We discuss the interplay between dark matter, leptogenesis and a new gauge boson $$Z^\prime $$ in the $$B-L$$ model. A fermion dark matter $$\chi $$ carrying $$U(1)_{B-L}$$ charge is introduced to the model but not coupling with other particles. We consider the Freeze-out and Freeze-in mechanisms, and obtain the correct relic density respectively. We have scanned the feasible parameter space and found that the dark matter direct detection experiments imposed the most stringent constraints on the parameter space. The constraint on the parameter space places a limit on the mass of dark matter with $$m_{\chi } \approx 1/2 M_{Z'}$$ within a narrow region in the case of the Freeze-out scenario, and we can obtain the right baryon asymmetry result in the case of $$m_{\chi }\subset [654$$ GeV, 664 GeV]. For the Freeze-in scenario, we have a much broader parameter space for $$m_{\chi }$$ and $$M_{Z^\prime }$$ but $$g_{BL}$$ is restricted at $$10^{-5}$$ level for $$Q=0.1$$ . In both scenarios, $$g_{BL}-M_{Z^\prime }$$ is limited within a narrow region by the dark matter relic density, direct detection and baryon asymmetry constraints.

China

XinXin Qi

Hao Sun

Dark matter, leptogenesis and $$Z^\prime $$ in the $$B-L$$ model

We construct a realistic supersymmetric model for superheavy metastable cosmic strings (CSs) that can be investigated in the current pulsar timing array (PTA) experiments. It is based on shifted <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>μ</mi></math>-hybrid inflation in which the symmetry breaking <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>U</mi><mo stretchy="false">(</mo><mn>1</mn><msub><mo stretchy="false">)</mo><mi>R</mi></msub><mo stretchy="false">→</mo><mi>S</mi><mi>U</mi><mo stretchy="false">(</mo><mn>3</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>U</mi><mo stretchy="false">(</mo><mn>1</mn><msub><mo stretchy="false">)</mo><mrow><mi>B</mi><mo>−</mo><mi>L</mi></mrow></msub><mo>×</mo><mi>U</mi><mo stretchy="false">(</mo><mn>1</mn><msub><mo stretchy="false">)</mo><mi>R</mi></msub></math> proceeds along an inflationary trajectory such that the topologically unstable primordial monopoles are inflated away. The breaking of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>U</mi><mo stretchy="false">(</mo><mn>1</mn><msub><mo stretchy="false">)</mo><mrow><mi>B</mi><mo>−</mo><mi>L</mi></mrow></msub><mo>×</mo><mi>U</mi><mo stretchy="false">(</mo><mn>1</mn><msub><mo stretchy="false">)</mo><mi>R</mi></msub><mo stretchy="false">→</mo><mi>U</mi><mo stretchy="false">(</mo><mn>1</mn><msub><mo stretchy="false">)</mo><mi>Y</mi></msub></math> after inflation ends yields the superheavy metastable CSs carrying the right handed neutrino zero modes that generate the stochastic gravitational wave background, which we show is consistent with the current PTA dataset and the LIGO O3 run. The scalar spectral index <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>n</mi><mi>s</mi></msub></math> and the tensor-to-scalar ratio <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>r</mi></math> are compatible with the Planck 2018 and Atacama Cosmology Telescope measurements. Both reheating and leptogenesis are briefly discussed.

Pakistan

Adeela Afzal

Maria Mehmood

Saudi Arabia

Mansoor Ur Rehman

United States

Qaisar Shafi

Supersymmetric hybrid inflation and current-carrying metastable cosmic strings 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>U</mi><mo stretchy="false">(</mo><mn>1</mn><msub><mo stretchy="false">)</mo><mi>R</mi></msub></math>

Thermal dark matter is a compelling setup that has been probed by a multitude of experiments, mostly in the GeV–TeV mass range. The thermal paradigm in the sub-GeV range is about to experience the same experimental test with the next generation of low-energy accelerators and light dark matter detectors. Motivated by this, we investigate thermal dark matter in the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>L</mi><mi>μ</mi></msub><mo>−</mo><msub><mi>L</mi><mi>τ</mi></msub></math> and assess how the introduction of a matter-dominated era impacts the parameter that yields the correct relic density. Interestingly, we show that the projected experiments, such as the Muon (Synchrotron) Ion Collider, Future Circular Collider-ee, and Light Dark Matter eXperiment, will probe a large region of the viable parameter space that yields the correct relic density. In the GeV–TeV mass regime, the usual large-scale detectors push the sensitivity. Our work highlights the rich interplay between early-Universe dynamics, dark matter phenomenology, and the discovery potential of next-generation experiments.

