<p>The solar steady emission in gamma rays is due to the interactions of Galactic cosmic rays with the solar atmosphere and with the low-energy solar photon field via inverse Compton scattering. The emission is sensitive to the magnetic field nearby the Sun and to the cosmic-ray transport in the magnetic field in the inner Solar System. Modeling the inverse Compton emission in the presence of a magnetic field is, therefore, crucial to better interpret the observations. In a previous work, we have presented a comprehensive calculation of the secondary productions due to the collision of cosmic rays with the solar atmosphere in the presence of magnetic fields. In this paper, we present a general approach to calculate the (anisotropic) inverse Compton scattering in a 3D Monte Carlo simulation, also in the presence of magnetic and electric fields. After a short review of the scattering process of photons with electrons, examples of inverse Compton emission are presented, including the predictions for the Sun.</p>

Italy

M.N. Mazziotta

3D Monte Carlo calculation of the inverse Compton emission from the Sun and stars in the presence of magnetic and electric fields

We present the first calculation of the connected scalar matrix element and the momentum fraction of the charm quark within the ${3}/{2}^{+}$ and ${3}/{2}^{-}$ triply charmed baryons on lattice QCD. The results are based on overlap valence fermions on two ensembles of $ N_f=2+1 $ domain wall fermion configurations with two lattice spacings. The corresponding sea quark pion masses are 300 MeV and 278 MeV. The separated contributions to the triply charmed baryon mass are derived through the decomposition of the QCD energy-momentum tensor. The contribution of the connected charm quark matrix element to the triply charmed baryon is about 3/2 times that of the charmonium, and it is almost 70% of the total mass. The mass splitting of ${3}/{2}^{+}$ and ${3}/{2}^{-}$ triply charmed baryons is mainly from the $ \langle H_{E}\rangle $ of the QCD energy-momentum tensor. A mass decomposition based on the quark model is also studied for comparison.

China

Jin-Bo Li

Long-Cheng Gui

Wen Qin

Wei Sun

Jian Liang

Triply charmed baryons mass decomposition from lattice QCD * Supported by the National Natural Science Foundation of China (12175036, 11935017, 12175073, 12205311, 12222503), the Natural Science Foundation of Hunan Province, China (2023JJ30380, 2024JJ6300), the Department of Education Foundation of Hunan Province, China (20A310, 22B0044), and the Major Project of Basic and Applied Basic Research of Guangdong Province, China (2020B0301030008)

The discovery of solar neutrinos confirmed that the inner workings of the Sun generally match our theoretical understanding of the fusion process. Solar neutrinos have also played a role in discovering that neutrinos have mass and that they oscillate. We combine the latest solar neutrino data along with other oscillation data from reactors to determine the Sun's density profile. We derive constraints given the current data and show the anticipated improvements with more reactor neutrino data from JUNO constraining the true oscillation parameters and more solar neutrino data from DUNE which should provide a crucial measurement of <italic>hep</italic> neutrinos.

United States

Peter B. Denton

Charles Gourley

Determining the density of the sun with neutrinos

In this study, we investigate the $R^2$ corrections to the dissociation of heavy quarkonium in the Gauss-Bonnet gravitational background. We analyze the impact of the Gauss-Bonnet parameter $\lambda_{\rm GB}$ on the spectral function of charmonium and bottomonium and examine the effect of $\lambda_{\rm GB}$ on the dissociation of heavy quarkonium. Our results show that $\lambda_{\rm GB}$ reduces the peak height and increases the peak width of the spectral function, suggesting that $\lambda_{\rm GB}$ enhances the dissociation of heavy quarkonium. We also discuss the variation in the dissociation of heavy quarkonium with the ratio of shear viscosity to entropy density and observe that the dissociation is easier in more perfect plasma. Additionally, we observe that the temperature decreases the peak height and widens the peak, thereby accelerating the dissociation.

