In the Pati-Salam gauge symmetry <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>S</mi><mi>U</mi><mo stretchy="false">(</mo><mn>4</mn><msub><mo stretchy="false">)</mo><mi>c</mi></msub><mo>×</mo><mi>S</mi><mi>U</mi><mo stretchy="false">(</mo><mn>2</mn><msub><mo stretchy="false">)</mo><mi>L</mi></msub><mo>×</mo><mi>S</mi><mi>U</mi><mo stretchy="false">(</mo><mn>2</mn><msub><mo stretchy="false">)</mo><mi>R</mi></msub></math> (4-2-2, for short), the observed quarks and leptons of each family reside in the bi-fundamental representations (4,2,1) and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mo stretchy="false">(</mo><mover accent="true"><mn>4</mn><mo stretchy="false">¯</mo></mover><mo>,</mo><mn>1</mn><mo>,</mo><mn>2</mn><mo stretchy="false">)</mo></math>. There exist, however, the fundamental representations (4,1,1), (1,2,1), and (1,1,2) and their Hermitian conjugates, which show the presence, in principle, of yet to be discovered color triplets that carry electric charge <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mo>±</mo><mrow><mi>e</mi><mo>/</mo><mn>6</mn></mrow></math>, and color singlet particles with charges of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mo>±</mo><mrow><mi>e</mi><mo>/</mo><mn>2</mn></mrow></math>. These standard model charges are in full accord with the fact that the 4-2-2 model predicts the presence of a topologically stable, finite energy magnetic monopole that carries two quanta of Dirac magnetic charge, i.e., <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mn>4</mn><mi>π</mi><mo>/</mo><mi>e</mi></math>, as well as color magnetic charge that is screened beyond the quark confinement scale. The 4-2-2 model, therefore, predicts the existence of exotic baryons, mesons, and leptons that carry fractional (<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mo>±</mo><mrow><mi>e</mi><mo>/</mo><mn>2</mn></mrow></math>) electric charges. Since their origin lies in the fundamental representations of 4-2-2, these exotic particles may turn out to be relatively light, in the TeV mass range or so. The 4-2-2 magnetic monopole mass depends on the 4-2-2 symmetry breaking scale, which is approximately 100 TeV.

United States

Thomas W. Kephart

Qaisar Shafi

Magnetic monopoles and exotic states in <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>S</mi><mi>U</mi><mo stretchy="false">(</mo><mn>4</mn><msub><mo stretchy="false">)</mo><mi>c</mi></msub><mo>×</mo><mi>S</mi><mi>U</mi><mo stretchy="false">(</mo><mn>2</mn><msub><mo stretchy="false">)</mo><mi>L</mi></msub><mo>×</mo><mi>S</mi><mi>U</mi><mo stretchy="false">(</mo><mn>2</mn><msub><mo stretchy="false">)</mo><mi>R</mi></msub></math>

In this study, we construct a traversable wormhole solution within the framework of <math altimg='si16.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> gravity by assuming conformal symmetry. The matter content is modeled using phantom energy, characterized by an equation of state parameter <math altimg='si17.svg'><mrow><mi>&#969;</mi><mo linebreak='goodbreak'>&lt;</mo><mo>&#8722;</mo><mn>1</mn></mrow></math>, which inherently violates the null energy condition. By employing conformal Killing vector symmetry, we derive exact analytical expressions for the shape function, energy density, and pressure components of the anisotropic fluid. Our analysis includes a detailed examination of the flare-out condition, proper radial distance, embedding diagrams, and the generalized Tolman-Oppenheimer-Volkoff equation. Notably, the model yields a positive active gravitational mass and positive total gravitational energy, despite the presence of exotic matter.

