflection) symmetry acting on the neutrino mass Lagrangian, which forces the flavoured CP asymmetries to satisfy $\varepsilon_{ie} = 0$ and $\varepsilon_{i\mu} = -\varepsilon_{i\tau}$ while the total unflavoured asymmetry vanishes. Within the minimal two-right-handed-neutrino seesaw, three ingredients do the quantitative work: the flavoured decay parameters $K_{i\alpha}$, which set the washout strength in each flavour; the overlap probability $p_{12}$ (the squared projection of the $N_2$ lepton state onto the $N_1$ lepton state in the $\tau$-perpendicular plane, never equal to unity in this model because the two heavy states define different $\tau^\perp$ directions); and the decoherence condition $F_\tau = \Gamma_\tau/(2Hz) > W(z)$, which fixes the upper end of the $N_1$ mass window.

What would settle it

Compute the full density-matrix (quantum-kinetic) leptogenesis equations, including off-diagonal flavour coherence, for a point inside the claimed window (e.g., $M_1 = 10^{10}$ GeV with $M_2/M_1 = 4.7$ and $K_{1\tau} \approx K_{2\tau} \approx 5$); if the resulting baryon-to-photon ratio differs from the flavour-projected Boltzmann result by more than an order-one factor, the window is invalid. Alternatively, a future neutrinoless double-$\beta$ decay measurement finding $|(M_\nu)_{\beta\beta}|$ outside the model's required 3–5 meV range would exclude the parameter space that underlies all of these results.

Watch

Extended reading notes

Core claim

This paper's central claim is that in the CP$\mu\tau$ ($\mu\tau$-reflection) symmetric two-right-handed-neutrino seesaw model, flavoured leptogenesis works across a much wider region of parameter space than earlier analyses concluded. In the two-flavour regime, the heavy neutrino masses can be mildly hierarchical, $M_2 \simeq 4.7 M_1$, and still realize a perfectly hierarchical $N_1$-dominated scenario; the loop-function enhancement of the CP asymmetry at this mild hierarchy lowers the minimal allowed $M_1$ to about $7.5\times 10^{9}$ GeV. $N_1$-domination is valid only for $7.5\times 10^{9}\,\mathrm{GeV} \lesssim M_1 \lesssim 4\times 10^{10}\,\mathrm{GeV}$, with the upper bound set by the requirement that $\tau$ charged-lepton interactions decohere the lepton flavour states before the washout rates peak; beyond this window, about 26% of the parameter space favours $N_2$-domination while 37% favours $N_1$-domination. When $M_2$ lies in the two-flavour regime and $M_1$ in the three-flavour regime, the asymmetry produced by $N_2$ is essentially erased by $N_1$ in the $\mu$ and $\tau$ flavours, leaving the electron flavour as the only survivor, with the probability of survival (quantified by $K_{1e} < 1$) around 33%.

Load-bearing premise

The upper bound on $M_1$ (and hence the quoted domination fractions) rests on the condition that the $\tau$ charged-lepton interaction rate exceeds every relevant washout rate throughout the asymmetry epoch ($F_\tau > W$ at the relevant $z$); if this decoherence condition fails, the full quantum-kinetic density-matrix treatment is needed and the mass window and fractions could shift.

Editorial extensions

If this is right

  • The lower bound on $M_1$ drops by roughly an order of magnitude, so CP$\mu\tau$ models can be compatible with reheating temperatures around $10^{10}$ GeV rather than requiring $M_1 \gtrsim 6\times 10^{10}$ GeV.
  • A pure $N_1$-dominated analysis that assumes strong hierarchy ($M_2/M_1 = 10^3$) is not generally valid inside the allowed window, since $1-p_{12}$ never vanishes and $N_2$ dominates the final asymmetry for about 26% of the parameter space.
  • When $M_1 < 10^9$ GeV and $M_2$ is in the two-flavour regime, the surviving asymmetry is electron-flavoured; a pure $N_2$ leptogenesis signal would then be a single-flavour asymmetry, with the other flavours erased by $N_1$ washout.
  • The decoherence condition $F_\tau > W$ pins down a concrete scale, $M_1 \lesssim 4\times 10^{10}$ GeV, above which either $N_2$ contributions become relevant or the flavour-projected Boltzmann approach must be replaced by a density-matrix treatment.

Reading between the lines

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

  • The same flavour-survival logic applies to any pre-existing electron-flavour asymmetry: in the low-$M_1$ spectrum, a high-scale source of $e$-flavour lepton asymmetry would also evade $N_1$ washout, a possibility the paper sets aside by assuming no pre-existing asymmetry.
  • The claimed window is computed in the rate-equation (flavour-projected) approximation; a full quantum-kinetic computation could shift $M_{\rm max}$ and the 26%/37% fractions, so those percentages should be read as the rate-approximation estimate rather than exact model predictions.
  • The mild-hierarchy result depends on the loop-function enhancement in $g_1(x_{12})$; variants of CP$\mu\tau$ with additional right-handed neutrinos (or with a differently charged-lepton sector) would modify the allowed mass window, making the 33% electron-flavour survival fraction a useful discriminator between symmetry variants.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 3 minor

Summary. This paper studies thermal flavoured leptogenesis in the minimal two-right-handed-neutrino seesaw with CP^{μτ} symmetry. The authors use analytic efficiency factors, validated against explicit one-flavour Boltzmann solutions, and scan the CP^{μτ} parameter space constrained by neutrino oscillation data. They claim three main results: (i) a mild hierarchy M2/M1 ≈ 4.7 is sufficient for a hierarchical N1-dominated scenario, lowering the lower bound on M1 to about 7.5 × 10^9 GeV; (ii) in the two-flavour regime the N1-dominated scenario is valid only for 7.5 × 10^9 GeV ≲ M1 ≲ 4 × 10^10 GeV, with N2 domination possible for a substantial part of the parameter space above the upper bound; and (iii) if M1 lies in the three-flavour regime, an asymmetry produced by N2 in the two-flavour regime survives N1 washout mainly in the electron flavour, with about 33% probability for a hierarchical light neutrino spectrum.

