We construct superinvariants in M-theory via local supersymmetry, which include ($\textit{DF}$) terms and fermionic bilinear terms with mass dimension eight. The bases of the ($\textit{DF}$) and the fermionic bilinear terms are classified and the variations under the local supersymmetry are evaluated by using the Mathematica codes. By imposing the local supersymmetry, we find that 24 independent terms of ($\textit{DF}$) are governed by 10 parameters. The result is consistent with the effective action obtained by analyzing scattering amplitudes of superparticles or supermembranes.

Japan

Yoshifumi Hyakutake

Effective action in M-theory: ($\textit{DF}$)

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

Uzbekistan

B. Turimov

Kazakhstan

A. Syzdykova

K. Myrzakulov

Saudi Arabia

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

<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mtext>DMRadio-</mtext><msup><mrow><mi mathvariant="normal">m</mi></mrow><mrow><mn>3</mn></mrow></msup></mrow></math> is an experimental search for dark matter axions. It uses a solenoidal dc magnetic field to convert an axion dark-matter signal to an ac electromagnetic response in a coaxial copper pickup. The current induced by this axion signal is measured by dc SQUIDs. <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mtext>DMRadio-</mtext><msup><mrow><mi mathvariant="normal">m</mi></mrow><mrow><mn>3</mn></mrow></msup></mrow></math> is designed to be sensitive to Kim-Shifman-Vainshtein-Zakharov (KSVZ) and Dine-Fischler-Srednicki-Zhitnisky (DFSZ) QCD axion models in the 10–200 MHz (<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>41</mn><mtext> </mtext><mtext> </mtext><mi>neV</mi><mo>/</mo><msup><mi>c</mi><mn>2</mn></msup><mi>–</mi><mrow><mn>0.83</mn><mtext> </mtext><mtext> </mtext><mi mathvariant="normal">μ</mi><mi>eV</mi><mo>/</mo><msup><mi>c</mi><mn>2</mn></msup></mrow></mrow></math>) range, and to axions with <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>g</mi><mrow><mi>a</mi><mi>γ</mi><mi>γ</mi></mrow></msub><mo>=</mo><msub><mi>g</mi><mrow><mi>a</mi><mi>γ</mi><mi>γ</mi><mo>,</mo><mrow><mi>DFSZ</mi></mrow></mrow></msub><mo stretchy="false">(</mo><mn>30</mn><mtext> </mtext><mtext> </mtext><mi>MHz</mi><mo stretchy="false">)</mo><mo>=</mo><mn>1.87</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>17</mn></mrow></msup><mtext> </mtext><mtext> </mtext><msup><mrow><mi>GeV</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></math> over 5–30 MHz as an extended goal. In this work, we present the electromagnetic modeling of the response of the experiment to an axion signal over the full frequency range of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mtext>DMRadio-</mtext><msup><mrow><mi mathvariant="normal">m</mi></mrow><mrow><mn>3</mn></mrow></msup></mrow></math>, which extends from the low-frequency, lumped-element limit to a regime where the axion Compton wavelength is only a factor of 2 larger than the detector size. With these results, we determine the live time and sensitivity of the experiment. The primary science goal of sensitivity to DFSZ axions across 30–200 MHz can be achieved with a <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mn>3</mn><mi>σ</mi></math> live scan time of 2.9 years.

United States

A. AlShirawi

V. Ankel

C. Bartram

J. Begin

C. Bell

J.N. Benabou

L. Brouwer

S. Chaudhuri

H.M. Cho

J. Corbin

W. Craddock

S. Cuadra

A. Droster

J. Echevers

J.W. Foster

J.T. Fry

P.W. Graham

R. Henning

K.D. Irwin

F. Kadribasic

Y. Kahn

A. Keller

R. Kolevatov

S. Kuenstner

A. Kunder

N. Kurita

A.F. Leder

D. Li

N. Otto

J.L. Ouellet

K.M.W. Pappas

A. Phipps

N.M. Rapidis

B.R. Safdi

C.P. Salemi

M. Simanovskaia

J. Singh

P. Stark

E.C. van Assendelft

K. van Bibber

K. Wells

J. Wiedemann

L. Winslow

W.J. Wisniewski

D. Wright

A.K. Yi

B.A. Young

Electromagnetic modeling and science reach of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mtext>DMRadio-</mtext><msup><mrow><mi mathvariant="normal">m</mi></mrow><mrow><mn>3</mn></mrow></msup></mrow></math>

Combining toric geometry techniques and $$\mathcal {N}=2$$ supergravity formalisms, we study 5D black branes in the M-theory compactification on a four parameter Calabi–Yau threefold. First, we investigate 5D BPS and non-BPS black holes that are derived by wrapping M2-branes on non-holomorphic 2-cycles in such a toric Calabi–Yau manifold. Concretely, we provide the allowed electric charge regions of BPS and non-BPS black hole states that are obtained by surrounding M2-branes over appropriate 2-cycles. Then, we approach the black hole thermodynamic behavior by computing the entropy and the temperature. By evaluating the recombination factor, we examine the stability of such non-BPS black holes. Precisely, we find stable and unstable solutions depending on the allowed electric charge regions. After that, we study 5D black strings by wrapping M5-branes on non-holomorphic dual 4-cycles in the proposed toric Calabi–Yau manifold by focusing on the stability behaviors. In the allowed regions of the moduli space of the non-BPS stringy solutions, we find stable and unstable states depending on the magnetic charge values.