Türkiye

Doğukan Taşer

Existence of conformal symmetric wormhole with phantom energy in <math altimg='si16.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> theory

We explore the impact of a combined analysis of $\textit{B}$ → $\textit{K}$ form factors on a set of $\textit{L}$-observables. The $\textit{L}$-observables are constructed from ratios of branching fractions in $\textit{B}$ → $\textit{VV}$, $\textit{PP}$, $\textit{PV}$ versus $\textit{B}$ → $\textit{VV}$, $\textit{PP}$, $\textit{PV}$ decays with $\textit{P}$ = $\textit{K}$ , $$ {\overline{K}}^0 $$ and $\textit{V}$ = $\textit{K}$ , $$ {\overline{K}}^{\ast 0} $$ , thereby partially reducing their hadronic uncertainties. We show the change of the Standard Model predictions of the $\textit{L}$-observables under different determinations of the ratio of the relevant form factors (with correlations) including lattice QCD data and a novel light-cone sum rule analysis. In addition, we provide precise results for all $\textit{B}$ → $\textit{K}$ form factors in machine-readable files. We find that the inclusion of our up-to-date results, as well as the use or omission of lattice QCD data for the form factors, has a significant impact on the $\textit{L}$-observables. We also discuss how the New Physics interpretation is affected by the updated form factors and present revised predictions for the mechanism identified in our analysis of $\textit{B}$ → $\textit{VP}$ decays, now employing more suitable new experimental observables defined in this paper.

Germany

Aritra Biswas

United Kingdom

Nico Gubernari

Spain

Joaquim Matias

Gilberto Tetlalmatzi-Xolocotzi

Impact on $\textit{L}$-observables of a new combined analysis of $\textit{B}$

In this study, we investigate the viability of the <math altimg='si4.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi mathvariant='script'>L</mi><mi>m</mi></msub><mo>)</mo></mrow></math> gravity framework in explaining the accelerated expansion of the universe within the context of the locally rotationally symmetric (LRS) Bianchi-I space-time. Modified gravity theories have emerged as promising alternatives to General Relativity (GR) to account for cosmic acceleration and dark energy phenomena. We employ observational constraints from Type Ia Supernovae (SN Ia), Baryon Acoustic Oscillations (BAO), and Cosmic Chronometers (CC) to calibrate the free parameters of our model. The field equations are formulated based on a specific functional form of <math altimg='si4.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi mathvariant='script'>L</mi><mi>m</mi></msub><mo>)</mo></mrow></math>, and analytical solutions are obtained. The Hubble parameter, deceleration parameter ( <math altimg='si10.svg'><mi>q</mi></math>), statefinder diagnostics <math altimg='si74.svg'><mrow><mo>(</mo><mi>r</mi><mo>,</mo><mi>s</mi><mo>)</mo></mrow></math>, and the jerk parameter ( <math altimg='si12.svg'><mi>j</mi></math>) are utilized to analyze the evolutionary dynamics of the universe. Our results indicate a transition from a decelerating to an accelerating phase, with the transition redshift <math altimg='si75.svg'><mrow><msub><mi>z</mi><mi>t</mi></msub><mo linebreak='goodbreak'>=</mo><mn>0</mn><mo>.</mo><msubsup><mn>7293</mn><mrow><mo>&#8722;</mo><mn>0.06</mn></mrow><mrow><mo>+</mo><mn>0.07</mn></mrow></msubsup></mrow></math> and present deceleration parameter <math altimg='si76.svg'><mrow><msub><mi>q</mi><mn>0</mn></msub><mo linebreak='goodbreak'>=</mo><mo>&#8722;</mo><mn>0.56</mn></mrow></math>, consistent with observational data. The estimated age of the universe in this framework is <math altimg='si77.svg'><mrow><mn>13.27</mn><mo>&#177;</mo><mn>0.26</mn></mrow></math> Gyrs. The statefinder parameters suggest that the model closely mimics the standard <math altimg='si5.svg'><mstyle mathvariant='normal'><mi>&#923;</mi></mstyle></math>CDM scenario at present but exhibits deviations at earlier epochs, potentially indicating a dynamic nature of dark energy. The <math altimg='si78.svg'><msub><mi>O</mi><mi>m</mi></msub></math> diagnostic further confirms the compatibility of our model with a phantom-like behavior of dark energy. These findings support the viability of <math altimg='si4.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi mathvariant='script'>L</mi><mi>m</mi></msub><mo>)</mo></mrow></math> gravity as an alternative framework for explaining cosmic acceleration, providing new interplay between matter and curvature in gravitational dynamics.