Significance. If the claims are correct, the paper is significant: it extends leptogenesis studies of CP^{μτ} models beyond the strong-hierarchy limit, identifies a specific RH neutrino mass window, and quantifies the conditions under which N2 contributions matter. The paper is commendable for the explicit one-flavour Boltzmann check of the analytic efficiency factors and for the transparent parameter scan tied to oscillation data. The main caveats are the semi-classical decoherence criterion used to set the upper bound M_max and the ad hoc introduction of N3 in the three-flavour-regime scenario without a corresponding refit of the light-neutrino parameter space; these points need to be addressed before the central quantitative claims can be considered fully established.

major comments (3)
  1. [Sec. V.A, Eq. (V.10)] The upper bound M_max ≈ 4 × 10^10 GeV is set by the condition F_τ = Γ_τ/(2Hz_i) > W(z_i^max), where W is a single scalar washout rate. The two-flavour regime is a density-matrix problem with flavour off-diagonal coherence terms, as the paper itself notes in footnote 11, and the rate comparison in Eq. (V.10) does not by itself establish the decoherence of those off-diagonal terms. Because the quoted mass window and the N1/N2 dominance percentages in Section V.A rest on this criterion, the upper bound should be checked with a full quantum-kinetic calculation for representative parameter points or with a quantitative estimate of the error incurred by the rate comparison; otherwise the window 7.5 × 10^9 GeV < M1 < 4 × 10^10 GeV is not rigorously delimited.
  2. [Sec. V.B, footnote 14] The M1 < 10^9 GeV scenario requires adding a third right-handed neutrino N3 with M3 > 10^12 GeV and Yukawa couplings 'of similar order of magnitude' to N1 and N2, but the light-neutrino parameter scan and the K_{1α} distributions in Fig. 13 are computed from the two-RHN mass matrix without N3. If y3 ~ y2 and M3 ~ 10^12 GeV, the N3 contribution to M_ν is of order 10^-4 eV for K ~ 20 and M2 ~ 10^10 GeV, which is a few percent of the solar mass scale and not manifestly negligible for the 3σ fit. The authors should demonstrate that the N3 contribution is below the fit sensitivity or repeat the scan with N3 included; otherwise the central 33% survival probability is not the probability in the stated model.
  3. [Sec. V.A, Fig. 9 and Eq. (IV.13)] The critical mild hierarchy M2/M1 = 4.7 is determined from the one-flavour efficiency factors of Eqs. (III.13)/(III.18) applied to the tau-flavour decay parameters, not from a numerical solution of the flavoured Boltzmann equations (IV.10)-(IV.11). Since the claim is specifically about flavour-dependent N1 dominance, a flavoured Boltzmann check analogous to Fig. 2 for the representative points of Fig. 9 would strengthen the identification of δ12 = 3.7 as the critical point; as it stands, the conclusion relies on the analytic hierarchy-exponential approximation without direct verification in the flavoured case.
minor comments (3)
  1. [Sec. II, Eq. (II.11)] The symbol θ is reused for the relative phase after the redefinition θ1 = 0, θ2 = θ; the allowed range of θ should be stated explicitly next to Eq. (II.11) rather than only in the discussion around Fig. 6.
  2. [Sec. V.A, Eq. (V.6)] The expression for ε1^μ in the 'strong hierarchical limit' is used in a context where x12 = (4.7)^2 ≈ 22, which is not strongly hierarchical; please clarify whether the full g'(x12) expression of Eq. (V.5) is used in the numerical analysis.
  3. [Fig. 12 caption] The caption does not state that parameter points with large decay parameters are discarded for M1 = 7 × 10^10 GeV, although the text explains this; the truncation should be stated in the caption so that the plot is not misread as covering the full allowed parameter space.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the central mass-window and N2-survival claims are computed from neutrino-oscillation constraints and model dynamics, not fitted to the observed baryon asymmetry.

full rationale

The paper's central quantitative claims are (i) the mild hierarchy M2/M1 ~ 4.7 required for N1-dominated leptogenesis, (ii) the resulting window 7.5e9 GeV < M1 < 4e10 GeV, and (iii) the ~33% probability that N2-generated asymmetry survives in the electron flavour after N1 washout in the three-flavour regime. All three are derived from the CPmu-tau parametrization of the Dirac mass matrix (Eq. II.11), constrained by neutrino oscillation data, and then evolved through standard Boltzmann or analytic efficiency-factor equations. The observed baryon-to-photon ratio etaB is used as a target to compare against, but no parameter is fitted to it. The threshold M2/M1 = 4.7 is obtained by comparing efficiency factors kappa1 with kappa1^infinity and by scanning the model's allowed flavoured decay parameters; it is not imposed by construction. The upper bound M_max ~ 4e10 GeV follows from the explicit decoherence condition F_tau > W in Eq. V.10, again a computed consistency requirement rather than an input. The 33% electron-flavour survival probability is computed from the distribution of K1e in the model parameter space, with the washout condition K1e < 1 taken from standard leptogenesis literature; this is a model prediction, not a fitted output. The paper's self-citations supply the model texture (Ref. [35]) and some analytic tools (Ref. [63]), but these are external premises and standard machinery, not results that already contain the quoted mass window or survival probability. The limitations acknowledged by the authors, such as the neglect of flavour couplings and the need for a full density-matrix treatment beyond M_max, are correctness or robustness concerns, not circularity. The derivation chain is therefore self-contained with respect to the claims that are actually presented as predictions.

Assumptions & free parameters 5 free parameters · 7 assumptions · 1 invented entities

The central claims rest on a specific CPmu-tau-antisymmetric seesaw texture with six scanning parameters {x1,x2,y1,y2,theta,M1}, plus standard strong-washout and thermal-production assumptions. The second scenario adds an unobserved N3 with assumed Yukawa couplings. These are model assumptions rather than fitted constants for eta_B, which keeps the circularity burden low.

