Thu·Mar 7, 2024Thursday·March 7, 2024

1. 01*

   Quark Counting, Drell-Yan West, and the Pion Wave Function

   Mary Alberg🇺🇸 · Gerald A. Miller🇺🇸

   The relation between the pion's quark distribution function, $q(x)$, its light-front wave function, and the elastic charge form factor, $F({\Delta }^2)$ is explored. The square of the leading-twist pion wave function at a special probe scale, ${\zeta }_H$, is determined using models and Poincare covariance from realistic results for $q(x)$. This wave function is then used to compute form factors with the result that the Drell-Yan-West and quark counting relationships are not satisfied. A new relationship between $q(x)$ and $F({\Delta }^2)$ is proposed.

   hep-phnucl-exnucl-thPRC(2024)·5 citations
2. 02*

   Mass and decay width of $T_{ccs}$ from symmetries

   Mitsuru Tanaka🇯🇵 · Yasuhiro Yamaguchi🇯🇵 · Masayasu Harada🇯🇵

   We analyze the mass and width of the doubly heavy tetraquark $T_{ccs}$ composed of a heavy diquark and a light-quark cloud with strangeness with assuming that a color antitriplet heavy diquark is a dominant component of the doubly charmed tetraquarks $T_{cc}$ and $T_{ccs}$. We construct an effective Lagrangian for masses of heavy hadrons based on the superflavor symmetry between the doubly heavy tetraquarks and the singly heavy baryons by including the terms that simultaneously break the heavy-quark and light-flavor symmetries, and predict the mass of $T_{ccs}$ as $M(T_{ccs})=4047\pm 11$\,MeV. The comparison of this prediction with future experimental observation will give a clue to understand the color structure of the heavy diquark. We also predict the mass of ${\Omega }_{cc}$ as $M({\Omega }_{cc})=3706_{-15}^{+14}$MeV. We next calculate the decay width of $T_{ccs}$, based on solely the light-flavor symmetry, as $\Gamma (T_{ccs})=42\pm 24$\,MeV.

   hep-phnucl-thPRD(2024)·8 citations
3. 03*

   How higher charmonia shape the puzzling data of the $e^{+}{e}^{-}\to \eta J/\psi$ cross section

   Tian-Cai Peng🇨🇳 · Zi-Yue Bai🇨🇳 · Jun-Zhang Wang🇨🇳 · Xiang Liu🇨🇳

   Recently, the BESIII collaboration performed a precise measurement of the $e^{+}{e}^{-}\to \eta J/\psi$ cross section. It is puzzling that the resonance parameters of the reported $Y(4230)$ show a substantial divergence from the previously measured results in both the open-charmed and hidden-charmed decay channels, and the line shape asymmetry of the data approaching 4.2 GeV also suggests that it might be difficult to characterize the details of the structure around 4.2 GeV by a single resonance. This has motivated our great curiosity about how the charmonium states are distributed in the measured energy range and how they shape the puzzling data of the $e^{+}{e}^{-}\to \eta J/\psi$ cross section. In this work, we use five theoretically constructed charmonia in the range of $4.0-4.5$ $\text{GeV}$, i.e., $\psi (4040)$, $\psi (4160)$, $\psi (4220)$, $\psi (4380)$, and $\psi (4415)$, to apply a combined fit to the data, in which their calculated decay ratios into $\eta J/\psi$ via hadronic loop mechanism are taken as input. The fit results can reproduce the measured cross section data well, especially for the subtle line shape around 4.2 GeV, showing that the structure around 4.2 GeV is possible from the contribution of both $\psi (4160)$ and $\psi (4220)$.

   hep-phhep-exPRD(2024)·13 citations
4. 04*

   Impact of theoretical uncertainties on model parameter reconstruction from GW signals sourced by cosmological phase transitions

   Marek Lewicki🇵🇱 · Marco Merchand🇸🇪 · Laura Sagunski🇩🇪 · Philipp Schicho🇩🇪 · Daniel Schmitt🇩🇪