India

Vinod Kumar Bhardwaj

Anil Kumar Yadav

S.H. Shekh

Constraining <math altimg='si4.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi mathvariant='script'>L</mi><mi>m</mi></msub><mo>)</mo></mrow></math> gravity with SN Ia and BAO observational data in Bianchi I space time

In the field of particle physics, the phenomenon of dihadron production in semi-inclusive deep inelastic scattering (SIDIS) process has always been a significant focus. This paper focuses on the single longitudinal spin asymmetry $$A_{UL }^{\sin (3\phi _{h}-\phi _{R})}$$ in the dihadron production during this process and combines the transverse-momentum-dependent dihadron fragmentation function (DiFF) $$H_1^{\perp }$$ to deeply analyze its underlying mechanism. Here, the involved DiFF $$H_1^{\perp }$$ is the analogue of the Collins function for single-hadron production and it describes the fragmentation of a transversely polarized quark at leading twist. Recent studies have shown that the azimuthal asymmetry signal observed by the COMPASS collaboration in the dihadron SIDIS is weak. To reveal the reason for this small signal and to study the asymmetry, we calculate the unknown T-odd DiFF $$H_1^{\perp }$$ using the spectator model. The spectator model, widely used in SIDIS, describes the internal structure of hadrons and the hadronization mechanism. This model has successfully explained dihadron production in unpolarized and single-polarized processes. During the research process, while maintaining the transverse momentum dependence of the hadron pair, we employ the transverse momentum dependent(TMD) factorization framework, using this method and the model, we first simulate the asymmetry in the COMPASS energy region and compare it with experimental data. Furthermore, we predict the same asymmetry at the HERMES, expecting to provide valuable theoretical references for relevant experimental studies.

China

Lei Tan

Gang Li

Mao Song

Xuan Luo

Single spin asymmetry $$ A _ { U L } ^ { \sin ( 3 \phi _ { h } - \phi _{ R } ) }$$ in dihadron production in SIDIS