Zhou-Run Zhu

Manman Sun

Rui Zhou

Jinzhong Han

$\textit{R}$ $^{2}$ corrections to holographic heavy quarkonium dissociation * Rui Zhou supported by the Science and Technology Development Plan Project of Henan Province, China (242102230085), the National Natural Science Foundation of China (12404470), the High Level Talents Research and Startup Foundation Projects for Doctors of Zhoukou Normal University, China (ZKNUC2023017). Manman Sun supported by the National Natural Science Foundation of China (12305076). Zhou-Run Zhu supported by the High Level Talents Research and Startup Foundation Projects for Doctors of Zhoukou Normal University, China (ZKNUC2023018)

<p>The Sun is not quite a perfect sphere, and its oblateness, thought to be induced through its rotation, has been measured using optical observations of its radius. Its gravitational quadrupole moment can then be deduced using solar models, or through helioseismology, and it can also be determined from measurements of its gravitational effects on Mercury’s orbit. The various assessments do not appear to agree, with the most complete and precise orbital assessments being in slight excess of other determinations. This may speak to the existence of a nonluminous disk or ring, where we also note evidence for a circumsolar dust ring within Mercury’s orbit from the Solar TErrestrial RElations Observatory (STEREO) mission. Historically, too, a protoplanetary disk may have been key to reconciling the Sun’s metallicity with its neutrino yield. The distribution of the nonluminous mass within Mercury’s orbit can modify the relative size of the optical and orbital quadrupole moments in different ways. We develop how we can use these findings to limit the mass of a dark disk, ring, or halo in the immediate vicinity of the Sun, and we note how future observational studies of the inner Solar System can not only refine these constraints but can also help to identify and to assess the mass of its dark-matter component.</p>

Brazil

Gustavo F.S. Alves

Susan Gardner

Pedro Machado

Mohammadreza Zakeri

Does the Sun have a dark disk?

We calculate the form factor   $M(q^2)$   for the Dalitz decay   $M(q^2)$   with   $M(q^2)$   being the SU(  $M(q^2)$  ) flavor singlet pseudoscalar meson. The difference among the partial widths   $M(q^2)$   at different   $M(q^2)$   can be attributed in part to the   $M(q^2)$   and quark mass dependences induced by the   $M(q^2)$   anomaly dominance.   $M(q^2)$   in both   $M(q^2)$   is well described by the single pole model   $M(q^2)$  . Combined with the known experimental results of the Dalitz decays   $M(q^2)$  , the pseudoscalar mass   $M(q^2)$   dependence of the pole parameter   $M(q^2)$   is approximated by   $M(q^2)$   with   $M(q^2)$   and   $M(q^2)$  . These results provide inputs for future theoretical and experimental studies on the Dalitz decays   $M(q^2)$  .

Chunjiang Shi

Ying Chen

Xiangyu Jiang

Ming Gong

Zhaofeng Liu

Form factor for Dalitz decays from / To Light Pseudoscalars  

Millicharged dark matter particles can be efficiently captured by the Sun, where they annihilate into tau leptons, leading to the production of high-energy neutrinos. In contrast to the Earth, the high temperature of the Sun suppresses the fraction of millicharged particles that are bound to nuclei, allowing for potentially high annihilation rates. We recast existing constraints from the IceCube Neutrino Observatory and use this information to place new limits on the fraction of the dark matter that is millicharged. This analysis excludes previously unexplored parameter space for masses of <math><mrow><msub><mrow><mi>m</mi></mrow><mrow><mi>χ</mi></mrow></msub><mo>∼</mo><mo>(</mo><mn>5</mn><mi>–</mi><mn>100</mn><mo>)</mo><mtext> </mtext><mtext> </mtext><mi>GeV</mi></mrow></math>, charges of <math><mrow><msub><mrow><mi>q</mi></mrow><mrow><mi>χ</mi></mrow></msub><mo>∼</mo><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>3</mn></mrow></msup><mi>–</mi><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>2</mn></mrow></msup></mrow></math>, and fractional abundances as small as <math><mrow><msub><mrow><mi>f</mi></mrow><mrow><mi>DM</mi></mrow></msub><mo>∼</mo><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>5</mn></mrow></msup></mrow></math>.

Asher Berlin

Dan Hooper

High-energy neutrinos from millicharged dark matter annihilation in the Sun

The exploration of the parameter space of axion and axion-like particle dark matter is a major aim of the future program of astroparticle physics investigations. In this context, we present a possible strategy that focuses on detecting radio emissions arising from the conversion of dark matter axions in the Sun's magnetic field, including conversion in sunspots. We demonstrate that near-future low-frequency radio telescopes, such as the SKA Low, may access regions of unexplored parameter space for masses <math><msub><mrow><mi>m</mi></mrow><mrow><mi>a</mi></mrow></msub><mo>≲</mo><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>6</mn></mrow></msup></math> eV.

