REVIEW
The KeV Majoron as Dark Matter Particle
High Energy Physics - Phenomenology · Submitted 2 Sep 1993 · 18 references
Pith's verdict: A genuine contribution on how to keep a keV majoron weakly coupled, but the model never generates the keV mass the whole scenario rests on.
T0 · AI review
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Referee report
The paper
The paper claims
A keV majoron produced at the lepton-number phase transition can account for the dark matter density and the galactic mass scale, with an explicit model and an X-ray line signature.
The reading
Extended reading notes
Core claim
A majoron with mass of order 1 keV, coupled to leptons only through heavy intermediaries, can be produced at the lepton-number phase transition with an abundance matching the critical density (Eq. 7: rho_J/rho_cr = 1.5 xi h^-2 m_J) and a Jeans mass matching the galactic scale (Eq. 16: M_gal ~ m_Pl^3/m_J^2 ~ 1.6e12 M_sun (m_J/1keV)^-2), while satisfying lifetime, photon, and nucleosynthesis bounds.
Load-bearing premise
The model as written gives a massless majoron: Section 3 states that the CP-odd scalar 'remains massless as a result of the spontaneous nature of the lepton number breaking.' The keV mass that the entire scenario requires is never generated. The paper distances itself from ref. [1], where the mass came from explicit Planck-suppressed breaking, so the origin of m_J ~ keV is an unstated input. Without it, the abundance formula (Eq. 7) and the Jeans-mass relation (Eq. 16) have no anchor.
Original abstract
We consider a very weakly interacting KeV majoron as dark matter particle (DMP), which provides both the critical density $\rho_{cr} = 1.88 \times 10^{-29} h^{2}$ $g/cm^{3}$ and the galactic scale $M_{gal}$ $\sim m^{3}_{Pl}/m^{2}_{J} \sim 10^{12} M_{\odot} (m_{J}/1 KeV)^{-2}$ for galaxy formation. The majoron couples to leptons only through some new "directly interacting particles", called DIPS, and this provides the required smallness of the coupling constants. If the masses of these DIPS are greater than the scale $V_s$ characterizing the spontaneous violation of the global lepton symmetry they are absent at the corresponding phase transition ($T \sim V_s$) and the majorons are produced during the phase transition, never being in thermal equilibrium during the history of the universe. In the alternative case $m_{DIP} < V_{s}$ the majorons can be for a short period in thermal equilibrium. This scenario is not forbidden by nucleosynthesis and gives a reasonable growth factor for the density fluctuations compatible with COBE. A possible signature is an X-ray line at $E_\gamma = \frac{m_J}{2}$, produced by the decay $J \to \gamma + \gamma$. A model is described which realizes the possibility of the KeV majoron as DMP and may also lead to observable rates for decays such as $\mu \ra e \gamma$ and $\mu \ra 3e$.
The compiled record
The paper's own sentences, arranged, kept beside the review and separate from it. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
The abstract, sentence by sentence
We consider a very weakly interacting KeV majoron as dark matter particle (DMP), which provides both the critical density $\rho_{cr} = 1.88 \times 10^{-29} h^{2}$ $g/cm^{3}$ and the galactic scale $M_{gal}$ $\sim m^{3}_{Pl}/m^{2}_{J} \sim 10^{12} M_{\odot} (m_{J}/1 KeV)^{-2}$ for galaxy formation. The majoron couples to leptons only through some new "directly interacting particles", called DIPS, and this provides the required smallness of the coupling constants. If the masses of these DIPS are greater than the scale $V_s$ characterizing the spontaneous violation of the global lepton symmetry they are absent at the corresponding phase transition ($T \sim V_s$) and the majorons are produced during the phase transition, never being in thermal equilibrium during the history of the universe. In the alternative case $m_{DIP} < V_{s}$ the majorons can be for a short period in thermal equilibrium. This scenario is not forbidden by nucleosynthesis and gives a reasonable growth factor for the density fluctuations compatible with COBE. A possible signature is an X-ray line at $E_\gamma = \frac{m_J}{2}$, produced by the decay $J \to \gamma + \gamma$. A model is described which realizes the possibility of the KeV majoron as DMP and may also lead to observable rates for decays such as $\mu \ra e \gamma$ and $\mu \ra 3e$.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We consider a very weakly interacting KeV majoron as dark matter particle (DMP), which provides both the critical density $\rho_{cr} = 1.88 \times 10^{-29} h^{2}$ $g/cm^{3}$ and the galactic scale $M_{gal}$ $\sim m^{3}_{Pl}/m^{2}_{J} \sim 10^{12} M_{\odot} (m_{J}/1 KeV)^{-2}$ for galaxy formation. | contribution 0.84 | 0.61 | 0.70 | asserted 0.86 |
| s1 | The majoron couples to leptons only through some new "directly interacting particles", called DIPS, and this provides the required smallness of the coupling constants. | method 0.67 | 0.43 | 0.05 | asserted 0.98 |
| s2 | If the masses of these DIPS are greater than the scale $V_s$ characterizing the spontaneous violation of the global lepton symmetry they are absent at the corresponding phase transition ($T \sim V_s$) and the majorons are produced during the phase transition, never being in thermal equilibrium during the history of the universe. | method 0.53 | 0.42 | 0.06 | asserted 0.95 |
| s3 | In the alternative case $m_{DIP} < V_{s}$ the majorons can be for a short period in thermal equilibrium. | method 0.36 | 0.35 | 0.03 | hedged possibility 0.97 |
| s4 | This scenario is not forbidden by nucleosynthesis and gives a reasonable growth factor for the density fluctuations compatible with COBE. | interpretation 0.53 | 0.57 | 0.10 | asserted 0.74 |
| s5 | A possible signature is an X-ray line at $E_\gamma = \frac{m_J}{2}$, produced by the decay $J \to \gamma + \gamma$. | result 0.58 | 0.54 | 0.08 | hedged possibility 0.97 |
| s6 | A model is described which realizes the possibility of the KeV majoron as DMP and may also lead to observable rates for decays such as $\mu \ra e \gamma$ and $\mu \ra 3e$. | contribution 0.87 | 0.81 | 0.22 | hedged possibility 0.93 |
What was examined, and what was not
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References
How the literature uses it
57 arXiv papers cite this in 72 sentences
Papers citing it · 44 sentences without a confident label
Compares with it 1 paper
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This can be understood from a comparison with the conventional Majoron models with type-I seesaw mechanism [ref] .
How low-scale Trinification sheds light in the flavour hierarchies, neutrino puzzle, dark matter and leptogenesis · The scalar sector · 0.93
Cites it as background 27 papers
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We include an additional complex scalar field, $Φ$ containing the Majoron [ref] , that acts as an intermediate state in the interactions of the inflaton and RHNs.
Gravity as a Portal to Reheating, Leptogenesis and Dark Matter · Dark matter & leptogenesis with a Majoron · 0.88
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Among WDM candidates, there are sterile neutrinos [ref] , majorons [ref] and light DM (LDM) particles [ref] .
Signatures of clumpy dark matter in the global 21 cm background signal · Introduction · 0.93
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Another dark matter candidate closely connected to the origin of neutrino masses and mixings is the majoron, our focus in this article [ref] .
Minimal Majoron Dark Matter from a Discrete $Z_N$ Gauge Symmetry · Introduction · 0.88
Discussion
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