free parameters (5)
  • x1, x2, y1, y2 (Dirac mass texture parameters) = ranges shown in Fig. 6, in sqrt(eV)
    Free parameters of the CPmu-tau-antisymmetric m_D texture of Eq. II.11-II.13, scanned and constrained by NuFIT 3-sigma oscillation data.
  • theta (relative phase) = -150 deg < theta < 150 deg
    The phase difference theta2 - theta1 after phase redefinition in Sec. II, constrained by the neutrino oscillation fit.
  • M1 (lightest right-handed neutrino mass) = allowed window roughly 7.5e9 to 4e10 GeV
    Input mass scale; the paper derives an allowed window but the value of M1 itself is not predicted.
  • M2/M1 hierarchy ratio = 4.7, corresponding to delta12 = 3.7
    Chosen as the critical mild hierarchy for a valid N1-dominated scenario, derived from efficiency-factor comparisons rather than fitted to the baryon asymmetry.
  • M3 (third right-handed neutrino mass, second scenario) = greater than 1e12 GeV
    Introduced in Sec. V B to make the N2 CP asymmetry nonvanishing when M1 is below 1e9 GeV.
assumptions (7)
  • domain assumption Type-I seesaw with diagonal charged-lepton and right-handed neutrino mass matrices
    Eqs. II.2-II.3 establish the minimal seesaw framework and the basis used throughout.
  • domain assumption CPmu-tau-antisymmetric invariance of the Dirac mass matrix: m_D G = -i m_D^*
    Eq. II.10 is the defining symmetry of the model, taken from prior work by some of the same authors.
  • domain assumption Two right-handed neutrino minimal seesaw with det(M_nu) = 0 and massless lightest neutrino
    Sec. II after Eq. II.12; this texture is required by the CPmu-tau structure and sets a hierarchical light neutrino spectrum.
  • domain assumption Thermal production of right-handed neutrinos with TRH > M2 and no pre-existing asymmetry
    Sec. III opening states both RH neutrinos are thermally produced and pre-existing asymmetries are not considered.
  • domain assumption Strong washout regime with neglect of Delta L = 1 and Delta L = 2 scatterings in the efficiency equations
    Sec. III after Eq. III.7; this standard approximation is used for the strong-washout parameter region.
  • domain assumption Full charged-lepton flavour decoherence, valid when F_tau = Gamma_tau/(2Hz) dominates the washout rates
    Eq. V.10 and the surrounding text define the condition used to set M_max ~ 4e10 GeV; violation requires density-matrix equations.
  • ad hoc to paper A third right-handed neutrino N3 with M3 > 1e12 GeV and Yukawa couplings of similar order to N1 and N2
    Sec. V B introduces N3 to give N2 a nonvanishing CP asymmetry in the second scenario; this goes beyond the minimal two-RH seesaw used in the first part.
invented entities (1)
  • Right-handed neutrino N3 with M3 > 1e12 GeV
    purpose: Provides a nonvanishing N2 CP asymmetry when M1 is in the three-flavour regime; its seesaw contribution is suppressed by M3.
    Assumed in Sec. V B with Yukawa couplings of similar order to N1 and N2; no direct observable signature is identified in the paper.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Flavoured leptogenesis and ${\rm CP}^{\mu\tau}$ symmetry." pith.science (2026). https://pith.science/paper/2VFRYY5L

@misc{pith2026190808126,
  author       = {Pith},
  title        = {Pith review of: Flavoured leptogenesis and $\rm CP^\mu\tau$ symmetry},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/2VFRYY5L}},
  note         = {Machine review of arXiv:1908.08126}
}
abstract

We present a systematic study of leptogenesis in neutrino mass models with $\mu\tau$-flavoured CP symmetry. In addition to the strong hierarchical $N_1$-dominated scenario ($N_1$DS) in the `two flavour regime' of leptogenesis, we show that one may choose the right-handed (RH) neutrino mass hierarchy as mild as $M_2\simeq 4.7 M_1$ for a perfectly valid hierarchical $N_1$DS. This in turn reduces the lower bound on the allowed values of $M_1$, compared to what is stated in the literature. The consideration of flavour effects due to the heavy neutrinos also translate into an upper bound on $M_1$. It is only below this bound that the observed baryon-to-photon ratio can be realized for a standard ${ N_1}$ domination, else a substantial part of the parameter space is also compatible with $N_2$DS. We deduce conditions under which the baryon asymmetry produced by the second RH neutrino plays an important role. Finally, we discuss another interesting scenario where lepton asymmetry generated by $N_2$ in the two flavour regime faces washout by $N_1$ in the three flavour regime. Considering a hierarchical light neutrino mass spectrum, which is now favoured by cosmological observations, we show that at the end of $N_1$-leptogenesis, the asymmetry generated by $N_2$ survives only in the electron flavour and around $33\%$ of the parameter space is consistent with a pure $N_2$-leptogenesis.

Figures

Figures reproduced from arXiv: 1908.08126 by the authors.

Figure 1
Figure 1. FIG. 1. Top left [PITH_FULL_IMAGE:figures/full_fig_p008_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2. Efficiency factor with [PITH_FULL_IMAGE:figures/full_fig_p010_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3. Left: Possible error due to [PITH_FULL_IMAGE:figures/full_fig_p011_3.png] view at source ↗
Figures from the paper (11 more)
Figure 4
Figure 4. Figure 4: FIG. 4. Ilustration of the two flavour regime for two RH neutrino model. [PITH_FULL_IMAGE:figures/full_fig_p013_4.png]
Figure 5
Figure 5. Figure 5: FIG. 5. Various mass pattern in a leptogenesis scenario dominated by two right handed neutrinos. [PITH_FULL_IMAGE:figures/full_fig_p015_5.png]
Figure 6
Figure 6. Figure 6: FIG. 6. Parameter space of CP [PITH_FULL_IMAGE:figures/full_fig_p016_6.png]
Figure 7
Figure 7. Figure 7: FIG. 7. Flavoured decay parameters for both the RH neutrinos. [PITH_FULL_IMAGE:figures/full_fig_p017_7.png]
Figure 8
Figure 8. Figure 8: FIG. 8. Plot showing the quantity (1 [PITH_FULL_IMAGE:figures/full_fig_p019_8.png]
Figure 9
Figure 9. Figure 9: FIG. 9. Upper panel: (Colour codes for the [PITH_FULL_IMAGE:figures/full_fig_p020_9.png]
Figure 10
Figure 10. Figure 10: FIG. 10. Comparison among rates of various processes involved in the leptogenesis. The horizontal [PITH_FULL_IMAGE:figures/full_fig_p021_10.png]
Figure 11
Figure 11. Figure 11: FIG. 11. Top panel [PITH_FULL_IMAGE:figures/full_fig_p022_11.png]
Figure 12
Figure 12. Figure 12: FIG. 12. Normalised baryon to photon ratio with the [PITH_FULL_IMAGE:figures/full_fig_p023_12.png]
Figure 13
Figure 13. Figure 13: FIG. 13. Distributions of the flavoured decay parameters. The probability for the electron decay [PITH_FULL_IMAGE:figures/full_fig_p024_13.png]
Figure 14
Figure 14. Figure 14: FIG. 14. Left: Possible range of the orientation of the state [PITH_FULL_IMAGE:figures/full_fig_p025_14.png]

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

134 extracted references · 20 canonical work pages

  1. [1]