United Arab Emirates

Nicolás Bernal

Italy

Brazil

Jacinto P. Neto

Peru

Javier Silva-Malpartida

Chile

Farinaldo S. Queiroz

Enabling thermal dark matter within the vanilla <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msub><mrow><mi>L</mi></mrow><mrow><mi>μ</mi></mrow></msub><mo>−</mo><msub><mrow><mi>L</mi></mrow><mrow><mi>τ</mi></mrow></msub></mrow></math> model

The Muon <math altimg='si4.svg'><mrow><mi>g</mi><mo linebreak='goodbreak'>&#8722;</mo><mn>2</mn></mrow></math> collaboration at Fermilab has announced their final result of the anomalous magnetic moment of the muon. By adopting the lattice-QCD evaluation of the leading-order hadronic-vacuum-polarization, this result is now in agreement with the latest theoretical prediction to the <math altimg='si15.svg'><mrow><mn>1</mn><mi>&#963;</mi></mrow></math> level. This new result further constrains the allowed parameter space, but does not rule out all possible new physics contributions the muon <math altimg='si4.svg'><mrow><mi>g</mi><mo linebreak='goodbreak'>&#8722;</mo><mn>2</mn></mrow></math>. We study the implications for one of the relevant models, the gauged <math altimg='si12.svg'><mrow><mi>U</mi><msub><mrow><mo>(</mo><mn>1</mn><mo>)</mo></mrow><mrow><msub><mi>L</mi><mi>&#956;</mi></msub><mo>&#8722;</mo><msub><mi>L</mi><mi>&#964;</mi></msub></mrow></msub></mrow></math>. When using this model to resolve the previous <math altimg='si16.svg'><mrow><mn>4</mn><mi>&#963;</mi></mrow></math> tension, results from muon neutrino trident (MNT) scattering experiments would restrict the mass of the new gauge boson ( <math altimg='si17.svg'><msup><mi>Z</mi><mo>&#8242;</mo></msup></math>) to be less than 300 MeV. Since the theory and experimental data difference for muon <math altimg='si4.svg'><mrow><mi>g</mi><mo linebreak='goodbreak'>&#8722;</mo><mn>2</mn></mrow></math> is lowered down to <math altimg='si15.svg'><mrow><mn>1</mn><mi>&#963;</mi></mrow></math>, the requirement for <math altimg='si18.svg'><mrow><msub><mi>m</mi><msup><mi>Z</mi><mo>&#8242;</mo></msup></msub><mo>&#8818;</mo><mn>300</mn><mspace width='0.16em' /><mrow><mrow><mi mathvariant='normal'>M</mi></mrow><mi>e</mi><mi>V</mi></mrow></mrow></math> is much relaxed. Within the updated allowed range of <math altimg='si17.svg'><msup><mi>Z</mi><mo>&#8242;</mo></msup></math> boson mass, we study the models implications for electron and tauon <math altimg='si4.svg'><mrow><mi>g</mi><mo linebreak='goodbreak'>&#8722;</mo><mn>2</mn></mrow></math> as well as future muon colliders. We find that muon collider can effectively probe the <math altimg='si12.svg'><mrow><mi>U</mi><msub><mrow><mo>(</mo><mn>1</mn><mo>)</mo></mrow><mrow><msub><mi>L</mi><mi>&#956;</mi></msub><mo>&#8722;</mo><msub><mi>L</mi><mi>&#964;</mi></msub></mrow></msub></mrow></math>.

Ming-Wei Li

Xiao-Gang He

Andrew Cheek

Xinhui Chu

The <math altimg='si12.svg'><mrow><mi>U</mi><msub><mrow><mo>(</mo><mn>1</mn><mo>)</mo></mrow><mrow><msub><mi>L</mi><mi>&#956;</mi></msub><mo>&#8722;</mo><msub><mi>L</mi><mi>&#964;</mi></msub></mrow></msub></mrow></math> model meets the new <math altimg='si14.svg'><msub><mrow><mo>(</mo><mi>g</mi><mo>&#8722;</mo><mn>2</mn><mo>)</mo></mrow><mi>&#956;</mi></msub></math> data and muon neutrino trident scattering