   Different computational techniques for cosmological phase transition parameters can impact the Gravitational Wave (GW) spectra predicted in a given particle physics model. To scrutinize the importance of this effect, we perform large-scale parameter scans of the dynamical real-singlet extended Standard Model using three perturbative approximations for the effective potential: the $\overline{\mathrm{MS}}$ and on-shell schemes at leading order, and three-dimensional thermal effective theory (3D EFT) at next-to-leading order. While predictions of GW amplitudes are typically unreliable in the absence of higher-order corrections, we show that the reconstructed model parameter spaces are robust up to a few percent in uncertainty. While 3D EFT is accurate from one loop order, theoretical uncertainties of reconstructed model parameters, using four-dimensional standard techniques, remain dominant over the experimental ones even for signals merely strong enough to claim a detection by LISA.

   hep-phastro-ph.COPRD(2024)·54 citations
5. 05*

   An assessment of $\mathbf{{\rm Y}}$-states above $\mathbf{B}\bar{\mathbf{B}}$-threshold using a constituent-quark-model based meson-meson coupled-channels framework

   P. G. Ortega🇪🇸 · D. R. Entem🇪🇸 · F. Fernández🇪🇸 · J. Segovia🇪🇸

   The ${\rm Y}(10753)$ state has been recently observed by the Belle and Belle~II collaborations with enough global significance to motivate an assessment of the high-energy spectrum usually predicted by any reasonable \emph{naïve} quark model. In the framework of a constituent quark model which satisfactorily describes a wide range of properties of conventional hadrons containing heavy quarks, the quark-antiquark and meson-meson degrees of freedom have been incorporated with the goal of elucidating the influence of open-bottom meson-meson thresholds into the ${\rm Y}$ states whose masses are within the energy range of the ${\rm Y}(10753)$'s mass. It is well known that such effects could be relevant enough as to generate dynamically new states and thus provide a plausible explanation of the nature of the ${\rm Y}(10753)$ state. In particular, we have performed a coupled-channels calculation in which the bare states ${\rm Y}(4S)$, ${\rm Y}(3D)$, ${\rm Y}(5S)$ and ${\rm Y}(4D)$ are considered together with the threshold channels $B\bar{B}$, $B{\bar{B}}^{\ast }$, $B^{\ast }{\bar{B}}^{\ast }$, $B_s{\bar{B}}_s$, $B_s{\bar{B}}_s^{\ast }$ and $B_s^{\ast }{\bar{B}}_s^{\ast }$. Among the results we have described, the following conclusions are of particular interest: (i) a richer complex spectrum is gained when thresholds are present and bare bound states are sufficiently non-relativistic; (ii) those poles obtained in the complex energy plane do not have to appear as simple peaks in the relevant cross sections; and (iii) the ${\rm Y}(10750)$ candidate is interpreted as a dressed hadronic resonance whose structure is an equally mixture of a conventional $b\bar{b}$ state and $B^{\ast }{\bar{B}}^{\ast }$ molecule.

   hep-phhep-exhep-latnucl-ex+1PRD(2024)·4 citations
6. 06*

   Complete NLO corrections to top-quark pair production with isolated photons

   Daniel Stremmer🇩🇪 · Malgorzata Worek🇩🇪

   We compute for the first time the so-called complete NLO corrections to top-quark pair production with one and two isolated photons in the di-lepton top-quark decay channel. The Narrow Width Approximation is used for the modeling of unstable top quarks and $W$ bosons. Higher-order QCD and EW effects as well as photon bremsstrahlung are consistently included at all stages: in production and top-quark decays. We present results at the integrated and differential fiducial cross-section level for both processes for the LHC Run II center-of-mass energy of $\sqrt{s}=13$ TeV. In addition, we investigate the scale choice in photonic observables. Finally, the individual size of each subleading contribution is discussed in detail and the origin of the main subleading corrections is scrutinised. For the latter case, alternative calculations are performed in which the subleading NLO corrections are included only in the production of $t\bar{t}\gamma$ and $t\bar{t}\gamma \gamma$.