    (V.6) Similarly for i = 2 the CP asymmetry parameter can be calculated as εµ 2 = g′(x21)M1 4πv2 [(x1x2 +y1y2 cosθ)y1y2 sinθ x2 2 +y2 2 ] =−ετ

  2. [2]

    − √ 2eiπ/4(x1y1eiθ1 +x2y2eiθ2) −i √ 2eiπ/4(x1y1e−iθ1 +x2y2e−iθ2) − √ 2eiπ/4(x1y1eiθ1 +x2y2eiθ2) −(e2iθ1y2 1 +e2iθ2y2

  3. [3]

    −i(y2 1 +y2 2) −i √ 2eiπ/4(x1y1e−iθ1 +x2y2e−iθ2) −i(y2 1 +y2

  4. [4]

    pre-existing asymmetry

    e−2iθ1y2 1 +e−2iθ2y2 2  . (II.12) In (II.12), new real parameters x1,2 and y1,2 are defined by scaling a1,2 and b1,2 with the square roots of the respective RH neutrino masses M1,2, i.e. a1,2√ M1,2 =x1,2, b1,2√ M1,2 =y1,2. (II.13) A few comments on the matrix MCPµτA ν are in order. Since det ( MCPµτA ν ) = 0, the lightest neutrino mass (either m1 for a n...

  5. [5]

    (V.7) Armed with these equations, we can proceed toward a systematic discussion of leptogenesis for the relevant cases. A. Two flavour regime: 109 GeV<M 1,2< 1012 GeV The N1-decay parameters in the muon and tau flavour are strong enough [63, 64] to washout any pre-existing asymmetry (see right panel of Fig. 7). Thus, all the terms which contain the exponent...

  6. [6]

    (V.9) 19 �-��� ⊥ ���� ���� ���� ���� ���� ���� FIG. 8. Plot showing the quantity (1 −p⊥

  7. [7]

    Esteban, M

    I. Esteban, M. C. Gonzalez-Garcia, A. Hernandez-Cabezudo, M. Maltoni and T. Schwetz, JHEP 1901, 106 (2019) doi:10.1007/JHEP01(2019)106 [arXiv:1811.05487 [hep-ph]]

  8. [8]

    An inter- esting fact is that (1−p⊥

    with the model parameterx1 andx2. An inter- esting fact is that (1−p⊥

Show all 134 references
  1. [9]

    This means N2 always contributes to the final asymmetry

    never vanishes in this model. This means N2 always contributes to the final asymmetry. In addition, one has a strong concentration of points towards the higher values (∼ 0.5) of (1 −p⊥

  2. [10]

    In fact we show as we proceed, N2 domination in this model is possible for a significant amount of parameter space ( ∼ 26%)

    which indicates there could be sizeable number of data points for which N2 domination could be realized. In fact we show as we proceed, N2 domination in this model is possible for a significant amount of parameter space ( ∼ 26%). We first concentrate on the choice of RH neutrino...

  3. [11]

    Tanabashi et al

    M. Tanabashi et al. [Particle Data Group], Phys. Rev. D 98, no. 3, 030001 (2018). doi:10.1103/PhysRevD.98.030001

  4. [12]

    Since lepton asymmetry generated by N2 is proportional to (1 −p⊥ 12), and clearly this never vanishes in this model, a pure N1 dominated scenario is not possible

    with the model parameter x1 and x2. Since lepton asymmetry generated by N2 is proportional to (1 −p⊥ 12), and clearly this never vanishes in this model, a pure N1 dominated scenario is not possible. Note that x1,2 are dimensional quantities, and are plotted in units of √ eV. I...

  5. [13]

    Abe et al

    K. Abe et al. [T2K Collaboration], Phys. Rev. Lett. 118, no. 15, 151801 (2017) doi:10.1103/PhysRevLett.118.151801 [arXiv:1701.00432 [hep-ex]]

  6. [14]

    Abe et al

    K. Abe et al. [T2K Collaboration], Phys. Rev. D 96, no. 9, 092006 (2017) Erratum: [Phys. Rev. D 98, no. 1, 019902 (2018)] doi:10.1103/PhysRevD.96.092006, 10.1103/Phys- RevD.98.019902 [arXiv:1707.01048 [hep-ex]]

  7. [15]

    Abe et al

    K. Abe et al. [T2K Collaboration], Phys. Rev. Lett. 121, no. 17, 171802 (2018) doi:10.1103/PhysRevLett.121.171802 [arXiv:1807.07891 [hep-ex]]

  8. [16]

    Adamson et al

    P. Adamson et al. [NOvA Collaboration], Phys. Rev. Lett. 118, no. 23, 231801 (2017) doi:10.1103/PhysRevLett.118.231801 [arXiv:1703.03328 [hep-ex]]

  9. [17]

    M. A. Acero et al. [NOvA Collaboration], Phys. Rev. D 98, 032012 (2018) doi:10.1103/PhysRevD.98.032012 [arXiv:1806.00096 [hep-ex]]

  10. [18]

    Altarelli and F

    G. Altarelli and F. Feruglio, Rev. Mod. Phys. 82, 2701 (2010) doi:10.1103/RevModPhys.82.2701 [arXiv:1002.0211 [hep-ph]]

  11. [19]

    Ishimori, T

    H. Ishimori, T. Kobayashi, H. Ohki, Y. Shimizu, H. Okada and M. Tanimoto, Prog. Theor. Phys. Suppl. 183, 1 (2010) doi:10.1143/PTPS.183.1 [arXiv:1003.3552 [hep-ph]]

  12. [20]

    S. F. King, Prog. Part. Nucl. Phys. 94, 217 (2017) doi:10.1016/j.ppnp.2017.01.003 [arXiv:1701.04413 [hep-ph]]

  13. [21]

    S. T. Petcov [arXiv:1711.10806[hep-ph]]. 27

  14. [22]

    R. N. Mohapatra and S. Nussinov, Phys. Rev. D 60, 013002 (1999) doi:10.1103/PhysRevD.60.013002 [hep-ph/9809415]

  15. [23]

    C. S. Lam, Phys. Lett. B 507, 214 (2001) doi:10.1016/S0370-2693(01)00465-8 [hep- ph/0104116]

  16. [24]

    Ma and M

    E. Ma and M. Raidal, Phys. Rev. Lett. 87, 011802 (2001) Erratum: [Phys. Rev. Lett. 87, 159901 (2001)] doi:10.1103/PhysRevLett.87.159901, 10.1103/PhysRevLett.87.011802 [hep- ph/0102255]