Using <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mi>e</mi><mo>+</mo></msup><msup><mi>e</mi><mo>−</mo></msup></math> annihilation data corresponding to a total integrated luminosity of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>7.33</mn><mtext> </mtext><mtext> </mtext><msup><mrow><mi>fb</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></math> collected at center-of-mass energies between 4.128 and 4.226 GeV with the BESIII detector, we provide the first amplitude analysis and absolute branching fraction measurement of the hadronic decay <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msubsup><mrow><mi>D</mi></mrow><mrow><mi>s</mi></mrow><mrow><mo>+</mo></mrow></msubsup><mo stretchy="false">→</mo><msubsup><mrow><mi>K</mi></mrow><mrow><mi>S</mi></mrow><mrow><mn>0</mn></mrow></msubsup><msubsup><mrow><mi>K</mi></mrow><mrow><mi>L</mi></mrow><mrow><mn>0</mn></mrow></msubsup><msup><mrow><mi>π</mi></mrow><mrow><mo>+</mo></mrow></msup></mrow></math>. The branching fraction of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msubsup><mrow><mi>D</mi></mrow><mrow><mi>s</mi></mrow><mrow><mo>+</mo></mrow></msubsup><mo stretchy="false">→</mo><msubsup><mrow><mi>K</mi></mrow><mrow><mi>S</mi></mrow><mrow><mn>0</mn></mrow></msubsup><msubsup><mrow><mi>K</mi></mrow><mrow><mi>L</mi></mrow><mrow><mn>0</mn></mrow></msubsup><msup><mrow><mi>π</mi></mrow><mrow><mo>+</mo></mrow></msup></mrow></math> is determined to be <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mo stretchy="false">(</mo><mn>1.86</mn><mo>±</mo><mn>0.0</mn><msub><mrow><mn>6</mn></mrow><mrow><mi>stat</mi></mrow></msub><mo>±</mo><mn>0.0</mn><msub><mrow><mn>3</mn></mrow><mrow><mi>syst</mi></mrow></msub><mo stretchy="false">)</mo><mo>%</mo></mrow></math>. Combining the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mi mathvariant="script">B</mi><mo stretchy="false">[</mo><msubsup><mrow><mi>D</mi></mrow><mrow><mi>s</mi></mrow><mrow><mo>+</mo></mrow></msubsup><mo stretchy="false">→</mo><mi>ϕ</mi><mo stretchy="false">(</mo><mo stretchy="false">→</mo><msubsup><mrow><mi>K</mi></mrow><mrow><mi>S</mi></mrow><mrow><mn>0</mn></mrow></msubsup><msubsup><mrow><mi>K</mi></mrow><mrow><mi>L</mi></mrow><mrow><mn>0</mn></mrow></msubsup><mo stretchy="false">)</mo><msup><mrow><mi>π</mi></mrow><mrow><mo>+</mo></mrow></msup><mo stretchy="false">]</mo></mrow></math> obtained in this Letter and the world average of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mi mathvariant="script">B</mi><mo stretchy="false">[</mo><msubsup><mrow><mi>D</mi></mrow><mrow><mi>s</mi></mrow><mrow><mo>+</mo></mrow></msubsup><mo stretchy="false">→</mo><mi>ϕ</mi><mo stretchy="false">(</mo><mo stretchy="false">→</mo><msup><mrow><mi>K</mi></mrow><mrow><mo>+</mo></mrow></msup><msup><mrow><mi>K</mi></mrow><mrow><mo>−</mo></mrow></msup><mo stretchy="false">)</mo><msup><mrow><mi>π</mi></mrow><mrow><mo>+</mo></mrow></msup><mo stretchy="false">]</mo></mrow></math>, we measure the relative branching fraction <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mi mathvariant="script">B</mi><mo stretchy="false">(</mo><mi>ϕ</mi><mo stretchy="false">→</mo><msubsup><mrow><mi>K</mi></mrow><mrow><mi>S</mi></mrow><mrow><mn>0</mn></mrow></msubsup><msubsup><mrow><mi>K</mi></mrow><mrow><mi>L</mi></mrow><mrow><mn>0</mn></mrow></msubsup><mo stretchy="false">)</mo><mo>/</mo><mi mathvariant="script">B</mi><mo stretchy="false">(</mo><mi>ϕ</mi><mo stretchy="false">→</mo><msup><mrow><mi>K</mi></mrow><mrow><mo>+</mo></mrow></msup><msup><mrow><mi>K</mi></mrow><mrow><mo>−</mo></mrow></msup><mo stretchy="false">)</mo><mo>=</mo><mo stretchy="false">(</mo><mn>0.593</mn><mo>±</mo><mn>0.02</mn><msub><mrow><mn>3</mn></mrow><mrow><mi>stat</mi></mrow></msub><mo>±</mo><mspace linebreak="goodbreak"></mspace><mn>0.01</mn><msub><mrow><mn>4</mn></mrow><mrow><mi>syst</mi></mrow></msub><mo>±</mo><mn>0.01</mn><msub><mrow><mn>6</mn></mrow><mrow><mi>ϕ</mi><mi>π</mi></mrow></msub><mo stretchy="false">)</mo></mrow></math>, where the third error is due to the uncertainty of the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mi mathvariant="script">B</mi><mo