Elisa Todarello

Marco Regis

Marco Taoso

Spain

Maurizio Giannotti

Jaime Ruz

Julia K. Vogel

The Sun as a target for axion dark matter detection

By extracting the transition amplitudes, we give the first lattice QCD prediction of the two-body decay partial widths of the <math><msup><mn>1</mn><mrow><mo>−</mo><mo>+</mo></mrow></msup></math> charmoniumlike hybrid <math><msub><mi>η</mi><mrow><mi>c</mi><mn>1</mn></mrow></msub></math>. Given the calculated mass value <math><msub><mi>m</mi><msub><mi>η</mi><mrow><mi>c</mi><mn>1</mn></mrow></msub></msub><mo>=</mo><mn>4.329</mn><mo>(</mo><mn>36</mn><mo>)</mo><mtext> </mtext><mtext> </mtext><mi>GeV</mi></math>, the <math><msub><mi>η</mi><mrow><mi>c</mi><mn>1</mn></mrow></msub></math> decay is dominated by the open charm modes <math><msub><mi>D</mi><mn>1</mn></msub><mover><mi>D</mi><mo>¯</mo></mover></math>, <math><msup><mi>D</mi><mo>*</mo></msup><mover><mrow><mi>D</mi><mo>,</mo></mrow><mo>¯</mo></mover></math> and <math><msup><mi>D</mi><mo>*</mo></msup><msup><mover><mi>D</mi><mo>¯</mo></mover><mo>*</mo></msup></math> with partial widths of 258(133), 88(18), and 150(118) MeV, respectively. The coupling of <math><msub><mi>η</mi><mrow><mi>c</mi><mn>1</mn></mrow></msub></math> to <math><msub><mi>χ</mi><mrow><mi>c</mi><mn>1</mn></mrow></msub></math> plus a flavor singlet pseudoscalar is not small, but <math><msub><mi>χ</mi><mrow><mi>c</mi><mn>1</mn></mrow></msub><mi>η</mi></math> decay is suppressed by the small <math><mi>η</mi><mo>−</mo><msup><mi>η</mi><mo>′</mo></msup></math> mixing angle. The partial width of <math><msub><mi>η</mi><mrow><mi>c</mi><mn>1</mn></mrow></msub><mo>→</mo><msub><mi>η</mi><mi>c</mi></msub><msup><mi>η</mi><mo>′</mo></msup></math> is estimated to be around 1 MeV. We suggest experiments to search for <math><msub><mi>η</mi><mrow><mi>c</mi><mn>1</mn></mrow></msub></math> in the <math><mi>P</mi></math>-wave <math><msup><mi>D</mi><mo>*</mo></msup><mover><mi>D</mi><mo>¯</mo></mover></math> and <math><msup><mi>D</mi><mo>*</mo></msup><msup><mover><mi>D</mi><mo>¯</mo></mover><mo>*</mo></msup></math> systems. Especially, the polarization of <math><msup><mi>D</mi><mo>*</mo></msup><msup><mover><mi>D</mi><mo>¯</mo></mover><mo>*</mo></msup></math> can be used to distinguish the <math><msup><mn>1</mn><mrow><mo>−</mo><mo>+</mo></mrow></msup></math> product (total spin <math><mi>S</mi><mo>=</mo><mn>1</mn></math>) from <math><msup><mn>1</mn><mrow><mo>−</mo><mo>−</mo></mrow></msup></math> products (<math><mi>S</mi><mo>=</mo><mn>0</mn></math>).

Decays of <math><msup><mn>1</mn><mrow><mo>−</mo><mo>+</mo></mrow></msup></math> charmoniumlike hybrid using lattice QCD

The Sun may capture asymmetric dark matter (DM), which can subsequently form bound-states through the radiative emission of a sub-GeV scalar. This process enables generation of scalars without requiring DM annihilation. In addition to DM capture on nucleons, the DM-scalar coupling responsible for bound-state formation also induces capture from self-scatterings of ambient DM particles with DM particles already captured, as well as with DM bound-states formed in-situ within the Sun. This scenario is studied in detail by solving Boltzmann equations numerically and analytically. In particular, we take into consideration that the DM self-capture rates require a treatment beyond the conventional Born approximation. We show that, thanks to DM scatterings on bound-states, the number of DM particles captured increases exponentially, leading to enhanced emission of relativistic scalars through bound-state formation, whose final decay products could be observable. We explore phenomenological signatures with the example that the scalar mediator decays to neutrinos. We find that the neutrino flux emitted can be comparable to atmospheric neutrino fluxes within the range of energies below one hundred MeV. Future facilities like Hyper-K, and direct DM detection experiments can further test such scenario.