  17. [25]

    K. R. S. Balaji, W. Grimus and T. Schwetz, Phys. Lett. B508, 301 (2001) doi:10.1016/S0370- 2693(01)00532-9 [hep-ph/0104035]

  18. [26]

    Fukuyama and H

    T. Fukuyama and H. Nishiura, hep-ph/9702253

  19. [27]

    Fukuyama, PTEP 2017, no

    T. Fukuyama, PTEP 2017, no. 3, 033B11 (2017) doi:10.1093/ptep/ptx032 [arXiv:1701.04985 [hep-ph]]

  20. [28]

    R. N. Mohapatra and W. Rodejohann, Phys. Rev. D 72, 053001 (2005) doi:10.1103/PhysRevD.72.053001 [hep-ph/0507312]

  21. [29]

    Z. z. Xing, H. Zhang and S. Zhou, Phys. Lett. B 641, 189 (2006) doi:10.1016/j.physletb.2006.08.045 [hep-ph/0607091]

  22. [30]

    P. F. Harrison and W. G. Scott, Phys. Lett. B 547, 219 (2002) doi:10.1016/S0370- 2693(02)02772-7 [hep-ph/0210197]

  23. [31]

    Grimus and L

    W. Grimus and L. Lavoura, Phys. Lett. B 579, 113 (2004) doi:10.1016/j.physletb.2003.10.075 [hep-ph/0305309]

  24. [32]

    R. N. Mohapatra and C. C. Nishi, JHEP 1508, 092 (2015) doi:10.1007/JHEP08(2015)092 [arXiv:1506.06788 [hep-ph]]

  25. [33]

    R. N. Mohapatra and C. C. Nishi, Phys. Rev. D 86, 073007 (2012) doi:10.1103/PhysRevD.86.073007 [arXiv:1208.2875 [hep-ph]]

  26. [34]

    Gupta, A

    S. Gupta, A. S. Joshipura and K. M. Patel, Phys. Rev. D 85, 031903 (2012) doi:10.1103/PhysRevD.85.031903 [arXiv:1112.6113 [hep-ph]]

  27. [35]

    Feruglio, C

    F. Feruglio, C. Hagedorn and R. Ziegler, JHEP 1307, 027 (2013) doi:10.1007/JHEP07(2013)027 [arXiv:1211.5560 [hep-ph]]

  28. [36]

    Holthausen, M

    M. Holthausen, M. Lindner and M. A. Schmidt, JHEP 1304, 122 (2013) doi:10.1007/JHEP04(2013)122 [arXiv:1211.6953 [hep-ph]]. Nucl. Phys. B 883, 267 (2014)

  29. [37]

    M. C. Chen, M. Fallbacher, K. T. Mahanthappa, M. Ratz and A. Trautner, Nucl. Phys. B 883, 267 (2014) doi:10.1016/j.nuclphysb.2014.03.023 [arXiv:1402.0507 [hep-ph]]

  30. [38]

    G. J. Ding, S. F. King, C. Luhn and A. J. Stuart, JHEP 1305, 084 (2013) doi:10.1007/JHEP05(2013)084 [arXiv:1303.6180 [hep-ph]]

  31. [39]

    Feruglio, C

    F. Feruglio, C. Hagedorn and R. Ziegler, Eur. Phys. J. C 74, 2753 (2014) doi:10.1140/epjc/s10052-014-2753-2 [arXiv:1303.7178 [hep-ph]]

  32. [40]

    C. C. Nishi and B. L. Snchez-Vega, JHEP 1701, 068 (2017) doi:10.1007/JHEP01(2017)068 [arXiv:1611.08282 [hep-ph]]

  33. [41]

    Rodejohann and X

    W. Rodejohann and X. J. Xu, Phys. Rev. D 96, no. 5, 055039 (2017) doi:10.1103/PhysRevD.96.055039 [arXiv:1705.02027 [hep-ph]]

  34. [42]

    J. T. Penedo, S. T. Petcov and A. V. Titov, JHEP 1712, 022 (2017) doi:10.1007/JHEP12(2017)022 [arXiv:1705.00309 [hep-ph]]

  35. [43]

    Samanta and A

    R. Samanta and A. Ghosal, Nucl. Phys. B 911, 846 (2016) doi:10.1016/j.nuclphysb.2016.08.036 [arXiv:1507.02582 [hep-ph]]

  36. [44]

    Z. h. Zhao, Nucl. Phys. B 935, 129 (2018) doi:10.1016/j.nuclphysb.2018.08.007 [arXiv:1803.04603 [hep-ph]]. 28

  37. [45]

    Samanta, P

    R. Samanta, P. Roy and A. Ghosal, JHEP 1806, 085 (2018) doi:10.1007/JHEP06(2018)085 [arXiv:1712.06555 [hep-ph]]

  38. [46]

    S. F. King and C. C. Nishi, Phys. Lett. B 785, 391 (2018) doi:10.1016/j.physletb.2018.08.056 [arXiv:1807.00023 [hep-ph]]

  39. [47]

    Z. C. Liu, C. X. Yue and Z. H. Zhao, JHEP 1810, 106 (2018) doi:10.1007/JHEP10(2018)106 [arXiv:1807.10031 [hep-ph]]

  40. [48]

    M. H. Rahat, P. Ramond and B. Xu, Phys. Rev. D 98, no. 5, 055030 (2018) doi:10.1103/PhysRevD.98.055030 [arXiv:1805.10684 [hep-ph]]

  41. [49]

    C. C. Nishi, B. L. Snchez-Vega and G. Souza Silva, JHEP 1809, 042 (2018) doi:10.1007/JHEP09(2018)042 [arXiv:1806.07412 [hep-ph]]

  42. [50]

    D. M. Barreiros, R. G. Felipe and F. R. Joaquim, JHEP 1901, 223 (2019) doi:10.1007/JHEP01(2019)223 [arXiv:1810.05454 [hep-ph]]

  43. [51]

    F. J. de Anda, S. F. King and E. Perdomo, arXiv:1812.05620 [hep-ph]

  44. [52]

    S. F. King and Y. L. Zhou, arXiv:1901.06877 [hep-ph]

  45. [53]

    Ecker, W

    G. Ecker, W. Grimus and H. Neufeld, J. Phys. A 20, L807 (1987). doi:10.1088/0305- 4470/20/12/010

  46. [54]

    Grimus and M

    W. Grimus and M. N. Rebelo, Phys. Rept. 281, 239 (1997) doi:10.1016/S0370-1573(96)00030- 0 [hep-ph/9506272]

  47. [55]