stretchy="false">(</mo><msubsup><mrow><mi>D</mi></mrow><mrow><mi>s</mi></mrow><mrow><mo>+</mo></mrow></msubsup><mo stretchy="false">→</mo><mi>ϕ</mi><msup><mrow><mi>π</mi></mrow><mrow><mo>+</mo></mrow></msup><mo>,</mo><mi>ϕ</mi><mo stretchy="false">→</mo><msup><mrow><mi>K</mi></mrow><mrow><mo>+</mo></mrow></msup><msup><mrow><mi>K</mi></mrow><mrow><mo>−</mo></mrow></msup><mo stretchy="false">)</mo></mrow></math>. Our result deviates from the Particle Data Group value by more than <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>3</mn><mi>σ</mi></mrow></math>. Furthermore, the asymmetry of the branching fractions of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msubsup><mrow><mi>D</mi></mrow><mrow><mi>s</mi></mrow><mrow><mo>+</mo></mrow></msubsup><mo stretchy="false">→</mo><msubsup><mrow><mi>K</mi></mrow><mrow><mi>S</mi></mrow><mrow><mn>0</mn></mrow></msubsup><msup><mrow><mi>K</mi></mrow><mrow><mo>*</mo></mrow></msup><mo stretchy="false">(</mo><mn>892</mn><msup><mrow><mo stretchy="false">)</mo></mrow><mrow><mo>+</mo></mrow></msup></mrow></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msubsup><mrow><mi>D</mi></mrow><mrow><mi>s</mi></mrow><mrow><mo>+</mo></mrow></msubsup><mo stretchy="false">→</mo><msubsup><mrow><mi>K</mi></mrow><mrow><mi>L</mi></mrow><mrow><mn>0</mn></mrow></msubsup><msup><mrow><mi>K</mi></mrow><mrow><mo>*</mo></mrow></msup><mo stretchy="false">(</mo><mn>892</mn><msup><mrow><mo stretchy="false">)</mo></mrow><mrow><mo>+</mo></mrow></msup></mrow></math>, <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mo mathvariant="bold" stretchy="false">(</mo><mo stretchy="false">{</mo><mi mathvariant="script">B</mi><mo stretchy="false">[</mo><msubsup><mrow><mi>D</mi></mrow><mrow><mi>s</mi></mrow><mrow><mo stretchy="false">+</mo></mrow></msubsup><mo stretchy="false">→</mo><msubsup><mrow><mi>K</mi></mrow><mrow><mi>S</mi></mrow><mrow><mn>0</mn></mrow></msubsup><msup><mrow><mi>K</mi></mrow><mrow><mo stretchy="false">*</mo></mrow></msup><mo stretchy="false">(</mo><mn>892</mn><msup><mrow><mo stretchy="false">)</mo></mrow><mrow><mo stretchy="false">+</mo></mrow></msup><mo stretchy="false">]</mo><mo stretchy="false">−</mo><mspace linebreak="goodbreak"></mspace><mi mathvariant="script">B</mi><mo stretchy="false">[</mo><msubsup><mrow><mi>D</mi></mrow><mrow><mi>s</mi></mrow><mrow><mo stretchy="false">+</mo></mrow></msubsup><mo stretchy="false">→</mo><msubsup><mrow><mi>K</mi></mrow><mrow><mi>L</mi></mrow><mrow><mn>0</mn></mrow></msubsup><msup><mrow><mi>K</mi></mrow><mrow><mo stretchy="false">*</mo></mrow></msup><mo stretchy="false">(</mo><mn>892</mn><msup><mrow><mo stretchy="false">)</mo></mrow><mrow><mo stretchy="false">+</mo></mrow></msup><mo stretchy="false">]</mo><mo stretchy="false">}</mo><mo>/</mo><mo stretchy="false">{</mo><mi mathvariant="script">B</mi><mo stretchy="false">[</mo><msubsup><mrow><mi>D</mi></mrow><mrow><mi>s</mi></mrow><mrow><mo stretchy="false">+</mo></mrow></msubsup><mo stretchy="false">→</mo><msubsup><mrow><mi>K</mi></mrow><mrow><mi>S</mi></mrow><mrow><mn>0</mn></mrow></msubsup><msup><mrow><mi>K</mi></mrow><mrow><mo stretchy="false">*</mo></mrow></msup><mo stretchy="false">(</mo><mn>892</mn><msup><mrow><mo stretchy="false">)</mo></mrow><mrow><mo stretchy="false">+</mo></mrow></msup><mo stretchy="false">]</mo><mo stretchy="false">+</mo><mi mathvariant="script">B</mi><mo stretchy="false">[</mo><msubsup><mrow><mi>D</mi></mrow><mrow><mi>s</mi></mrow><mrow><mo stretchy="false">+</mo></mrow></msubsup><mo stretchy="false">→</mo><msubsup><mrow><mi>K</mi></mrow><mrow><mi>L</mi></mrow><mrow><mn>0</mn></mrow></msubsup><msup><mrow><mi>K</mi></mrow><mrow><mo stretchy="false">*</mo></mrow></msup><mo stretchy="false">(</mo><mn>892</mn><msup><mrow><mo stretchy="false">)</mo></mrow><mrow><mo stretchy="false">+</mo></mrow></msup><mo stretchy="false">]</mo><mo stretchy="false">}</mo><mo mathvariant="bold" stretchy="false">)</mo></mrow></math>, is determined to be <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mo stretchy="false">(</mo><mo>−</mo><mn>14.5</mn><mo>±</mo><msub><mn>5.1</mn><mrow><mi>stat</mi></mrow></msub><mo>±</mo><msub><mn>1.8</mn><mrow><mi>syst</mi></mrow></msub><mo stretchy="false">)</mo><mo>%</mo></math>.