The late-time acceleration of the universe remains one of the central challenges in modern cosmology, motivating both dynamical dark energy models and extensions of general relativity. In this work, we investigate the cosmology of the recently proposed <math altimg='si5.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> gravity framework, which generalizes the <math altimg='si34.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> and <math altimg='si35.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>)</mo></mrow></math> models by incorporating the Ricci scalar <math altimg='si36.svg'><mi>R</mi></math>, the matter Lagrangian <math altimg='si37.svg'><msub><mi>L</mi><mi>m</mi></msub></math>, and the trace of the energy-momentum tensor <math altimg='si38.svg'><mi>T</mi></math> within a unified gravitational action. By adopting the simplest functional form <math altimg='si39.svg'><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow><mo linebreak='goodbreak'>=</mo><mi>R</mi><mo linebreak='goodbreak'>+</mo><mi>&#945;</mi><msub><mi>L</mi><mi>m</mi></msub><mo linebreak='goodbreak'>+</mo><mi>&#946;</mi><mi>T</mi><mo linebreak='goodbreak'>+</mo><mi>&#947;</mi></mrow></math>, we derive modified Friedmann equations in a dust-dominated FLRW background and constrain the parameters <math altimg='si40.svg'><mrow><mo>(</mo><msub><mi>H</mi><mn>0</mn></msub><mo>,</mo><mi>&#945;</mi><mo>,</mo><mi>&#946;</mi><mo>,</mo><mi>&#947;</mi><mo>)</mo></mrow></math> using cosmic chronometers (CC), Type Ia supernovae from the PantheonPlus (PP)+SH0ES compilation, and their joint dataset. The inferred Hubble constant values are <math altimg='si41.svg'><mrow><msub><mi>H</mi><mn>0</mn></msub><mo linebreak='goodbreak'>=</mo><mn>68.69</mn><mo>&#177;</mo><mn>0.52</mn></mrow></math> km/s/Mpc (CC), <math altimg='si23.svg'><mrow><mn>72.75</mn><mo>&#177;</mo><mn>0.15</mn></mrow></math> km/s/Mpc (PP+SH0ES), and <math altimg='si26.svg'><mrow><mn>72</mn><mo>.</mo><msubsup><mn>68</mn><mrow><mo>&#8722;</mo><mn>0.12</mn></mrow><mrow><mo>+</mo><mn>0.15</mn></mrow></msubsup></mrow></math> km/s/Mpc (Joint), while the corresponding deceleration parameters are <math altimg='si42.svg'><mrow><msub><mi>q</mi><mn>0</mn></msub><mo>&#8764;</mo><mo>&#8722;</mo><mn>0.561</mn></mrow></math>, <math altimg='si43.svg'><mrow><msub><mi>q</mi><mn>0</mn></msub><mo>&#8764;</mo><mo>&#8722;</mo><mn>0.451</mn></mrow></math>, and <math altimg='si44.svg'><mrow><msub><mi>q</mi><mn>0</mn></msub><mo>&#8764;</mo><mo>&#8722;</mo><mn>0.458</mn></mrow></math>, respectively. Notably, the obtained <math altimg='si1.svg'><msub><mi>H</mi><mn>0</mn></msub></math> values lie between early-universe and local measurements, indicating that the model can accommodate both low- and high-redshift datasets, partially easing the Hubble tension. The <math altimg='si13.svg'><mrow><mi>O</mi><mi>m</mi><mo>(</mo><mi>z</mi><mo>)</mo></mrow></math> diagnostic analyses reveal a quintessence-like evolution of the cosmic energy density, distinguishing this framework from the standard <math altimg='si9.svg'><mstyle mathvariant='normal'><mi>&#923;</mi></mstyle></math>CDM model while preserving late-time acceleration.

Morocco

M. Koussour

Saudi Arabia

M.K.M. Ali

Uzbekistan

S. Muminov

J. Rayimbaev

Observational constraints on cosmic expansion in <math altimg='si5.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> gravity

In this paper, we present intriguing traversable and asymptotically flat wormhole solutions within <math altimg='si18.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> gravity. We integrate our model with the gravitational analog of the Schwinger effect, describing the emergence of particle-antiparticle pairs from the vacuum. By introducing a fundamental minimal length via the generalized uncertainty principle, we establish critical constraints on matter distribution and spacetime structure. Our findings reveal how this fundamental length shapes the wormhole geometry, steepening the slope toward the throat and mitigating violations of the weak and null energy conditions. This adjustment allows the supporting matter to avoid phantom behavior at the Planck scale, suggesting a more stable configuration. We also explore the intriguing effects of gravitational lensing, showing that these exotic wormholes repel light rather than capture it. For <math altimg='si9.svg'><mi>&#946;</mi></math> values ranging from 0 to 45, the deflection angle remains negative for all corresponding <math altimg='si14.svg'><mrow><mi>&#945;</mi><mo>(</mo><msub><mi>r</mi><mrow><mi>t</mi><mi>p</mi></mrow></msub><mo>)</mo></mrow></math> values, indicating a repulsive gravitational force that pushes photons away from the throat. Moreover, the forces acting on the wormhole exhibit a delicate balance, demonstrating equal strength in opposing directions&#8211;an essential feature of stability. The complexity factor <math altimg='si17.svg'><msub><mi>Y</mi><mrow><mi>T</mi><mi>F</mi></mrow></msub></math> decreases with distance from the throat, indicating that corrections from the generalized uncertainty principle are most significant near the throat and diminish outward. Overall, our work highlights the allure of these wormhole geometries and the pivotal role of quantum effects in their formation, paving new avenues for understanding gravity and spacetime.