    P. Chen, C. Y. Yao and G. J. Ding, Phys. Rev. D 92, no. 7, 073002 (2015) doi:10.1103/PhysRevD.92.073002 [arXiv:1507.03419 [hep-ph]]

  48. [56]

    Ma, Phys

    E. Ma, Phys. Lett. B 752, 198 (2016) doi:10.1016/j.physletb.2015.11.049 [arXiv:1510.02501 [hep-ph]]

  49. [57]

    P. Chen, G. J. Ding, F. Gonzalez-Canales and J. W. F. Valle, Phys. Lett. B 753, 644 (2016) doi:10.1016/j.physletb.2015.12.069 [arXiv:1512.01551 [hep-ph]]

  50. [58]

    P. Chen, G. J. Ding, F. Gonzalez-Canales and J. W. F. Valle, Phys. Rev. D 94, no. 3, 033002 (2016) doi:10.1103/PhysRevD.94.033002 [arXiv:1604.03510 [hep-ph]]

  51. [59]

    Sinha, P

    R. Sinha, P. Roy and A. Ghosal, Phys. Rev. D 99, no. 3, 033009 (2019) doi:10.1103/PhysRevD.99.033009 [arXiv:1809.06615 [hep-ph]]

  52. [60]

    Samanta, P

    R. Samanta, P. Roy and A. Ghosal, Eur. Phys. J. C 76, no. 12, 662 (2016) doi:10.1140/epjc/s10052-016-4528-4 [arXiv:1604.06731 [hep-ph]]

  53. [61]

    Samanta, P

    R. Samanta, P. Roy and A. Ghosal, Acta Phys. Polon. Supp. 9, 807 (2016) doi:10.5506/APhysPolBSupp.9.807 [arXiv:1604.01206 [hep-ph]]

  54. [62]

    Samanta, M

    R. Samanta, M. Chakraborty, P. Roy and A. Ghosal, JCAP 1703, no. 03, 025 (2017) doi:10.1088/1475-7516/2017/03/025 [arXiv:1610.10081 [hep-ph]]

  55. [63]

    Ghosal and R

    A. Ghosal and R. Samanta, JHEP 1505, 077 (2015) doi:10.1007/JHEP05(2015)077 [arXiv:1501.00916 [hep-ph]]

  56. [64]

    Samanta and M

    R. Samanta and M. Chakraborty, JCAP 1902, 003 (2019) doi:10.1088/1475- 7516/2019/02/003 [arXiv:1802.04751 [hep-ph]]

  57. [65]

    Sinha, R

    R. Sinha, R. Samanta and A. Ghosal, JHEP 1712, 030 (2017) doi:10.1007/JHEP12(2017)030 [arXiv:1706.00946 [hep-ph]]

  58. [66]

    Sinha, S

    R. Sinha, S. Bhattacharya and R. Samanta, JHEP 1903, 081 (2019) doi:10.1007/JHEP03(2019)081 [arXiv:1810.05391 [hep-ph]]

  59. [67]

    V. A. Kuzmin, V. A. Rubakov and M. E. Shaposhnikov, Phys. Lett. 155B, 36 (1985). doi:10.1016/0370-2693(85)91028-7

  60. [68]

    Fukugita and T

    M. Fukugita and T. Yanagida, Phys. Lett. B174, 45 (1986). doi:10.1016/0370-2693(86)91126- 3 29

  61. [69]

    Riotto and M

    A. Riotto and M. Trodden, Ann. Rev. Nucl. Part. Sci. 49, 35 (1999) doi:10.1146/annurev.nucl.49.1.35 [arXiv:9901362 [hep-ph]]

  62. [70]

    E. W. Kolb and M. S. Turner, Front. Phys. 69, 1 (1990)

  63. [71]

    Pilaftsis and T

    A. Pilaftsis and T. E. J. Underwood, Nucl. Phys. B 692, 303 (2004) doi:10.1016/j.nuclphysb.2004.05.029 [arXiv:0309342 [hep-ph]]

  64. [72]

    F. F. Deppisch and A. Pilaftsis, Phys. Rev. D 83, 076007 (2011) doi:10.1103/PhysRevD.83.076007 [arXiv:1012.1834 [hep-ph]]

  65. [73]

    Buchmuller, P

    W. Buchmuller, P. Di Bari and M. Plumacher, Annals Phys. 315, 305 (2005) doi:10.1016/j.aop.2004.02.003 [hep-ph/0401240]

  66. [74]

    Davidson, E

    S. Davidson, E. Nardi and Y. Nir, Phys. Rept. 466, 105 (2008) doi:10.1016/j.physrep.2008.06.002 [arXiv:0802.2962 [hep-ph]]

  67. [75]

    Minkowski, Phys

    P. Minkowski, Phys. Lett. 67B, 421 (1977)

  68. [76]

    Gell-Mann, P

    M. Gell-Mann, P. Ramond and R. Slansky, Conf. Proc. C 790927, 315 (1979) [arXiv:1306.4669 [hep-th]]

  69. [77]

    Yanagida, Prog

    T. Yanagida, Prog. Theor. Phys. 64, 1103 (1980). R. N. Mohapatra and G. Senjanovic, Phys. Rev. Lett. 44, 912 (1980). A variant of Type I seesaw: R. N. Mohapatra, Phys. Rev. Lett. 56, 561 (1986)

  70. [78]

    Aghanim et al

    N. Aghanim et al. [Planck Collaboration], Astron. Astrophys. 596, A107 (2016) doi:10.1051/0004-6361/201628890 [arXiv:1605.02985 [astro-ph.CO]]

  71. [79]

    P. Chen, G. J. Ding and S. F. King, JHEP 1603, 206 (2016) doi:10.1007/JHEP03(2016)206 [arXiv:1602.03873 [hep-ph]]

  72. [80]

    Hagedorn and E

    C. Hagedorn and E. Molinaro, Nucl. Phys. B 919, 404 (2017) doi:10.1016/j.nuclphysb.2017.03.015 [arXiv:1602.04206 [hep-ph]]

  73. [81]

    Abada, S

    A. Abada, S. Davidson, A. Ibarra, F.-X. Josse-Michaux, M. Losada and A. Riotto, JHEP 0609, 010 (2006) doi:10.1088/1126-6708/2006/09/010 [arXiv:0605281 [hep-ph]]

  74. [82]