M. Ablikim

Russia

M.N. Achasov

Sweden

P. Adlarson

X.C. Ai

Germany

R. Aliberti

A. Amoroso

Q. An

Y. Bai

JINR

O. Bakina

Y. Ban

H.R. Bao

Poland

V. Batozskaya

Mongolia

K. Begzsuren

N. Berger

M. Berlowski

M. Bertani

D. Bettoni

F. Bianchi

E. Bianco

A. Bortone

I. Boyko

R.A. Briere

A. Brueggemann

H. Cai

M.H. Cai

X. Cai

A. Calcaterra

G.F. Cao

N. Cao

Türkiye

S.A. Cetin

X.Y. Chai

J.F. Chang

G.R. Che

Y.Z. Che

G. Chelkov

C.H. Chen

Chao Chen

G. Chen

H.S. Chen

H.Y. Chen

M.L. Chen

S.J. Chen

S.L. Chen

S.M. Chen

T. Chen

X.R. Chen

X.T. Chen

X.Y. Chen

Y.B. Chen

Y.Q. Chen

Z.J. Chen

Z.K. Chen

South Korea

S.K. Choi

X. Chu

G. Cibinetto

F. Cossio

United Kingdom

J. Cottee-Meldrum

J.J. Cui

H.L. Dai

J.P. Dai

A. Dbeyssi

R.E. de Boer

D. Dedovich

C.Q. Deng

Z.Y. Deng

A. Denig

I. Denysenko

M. Destefanis

F. De Mori

B. Ding

X.X. Ding

Y. Ding

Y.X. Ding

J. Dong

L.Y. Dong

M.Y. Dong

X. Dong

M.C. Du

S.X. Du

Y.Y. Duan

Z.H. Duan

P. Egorov

G.F. Fan

J.J. Fan

Y.H. Fan

J. Fang

S.S. Fang

W.X. Fang

Y.Q. Fang

R. Farinelli

L. Fava

F. Feldbauer

G. Felici

C.Q. Feng

J.H. Feng

L. Feng

Study of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mi>ϕ</mi><mo stretchy="false">→</mo><mi>K</mi><mover accent="true"><mrow><mi>K</mi></mrow><mrow><mo stretchy="false">¯</mo></mrow></mover></mrow></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msubsup><mrow><mi>K</mi></mrow><mrow><mi>S</mi></mrow><mrow><mn>0</mn></mrow></msubsup><mo>−</mo><msubsup><mrow><mi>K</mi></mrow><mrow><mi>L</mi></mrow><mrow><mn>0</mn></mrow></msubsup></mrow></math> Asymmetry in the Amplitude Analysis of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msubsup><mrow><mi>D</mi></mrow><mrow><mi>s</mi></mrow><mrow><mo>+</mo></mrow></msubsup><mo stretchy="false">→</mo><msubsup><mrow><mi>K</mi></mrow><mrow><mi>S</mi></mrow><mrow><mn>0</mn></mrow></msubsup><msubsup><mrow><mi>K</mi></mrow><mrow><mi>L</mi></mrow><mrow><mn>0</mn></mrow></msubsup><msup><mrow><mi>π</mi></mrow><mrow><mo>+</mo></mrow></msup></mrow></math> Decays