South Africa

Azerbaijan

A. Errehymy

B. Turimov

Kazakhstan

A. Syzdykova

K. Myrzakulov

N. Alessa

A.H. Abdel-Aty

Dymnikova-Schwinger GUP-corrected wormholes in <math altimg='si18.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> gravity

We propose a symplectic structure for the phase space of a generic Lagrangian field theory expressed in the framework of $\textit{L}$ algebras. The symplectic structure does not require explicit knowledge of the derivative content of the Lagrangian, and therefore is applicable to nonlocal models, such as string field theory, where traditional constructions are difficult to apply. We test our proposal in a number of examples ranging from general relativity to $\textit{p}$-adic string theory.

Czechia

Vinícius Bernardes

Theodore Erler

Atakan Fırat

Covariant phase space and $\textit{L}$

We measure the spin-density matrix elements (SDMEs) for the photoproduction of <math xmlns="http://www.w3.org/1998/Math/MathML"><mrow><mi>ϕ</mi><mo>(</mo><mn>1020</mn><mo>)</mo></mrow></math> off of the proton in its decay to <math xmlns="http://www.w3.org/1998/Math/MathML"><mrow><msubsup><mi>K</mi><mi>S</mi><mn>0</mn></msubsup><msubsup><mi>K</mi><mi>L</mi><mn>0</mn></msubsup></mrow></math>, using 105 <math xmlns="http://www.w3.org/1998/Math/MathML"><msup><mrow><mi>pb</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></math> of data collected with a linearly polarized photon beam using the GlueX experiment. The SDMEs are measured in nine bins of the squared four-momentum transfer <math xmlns="http://www.w3.org/1998/Math/MathML"><mi>t</mi></math> in the range <math xmlns="http://www.w3.org/1998/Math/MathML"><mrow><mo>−</mo><mi>t</mi><mo>=</mo><mn>0.15</mn><mo>−</mo><mn>1.0</mn></mrow></math> <math xmlns="http://www.w3.org/1998/Math/MathML"><msup><mrow><mi>GeV</mi></mrow><mn>2</mn></msup></math>, providing the first measurement of their <math xmlns="http://www.w3.org/1998/Math/MathML"><mi>t</mi></math> dependence for photon beam energies of <math xmlns="http://www.w3.org/1998/Math/MathML"><mrow><msub><mi>E</mi><mi>γ</mi></msub><mo>=</mo><mn>8.2</mn><mo>−</mo><mn>8.8</mn></mrow></math> GeV. We confirm the dominance of Pomeron exchange in this region and put constraints on the contribution of other Regge exchanges. We also find that helicity amplitudes where the helicity of the photon and <math xmlns="http://www.w3.org/1998/Math/MathML"><mrow><mi>ϕ</mi><mo>(</mo><mn>1020</mn><mo>)</mo></mrow></math> differ by two units are negligible.