    Nardi, Y

    E. Nardi, Y. Nir, E. Roulet and J. Racker, JHEP 0601, 164 (2006) doi:10.1088/1126- 6708/2006/01/164 [arXiv:0601084 [hep-ph]]

  75. [83]

    Blanchet and P

    S. Blanchet and P. Di Bari, JCAP 0703, 018 (2007) doi:10.1088/1475-7516/2007/03/018 [hep-ph/0607330]

  76. [84]

    P. S. B. Dev, P. Di Bari, B. Garbrecht, S. Lavignac, P. Millington and D. Teresi, Int. J. Mod. Phys. A 33, 1842001 (2018) doi:10.1142/S0217751X18420010 [arXiv:1711.02861 [hep-ph]]

  77. [85]

    S. F. King, Nucl. Phys. B 576, 85 (2000) doi:10.1016/S0550-3213(00)00109-7 [hep- ph/9912492]

  78. [86]

    S. F. King, JHEP 0209, 011 (2002) doi:10.1088/1126-6708/2002/09/011 [hep-ph/0204360]

  79. [87]

    Di Bari and A

    P. Di Bari and A. Riotto, Phys. Lett. B 671, 462 (2009) doi:10.1016/j.physletb.2008.12.054 [arXiv:0809.2285 [hep-ph]]

  80. [88]

    Blanchet, P

    S. Blanchet, P. Di Bari, D. A. Jones and L. Marzola, JCAP 1301, 041 (2013) doi:10.1088/1475-7516/2013/01/041 [arXiv:1112.4528 [hep-ph]]

  81. [89]

    Di Bari, Nucl

    P. Di Bari, Nucl. Phys. B 727, 318 (2005) doi:10.1016/j.nuclphysb.2005.08.032 [hep- ph/0502082]

  82. [90]

    Di Bari, M

    P. Di Bari, M. Re Fiorentin and R. Samanta, JHEP 1905, 011 (2019) doi:10.1007/JHEP05(2019)011 [arXiv:1812.07720 [hep-ph]]

  83. [91]

    P. H. Frampton, S. L. Glashow and T. Yanagida, Phys. Lett. B 548, 119 (2002) doi:10.1016/S0370-2693(02)02853-8 [arXiv:hep-ph/0208157]

  84. [92]

    Raidal and A

    M. Raidal and A. Strumia, Phys. Lett. B 553, 72 (2003) doi:10.1016/S0370-2693(02)03124-6 [arXiv:hep-ph/0210021]. 30

  85. [94]

    Bambhaniya, P

    G. Bambhaniya, P. S. Bhupal Dev, S. Goswami, S. Khan and W. Rodejohann, Phys. Rev. D 95, no. 9, 095016 (2017) doi:10.1103/PhysRevD.95.095016 [arXiv:1611.03827 [hep-ph]]

  86. [95]

    Grimus, S

    W. Grimus, S. Kaneko, L. Lavoura, H. Sawanaka and M. Tanimoto, JHEP 0601, 110 (2006) doi:10.1088/1126-6708/2006/01/110 [arXiv:0510326 [hep-ph]]

  87. [96]

    G. F. Giudice, M. Peloso, A. Riotto and I. Tkachev, JHEP 9908, 014 (1999) doi:10.1088/1126-6708/1999/08/014 [hep-ph/9905242]

  88. [97]

    M. Y. Khlopov and A. D. Linde, Phys. Lett. 138B, 265 (1984). doi:10.1016/0370- 2693(84)91656-3

  89. [98]

    G. F. Giudice, A. Notari, M. Raidal, A. Riotto and A. Strumia, Nucl. Phys. B 685, 89 (2004) doi:10.1016/j.nuclphysb.2004.02.019 [hep-ph/0310123]

  90. [99]

    Croon, N

    D. Croon, N. Fernandez, D. McKeen and G. White, JHEP 1906, 098 (2019) doi:10.1007/JHEP06(2019)098 [arXiv:1903.08658 [hep-ph]]

  91. [100]

    Buchmuller, P

    W. Buchmuller, P. Di Bari and M. Plumacher, Nucl. Phys. B 665, 445 (2003) doi:10.1016/S0550-3213(03)00449-8 [hep-ph/0302092]

  92. [101]

    Buchmuller, P

    W. Buchmuller, P. Di Bari and M. Plumacher, Nucl. Phys. B 643, 367 (2002) Erratum: [Nucl. Phys. B 793, 362 (2008)] doi:10.1016/S0550-3213(02)00737-X, 10.1016/j.nuclphysb.2007.11.030 [hep-ph/0205349]

  93. [102]

    S. H. S. Alexander, M. E. Peskin and M. M. Sheikh-Jabbari, Phys. Rev. Lett. 96, 081301 (2006) doi:10.1103/PhysRevLett.96.081301 [hep-th/0403069]

  94. [103]

    Adshead, A

    P. Adshead, A. J. Long and E. I. Sfakianakis, Phys. Rev. D 97, no. 4, 043511 (2018) doi:10.1103/PhysRevD.97.043511 [arXiv:1711.04800 [hep-ph]]

  95. [104]

    Bertuzzo, P

    E. Bertuzzo, P. Di Bari and L. Marzola, Nucl. Phys. B 849, 521 (2011) doi:10.1016/j.nuclphysb.2011.03.027 [arXiv:1007.1641 [hep-ph]]

  96. [105]

    Engelhard, Y

    G. Engelhard, Y. Grossman, E. Nardi and Y. Nir, Phys. Rev. Lett. 99, 081802 (2007) doi:10.1103/PhysRevLett.99.081802 [hep-ph/0612187]

  97. [106]

    Antusch, P

    S. Antusch, P. Di Bari, D. A. Jones and S. F. King, Phys. Rev. D 86, 023516 (2012) doi:10.1103/PhysRevD.86.023516 [arXiv:1107.6002 [hep-ph]]

  98. [107]

    Di Bari and L

    P. Di Bari and L. Marzola, Nucl. Phys. B 877, 719 (2013) doi:10.1016/j.nuclphysb.2013.10.027 [arXiv:1308.1107 [hep-ph]]

  99. [108]

    Chianese and P

    M. Chianese and P. Di Bari, JHEP 1805, 073 (2018) doi:10.1007/JHEP05(2018)073 [arXiv:1802.07690 [hep-ph]]

  100. [109]

    Blanchet and P

    S. Blanchet and P. Di Bari, JCAP 0606, 023 (2006) doi:10.1088/1475-7516/2006/06/023 [hep-ph/0603107]

  101. [110]