   hep-phhep-exJHEP(2024)·17 citations
7. 07*

   On the cosmology and terrestrial signals of sexaquark dark matter

   Marianne Moore🇺🇸 · Tracy R. Slatyer🇺🇸

   We investigate the hypothesis that sexaquarks, hypothetical stable six-quark states, could be a significant component of the dark matter. We expand on previous studies of sexaquark cosmology, accounting for the possibility that some relevant interaction cross sections might be strongly suppressed below expectations based on dimensional analysis. We update direct-detection constraints on stable sexaquarks comprising a subdominant fraction of the dark matter, as well as limits on the annihilation of an antisexaquark component from Super-Kamiokande. We argue that the scenario where sexaquarks comprise a $O(1)$ fraction of the dark matter would require either a suppression of $O(10^{-19})$ in sexaquark interactions with baryons, combined with a very high yield of net sexaquark number from the quark-hadron transition, or else a very strong suppression of the cross section for antisexaquark annihilation on nucleons (24+ orders of magnitude below the QCD scale). Independently, we find that a sexaquark component comprising more than $O(10^{-3})$ of the dark matter can be excluded from direct-detection bounds, unless its scattering cross section is severely suppressed compared to the expected scale of strong and even electromagnetic interactions.

   hep-phastro-ph.COhep-exPRD(2024)·12 citations
8. 08*

   NNLO QCD corrections to the $q^2$ spectrum of inclusive semileptonic $B$-meson decays

   Matteo Fael🇨🇭 · Florian Herren🇨🇭

   We calculate the next-to-next-to-leading order QCD corrections to the leptonic invariant mass ($q^2$) spectrum of semileptonic $b\to c$ inclusive decays, taking into account the mass of the charm quark and the charged lepton in the final state. We obtain analytic results in terms of generalized polylogarithms and present numerical studies of the $\mathcal{O}({\alpha }_s^2)$ corrections to the $q^2$ spectrum of $b\to c\ell {\bar{\nu }}_{\ell }$ decays, for $\ell =e,\mu$ and $\tau$, in the kinetic scheme. Our computation can be used to incorporate the recent measurements of $q^2$ moments by Belle and Belle II into global fits of inclusive semileptonic $B$-decays.

   hep-phhep-exJHEP(2024)·16 citations
9. 09*

   Know your footprint -- Evaluation of the professional carbon footprint for individual researchers in high energy physics and related fields

   Valerie S. Lang🇩🇪 · Naman Kumar Bhalla · Simran Sunil Gurdasani · Pardis Niknejadi

   As the climate crisis intensifies, understanding the environmental impact of professional activities is paramount, especially in sectors with historically significant resource utilisation. This includes High Energy Physics (HEP) and related fields, which investigate the fundamental laws of our universe. As members of the young High Energy Physicists (yHEP) association, we investigate the CO${}_2$-equivalent emissions generated by HEP-related research on a personalised per-researcher level, for four distinct categories: Experiments, tied to collaborations with substantial infrastructure; Institutional, representing the resource consumption of research institutes and universities; Computing, focussing on simulations and data analysis; and Travel, covering professional trips to conferences, etc. The findings are integrated into a tool for self-evaluation, the Know-your-footprint (Kyf) calculator, allowing the assessment of the personal and professional footprint and optionally sharing the data with the yHEP association. The study aims to heighten awareness, foster sustainability, and inspire the community to adopt more environmentally responsible research practices urgently.