Morocco

A. Belhaj

H. Belmahi

A. Bouhouch

S. Ennadifi

M. Sedra

Black holes and black strings in M-theory on Calabi–Yau threefolds with four Kähler parameters

This Letter presents an investigation of low-energy electron-neutrino interactions in the Fermilab Booster Neutrino Beam by the MicroBooNE experiment, motivated by the excess of electron-neutrino-like events observed by the MiniBooNE experiment. This is the first measurement to use data from all five years of operation of the MicroBooNE experiment, corresponding to an exposure of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mn>1.11</mn><mo>×</mo><msup><mn>10</mn><mn>21</mn></msup></math> protons on target, a 70% increase on past results. Two samples of electron neutrino interactions without visible pions are used, one with visible protons and one without any visible protons. The MicroBooNE data show reasonable agreement with the nominal prediction, with <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>p</mi></math> values <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mo>≥</mo><mn>26.7</mn><mo>%</mo></math> when the two <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>ν</mi><mi>e</mi></msub></math> samples are combined, though the prediction exceeds the data in limited regions of phase space. The data are further compared to two empirical models that modify the predicted rate of electron-neutrino interactions in different variables in the simulation to match the unfolded MiniBooNE low energy excess. In the first model, this unfolding is performed as a function of electron neutrino energy, while the second model aims to match the observed shower energy and angle distributions of the MiniBooNE excess. This measurement excludes an electronlike interpretation of the MiniBooNE excess based on these models at <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mo>&gt;</mo><mn>99</mn><mo>%</mo><mtext> </mtext><mtext> </mtext><msub><mrow><mi>CL</mi></mrow><mrow><mi mathvariant="normal">s</mi></mrow></msub></mrow></math> in all kinematic variables.

P. Abratenko

D. Andrade Aldana

United Kingdom

L. Arellano

J. Asaadi

Israel

A. Ashkenazi

S. Balasubramanian

B. Baller

A. Barnard

G. Barr

D. Barrow

J. Barrow

V. Basque

J. Bateman

O. Benevides Rodrigues

S. Berkman

A. Bhat

M. Bhattacharya

M. Bishai

A. Blake

B. Bogart

T. Bolton

M.B. Brunetti

L. Camilleri

D. Caratelli

F. Cavanna

G. Cerati

A. Chappell

Y. Chen

J.M. Conrad

M. Convery

L. Cooper-Troendle

Spain

J.I. Crespo-Anadón

R. Cross

M. Del Tutto

S.R. Dennis

P. Detje

Switzerland

R. Diurba

Z. Djurcic

K. Duffy

S. Dytman

B. Eberly

P. Englezos

A. Ereditato

J.J. Evans

C. Fang

W. Foreman

B.T. Fleming

D. Franco

A.P. Furmanski

F. Gao

D. Garcia-Gamez

S. Gardiner

G. Ge

S. Gollapinni

E. Gramellini

P. Green

H. Greenlee

L. Gu

W. Gu

R. Guenette

P. Guzowski

L. Hagaman

M.D. Handley

O. Hen

C. Hilgenberg

G.A. Horton-Smith

A. Hussain

B. Irwin

M.S. Ismail

C. James

China

X. Ji

J.H. Jo

R.A. Johnson

Y.J. Jwa

D. Kalra

G. Karagiorgi

W. Ketchum

M. Kirby

T. Kobilarcik

N. Lane

J.Y. Li

Y. Li

K. Lin

B.R. Littlejohn

L. Liu

W.C. Louis

X. Luo

T. Mahmud

C. Mariani

D. Marsden

J. Marshall

N. Martinez

D.A. Martinez Caicedo

S. Martynenko

A. Mastbaum

I. Mawby

N. McConkey

L. Mellet

J. Mendez

J. Micallef

Search for an Anomalous Production of Charged-Current <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>ν</mi><mi>e</mi></msub></math> Interactions without Visible Pions across Multiple Kinematic Observables in MicroBooNE

We report on a search for sub-GeV dark matter (DM) particles interacting with electrons using the DAMIC-M prototype detector at the Modane Underground Laboratory. The data feature a significantly lower detector single <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msup><mrow><mi>e</mi></mrow><mrow><mo>−</mo></mrow></msup></mrow></math> rate (factor 50) compared to our previous search, while also accumulating a 10 times larger exposure of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mo>∼</mo><mn>1.3</mn><mtext> </mtext><mtext> </mtext><mi>kg</mi><mtext>−</mtext><mi>day</mi></mrow></math>. DM interactions in the skipper charge-coupled devices (CCDs) are searched for as groups of two or three adjacent pixels with a total charge between 2 and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mn>4</mn><mtext> </mtext><mtext> </mtext><msup><mi>e</mi><mo>−</mo></msup></math>. We find 144 candidates of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>2</mn><mtext> </mtext><mtext> </mtext><msup><mrow><mi>e</mi></mrow><mrow><mo>−</mo></mrow></msup></mrow></math> and 1 candidate of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>4</mn><mtext> </mtext><mtext> </mtext><msup><mrow><mi>e</mi></mrow><mrow><mo>−</mo></mrow></msup></mrow></math>, where 141.5 and 0.071, respectively, are expected from background. With no evidence of a DM signal, we place stringent constraints on DM particles with masses between 1 and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>1000</mn><mtext> </mtext><mtext> </mtext><mi>MeV</mi><mo>/</mo><msup><mrow><mi>c</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></math> interacting with electrons through an ultralight or heavy mediator. For large ranges of DM masses below <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>1</mn><mtext> </mtext><mi>GeV</mi><mo>/</mo><msup><mrow><mi>c</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></math>, we exclude theoretically motivated benchmark scenarios where hidden-sector particles are produced as a major component of DM in the Universe through the freeze-in or freeze-out mechanisms.