    Aristizabal Sierra, L

    D. Aristizabal Sierra, L. A. Munoz and E. Nardi, Phys. Rev. D 80, 016007 (2009) doi:10.1103/PhysRevD.80.016007 [arXiv:0904.3043 [hep-ph]]

  102. [111]

    Davidson and A

    S. Davidson and A. Ibarra, Phys. Lett. B 535, 25 (2002) doi:10.1016/S0370-2693(02)01735-5 [hep-ph/0202239]

  103. [112]

    Adhikary, M

    B. Adhikary, M. Chakraborty and A. Ghosal, JHEP1310, 043 (2013) Erratum: [JHEP 1409, 180 (2014)] doi:10.1007/JHEP10(2013)043, 10.1007/JHEP09(2014)180 [arXiv:1307.0988 [hep-ph]]

  104. [113]

    Agostini et al

    M. Agostini et al. , Nature 544, 47 (2017) doi:10.1038/nature21717 [arXiv:1703.00570 [nucl- ex]]

  105. [114]

    Gando et al

    A. Gando et al. [KamLAND-Zen Collaboration], Phys. Rev. Lett. 110, no. 6, 062502 (2013) doi:10.1103/PhysRevLett.110.062502 [arXiv:1211.3863 [hep-ex]]. 31

  106. [115]

    Auger et al

    M. Auger et al. [EXO-200 Collaboration], Phys. Rev. Lett. 109, 032505 (2012) doi:10.1103/PhysRevLett.109.032505 [arXiv:1205.5608 [hep-ex]]

  107. [116]

    Agostini, G

    M. Agostini, G. Benato and J. Detwiler, Phys. Rev. D 96, no. 5, 053001 (2017) doi:10.1103/PhysRevD.96.053001 [arXiv:1705.02996 [hep-ex]]

  108. [117]

    Shirai, Results and future plans for the KamLAND- Zen, (2016), Neutrino 2016, London, UK, http://neutrino2016.iopconfs.org/IOP/media/ uploaded/EVIOP/event 948/09.45 5 Shirai.pdf

    J. Shirai, Results and future plans for the KamLAND- Zen, (2016), Neutrino 2016, London, UK, http://neutrino2016.iopconfs.org/IOP/media/ uploaded/EVIOP/event 948/09.45 5 Shirai.pdf

  109. [118]

    Mong, nEXO Double Beta Decay, (2016), HQL2016, Blacksburg, VA, USA, http://indico.phys

    B. Mong, nEXO Double Beta Decay, (2016), HQL2016, Blacksburg, VA, USA, http://indico.phys. vt.edu/event/31/session/29/contribution/103/ material/slides/0.pdf

  110. [119]

    Wang et al

    G. Wang et al. [CUPID Collaboration], arXiv:1504.03599 [physics.ins-det]

  111. [120]

    Arnaboldi et al

    C. Arnaboldi et al. ([CUORE Collaboration]), Nucl. In- strum. Meth. A518, 775 (2004)

  112. [121]

    B. Schwingenheuer, Neutrinoless double beta decay with 76Ge, (2017), CERN EP Seminar, Geneva, Switzerland, https://indico.cern.ch/event/581028/ attachments/1395349/2129744/ge76 cern.pdf

  113. [122]

    Samanta, R

    R. Samanta, R. Sinha and A. Ghosal, arXiv:1805.10031 [hep-ph]

  114. [123]

    Barbieri, P

    R. Barbieri, P. Creminelli, A. Strumia and N. Tetradis, Nucl. Phys. B 575, 61 (2000) doi:10.1016/S0550-3213(00)00011-0 [hep-ph/9911315]

  115. [124]

    Antusch, P

    S. Antusch, P. Di Bari, D. A. Jones and S. F. King, Nucl. Phys. B 856, 180 (2012) doi:10.1016/j.nuclphysb.2011.10.036 [arXiv:1003.5132 [hep-ph]]

  116. [125]

    Moffat, S

    K. Moffat, S. Pascoli, S. T. Petcov, H. Schulz and J. Turner, Phys. Rev. D 98, no. 1, 015036 (2018) doi:10.1103/PhysRevD.98.015036 [arXiv:1804.05066 [hep-ph]]

  117. [126]

    P. S. Bhupal Dev, P. Millington, A. Pilaftsis and D. Teresi, Nucl. Phys. B 886, 569 (2014) doi:10.1016/j.nuclphysb.2014.06.020 [arXiv:1404.1003 [hep-ph]]

  118. [127]

    De Simone and A

    A. De Simone and A. Riotto, JCAP 0708, 002 (2007) doi:10.1088/1475-7516/2007/08/002 [hep-ph/0703175]

  119. [128]

    Garny, A

    M. Garny, A. Kartavtsev and A. Hohenegger, Annals Phys. 328, 26 (2013) doi:10.1016/j.aop.2012.10.007 [arXiv:1112.6428 [hep-ph]]

  120. [129]

    P. S. Bhupal Dev, P. Millington, A. Pilaftsis and D. Teresi, Nucl. Phys. B 891, 128 (2015) doi:10.1016/j.nuclphysb.2014.12.003 [arXiv:1410.6434 [hep-ph]]

  121. [130]

    Kartavtsev, P

    A. Kartavtsev, P. Millington and H. Vogel, JHEP 1606, 066 (2016) doi:10.1007/JHEP06(2016)066 [arXiv:1601.03086 [hep-ph]]

  122. [131]

    M. A. Luty, Phys. Rev. D 45, 455 (1992). doi:10.1103/PhysRevD.45.455

  123. [132]

    Hahn-Woernle, M

    F. Hahn-Woernle, M. Plumacher and Y. Y. Y. Wong, JCAP 0908, 028 (2009) doi:10.1088/1475-7516/2009/08/028 [arXiv:0907.0205 [hep-ph]]

  124. [133]

    Plumacher, Nucl

    M. Plumacher, Nucl. Phys. B 530, 207 (1998) doi:10.1016/S0550-3213(98)00410-6 [hep- ph/9704231]

  125. [134]

    E. K. Akhmedov, M. Frigerio and A. Y. Smirnov, JHEP 0309, 021 (2003) doi:10.1088/1126- 6708/2003/09/021 [hep-ph/0305322]

  126. [135]

    C. S. Fong, D. Meloni, A. Meroni and E. Nardi, JHEP 1501, 111 (2015) doi:10.1007/JHEP01(2015)111 [arXiv:1412.4776 [hep-ph]]

Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.