F. Afzal

C.S. Akondi

M. Albrecht

M. Amaryan

S. Arrigo

V. Arroyave

A. Asaturyan

A. Austregesilo

Z. Baldwin

F. Barbosa

J. Barlow

E. Barriga

R. Barsotti

D. Barton

V. Baturin

V.V. Berdnikov

T. Black

W. Boeglin

M. Boer

W.J. Briscoe

T. Britton

R. Brunner

S. Cao

E. Chudakov

G. Chung

P.L. Cole

O. Cortes

V. Crede

M.M. Dalton

D. Darulis

A. Deur

S. Dobbs

Russia

A. Dolgolenko

M. Dugger

R. Dzhygadlo

D. Ebersole

M. Edo

H. Egiyan

T. Erbora

P. Eugenio

A. Fabrizi

C. Fanelli

S. Fang

A.M. Foda

M. Fritsch

S. Furletov

L. Gan

H. Gao

A. Gardner

A. Gasparian

D.I. Glazier

C. Gleason

V.S. Goryachev

B. Grube

J. Guo

L. Guo

J. Hernandez

K. Hernandez

N.D. Hoffman

Canada

D. Hornidge

Chile

G. Huber

P. Hurck

W. Imoehl

D.G. Ireland

M.M. Ito

I. Jaegle

N.S. Jarvis

T. Jeske

M. Jing

R.T. Jones

Armenia

V. Kakoyan

G. Kalicy

V. Khachatryan

Greece

C. Kourkoumelis

A. LaDuke

I. Larin

D. Lawrence

D.I. Lersch

H. Li

B. Liu

K. Livingston

L. Lorenti

V. Lyubovitskij

A. Mahmood

H. Marukyan

V. Matveev

M. McCaughan

M. McCracken

C.A. Meyer

R. Miskimen

R.E. Mitchell

K. Mizutani

P. Moran

V. Neelamana

L. Ng

E. Nissen

S. Orešić

A.I. Ostrovidov

Z. Papandreou

C. Paudel

Measurement of spin-density matrix elements in <math xmlns="http://www.w3.org/1998/Math/MathML"><mrow><mi>ϕ</mi><mrow><mo>(</mo><mn>1020</mn><mo>)</mo></mrow><mo>→</mo><msubsup><mi>K</mi><mi>S</mi><mn>0</mn></msubsup><msubsup><mi>K</mi><mi>L</mi><mn>0</mn></msubsup></mrow></math> photoproduction with a linearly polarized photon beam at <math xmlns="http://www.w3.org/1998/Math/MathML"><mrow><msub><mi>E</mi><mi>γ</mi></msub><mo>=</mo><mn>8.2</mn><mo>–</mo><mn>8.8</mn><mo> </mo><mi>GeV</mi></mrow></math>

The radiative seesaw model with gauged <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mrow><mi mathvariant="normal">U</mi><mo stretchy="false">(</mo><mn>1</mn><mo stretchy="false">)</mo></mrow><mrow><mi>B</mi><mo>−</mo><mi>L</mi></mrow></msub><mo>×</mo><msub><mi mathvariant="double-struck">Z</mi><mn>2</mn></msub></math> extension is a well-motivated scenario that gives consistent predictions of active neutrino masses and the abundance of dark matter. Majorana masses of right-handed neutrinos, the lightest of which can be identified as dark matter, are given by the spontaneous breaking of the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mrow><mi mathvariant="normal">U</mi><mo stretchy="false">(</mo><mn>1</mn><mo stretchy="false">)</mo></mrow><mrow><mi>B</mi><mo>−</mo><mi>L</mi></mrow></msub></math> gauge symmetry. We revisit this model with the latest constraints from dark-matter searches, neutrino oscillations, flavor experiments, and collider experiments. We examine several benchmark scenarios and identify the valid parameter space of this model, finding that there are still allowed regions under the latest experimental constraints. We present new viable benchmark scenarios for this model, i.e., the right-handed neutrino dark-matter scenario and the scalar dark-matter scenario. We also mention the testability of these benchmark scenarios in future experiments.

Japan

Shinya Kanemura

Yushi Mura

Guohao Ying

Revisiting the model for radiative neutrino masses with dark matter in the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mstyle mathvariant="normal"><mi>U</mi></mstyle><mo stretchy="false">(</mo><mn>1</mn><msub><mrow><mo stretchy="false">)</mo></mrow><mrow><mi>B</mi><mo>−</mo><mi>L</mi></mrow></msub></mrow></math> gauge theory