   ↳ physics.soc-phhep-exhep-phhep-thnpj Clim. Action 4, 28 (2025)·9 citations
10. 10*

    Correlated scalar perturbations and gravitational waves from axion inflation

    Sofia P. Corbà🇺🇸 · Lorenzo Sorbo🇺🇸

    The scalar and tensor fluctuations generated during inflation can be correlated, if arising from the same underlying mechanism. In this paper we investigate such correlation in the model of axion inflation, where the rolling inflaton produces quanta of a $U(1)$ gauge field which, in turn, source scalar and tensor fluctuations. We compute the primordial correlator of the curvature perturbation, $\zeta$, with the gravitational energy density, ${\Omega }_{GW}$, at frequencies probed by gravitational wave detectors. This two-point function receives two contributions: one arising from the correlation of gravitational waves with the scalar perturbations generated by the standard mechanism of amplification of vacuum fluctuations, and the other coming from the correlation of gravitational waves with the scalar perturbations sourced by the gauge field. Our analysis shows that the former effect is generally dominant. For typical values of the parameters, the correlator, normalized by the amplitude of $\zeta$ and by the fractional energy in gravitational waves at interferometer frequencies, turns out to be of the order of $10^{-4}÷10^{-2}$.

    ↳ astro-ph.COhep-phhep-thJCAP(2024)·19 citations
11. 11*

    Universality of pseudo-Goldstone damping near critical points

    Yang-yang Tan🇨🇳 · Yong-rui Chen🇨🇳 · Wei-jie Fu🇨🇳 · Wei-Jia Li🇨🇳

    Real-time dynamics of strongly correlated systems, in particular its critical dynamics near phase transitions, have been always on the cutting edge of studies in diverse fields of physics, e.g., high energy physics, condensed matter, holography, etc. In this work, we investigate the critical damping of collective modes associated with spontaneous breaking of approximate symmetries, which are called pseudo-Goldstone modes, in strongly correlated systems. Using the Schwinger-Keldysh field theory, we find a universal pseudo-Goldstone damping via the critical O($N$) model that has never been found before by other approaches. Different from the conventional damping found in holography and hydrodynamics, the new one is controlled by critical fluctuations, hence is invisible in mean-field systems or strongly correlated systems with classical gravity duals. Since the critical damping depends solely on the universalities of the critical point, irrespective of the microscopic details, our conclusion should be applicable to a wide class of interacting systems.

    ↳ hep-thcond-mat.stat-mechhep-phNature Commun.(2025)·9 citations
12. 12*

    Controlling volume fluctuations for studies of critical phenomena in nuclear collisions

    Romain Holzmann🇩🇪 · Volker Koch🇺🇸 · Anar Rustamov🇩🇪 · Joachim Stroth🇩🇪

    We generalize and extend the recently proposed method to account for contributions of system size (or volume/participant) fluctuations to the experimentally measured moments of particle multiplicity distributions. We find that in the general case there are additional biases which are not directly accessible to experiment. These biases are, however, parametrically suppressed if the multiplicity of the particles of interest is small compared to the total charged-particle multiplicity, e.g., in the case of proton number fluctuations at top RHIC and LHC energies. They are also small if the multiplicity distribution of charged particles per wounded nucleon is close to the Poissonian limit, which is the case at low energy nuclear collisions, e.g., at GSI/SIS18. We further find that mixed events are not necessarily needed to extract the correction for volume fluctuations, albeit it can help if event statistics is small, which is typically the case for reconstructing the higher-order cumulants. We provide the formulas to correct pure and mixed cumulants of particle multiplicity distributions up to any order together with their associated biases.

    ↳ nucl-thhep-exhep-phnucl-exNPA(2024)·16 citations
13. 13*

    Gravitational waves from first-order phase transitions in LISA: reconstruction pipeline and physics interpretation

    Chiara Caprini🇨🇭 · Ryusuke Jinno🇯🇵 · Marek Lewicki🇵🇱 · Eric Madge🇮🇱 · Marco Merchand🇸🇪 · Germano Nardini🇳🇴 · Mauro Pieroni🇨🇭 · Alberto Roper Pol🇨🇭 · Ville Vaskonen (for the LISA Cosmology Working Group)🇪🇪