We study the longitudinal beam single spin asymmetry <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msubsup><mi>A</mi><mrow><mi>L</mi><mi>U</mi></mrow><mrow><mi>sin</mi><msub><mi>ϕ</mi><mi>R</mi></msub></mrow></msubsup></math> of dihadron production in the semi-inclusive deep inelastic scattering process with a polarized electron beam scattering off an unpolarized proton target. The asymmetry arises from the convolutions of the twist-3 parton distribution function (PDF) <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>e</mi><mo stretchy="false">(</mo><mi>x</mi><mo stretchy="false">)</mo></math> and the twist-2 dihadron fragmentation function (DiFF) <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msubsup><mrow><mi>H</mi></mrow><mrow><mn>1</mn></mrow><mrow><mo>∢</mo></mrow></msubsup></mrow></math> as well as the twist-2 PDF <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>f</mi><mn>1</mn></msub><mo stretchy="false">(</mo><mi>x</mi><mo stretchy="false">)</mo></math> and the twist-3 DiFF <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msup><mrow><mover accent="true"><mrow><mi>G</mi></mrow><mrow><mo stretchy="false">˜</mo></mrow></mover></mrow><mrow><mo>∢</mo></mrow></msup></mrow></math>. Using the spectator model calculations for the twist-3 PDF <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>e</mi><mo stretchy="false">(</mo><mi>x</mi><mo stretchy="false">)</mo></math> and the DiFFs <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msub><mrow><mi>D</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>,</mo><msubsup><mrow><mi>H</mi></mrow><mrow><mn>1</mn></mrow><mrow><mo>∢</mo></mrow></msubsup></mrow></math>, and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msup><mrow><mover accent="true"><mrow><mi>G</mi></mrow><mrow><mo stretchy="false">˜</mo></mrow></mover></mrow><mrow><mo>∢</mo></mrow></msup></mrow></math>, we estimate the beam single spin asymmetry (BSA) <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msubsup><mi>A</mi><mrow><mi>L</mi><mi>U</mi></mrow><mrow><mi>sin</mi><msub><mi>ϕ</mi><mi>R</mi></msub></mrow></msubsup></math> at the kinematical configuration of CLAS and CLAS12. We find good agreement with <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>z</mi></math>- and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>M</mi><mi>h</mi></msub></math>-dependencies data, though <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>x</mi></math>- and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mi>Q</mi><mn>2</mn></msup></math>-dependencies show discrepancies. We include the Dokshitzer-Gribov-Lipatov-Altarelli-Parisi evolution of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>e</mi><mo stretchy="false">(</mo><mi>x</mi><mo stretchy="false">)</mo></math> and provide predictions for COMPASS, EIC, and EicC. The negligible contribution from <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msub><mrow><mi>f</mi></mrow><mrow><mn>1</mn></mrow></msub><mo stretchy="false">(</mo><mi>x</mi><mo stretchy="false">)</mo><mo stretchy="false">⊗</mo><msup><mrow><mover accent="true"><mrow><mi>G</mi></mrow><mrow><mo stretchy="false">˜</mo></mrow></mover></mrow><mrow><mo>∢</mo></mrow></msup></mrow></math> supports the Wandzura-Wilczek approximation, while our results highlight the importance of QCD evolution in twist-3 PDF analyses.

Yanli Li

Keyang She

Hui Li

Xiaoyu Wang

De-Min Li

Zhun Lu

Beam single spin asymmetry <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msubsup><mrow><mi>A</mi></mrow><mrow><mi>L</mi><mi>U</mi></mrow><mrow><mi>sin</mi><msub><mrow><mi>ϕ</mi></mrow><mrow><mi>R</mi></mrow></msub></mrow></msubsup></mrow></math> of the dihadron production in SIDIS process

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.

Thomas W. Kephart

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.

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

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

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.

Aritra Biswas

Nico Gubernari

Spain

Joaquim Matias

Gilberto Tetlalmatzi-Xolocotzi

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