    We develop a tool for the analysis of stochastic gravitational wave backgrounds from cosmological first-order phase transitions with LISA: we initiate a template databank for these signals, prototype their searches, and forecast their reconstruction. The templates encompass the gravitational wave signals sourced by bubble collisions, sound waves and turbulence. Accounting for Galactic and extra-Galactic foregrounds, we forecast the region of the parameter space that LISA will reconstruct with better than $\sim 10\%$ accuracy, if certain experimental and theoretical uncertainties are solved by the time LISA flies. We illustrate the accuracy with which LISA can reconstruct the parameters on a few benchmark signals, both in terms of the template parameters and the phase transition ones. To show the impact of the forecasts on physics beyond the Standard Model, we map the reconstructed benchmark measurements into the parameter spaces of the singlet extension of the Standard Model and of the classically conformal invariant $U(1{)}_{B-L}$ model.

    ↳ astro-ph.COhep-phJCAP(2024)·151 citations
14. 14*

    Multimessenger signals from compact axion star mergers

    Liina Chung-Jukko🇬🇧 · Eugene A. Lim🇬🇧 · David J. E. Marsh🇬🇧

    Axion dark matter can form stable, self-gravitating, and coherent configurations known as axion stars, which are rendered unstable above a critical mass by the Chern-Simons coupling to electromagnetism. We study, using numerical relativity, the merger and subsequent decay of compact axion stars. We show that two sub-critical stars can merge, and form a more massive, excited and critical star, which survives for a finite period before rapidly decaying via electromagnetic radiation. We find a rich multimessenger signal, composed of gravitational waves, electromagnetic radiation, and axion radiation. The gravitational wave signal is broken into two parts: a weak and broad signal from the merger, followed by a much stronger signal of almost fixed frequency from the decay. The electromagnetic radiation follows only the gravitational waves from the decay, while the axion signal is continuous throughout the process. We briefly discuss the detectability of such a signal.

    ↳ astro-ph.COgr-qchep-phPRD(2024)·10 citations
15. 15*

    Superfluid dark stars

    Lorenzo Cipriani🇮🇹 · Massimo Mannarelli🇮🇹 · Fabrizio Nesti🇮🇹 · Silvia Trabucco🇮🇹

    We present a superfluid dark star model consisting of relativistic dark bosons with two-body self-interaction. The obtained masses, radii, and tidal deformability depend in a simple way on the boson mass and interaction strength. We report first results on binary mergers: the distinctive amplitude and frequency of the emitted gravitational waves are well within reach of terrestrial interferometers.

    ↳ astro-ph.COgr-qchep-phPRD(2024)·7 citations
16. 16*

    How open is the asteroid-mass primordial black hole window?

    Matthew Gorton🇬🇧 · Anne M. Green🇬🇧

    Primordial black holes (PBHs) can make up all of the dark matter (DM) if their mass, $m$, is in the so-called 'asteroid-mass window', $10^{17}\mathrm{g}\lesssim m\lesssim 10^{22}\mathrm{g}$. Observational constraints on the abundance of PBHs are usually calculated assuming they all have the same mass, however this is unlikely to be a good approximation. PBHs formed from the collapse of large density perturbations during radiation domination are expected to have an extended mass function (MF), due to the effects of critical collapse. The PBH MF is often assumed to be lognormal, however it has recently been shown that other functions are a better fit to numerically calculated MFs. We recalculate both current and potential future constraints for these improved fitting functions. We find that for current constraints the asteroid-mass window narrows, but remains open (i.e. all of the DM can be in the form of PBHs) unless the PBH MF is wider than expected. Future evaporation and microlensing constraints may together exclude all of the DM being in PBHs, depending on the width of the PBH MF and also the shape of its low and high mass tails.

    ↳ astro-ph.COhep-phSciPost Phys.(2024)·39 citations
17. 17*

    Pre-supernova evolution and final fate of stellar mergers and accretors of binary mass transfer

    F.R.N. Schneider🇦🇹 · Ph. Podsiadlowski · E. Laplace🇩🇪

    The majority of massive stars are expected to exchange mass or merge with a companion during their lives. This immediately implies that most supernovae (SNe) are from such post-mass-exchange objects. Here, we explore how mass accretion and merging affect the pre-SN structures of stars and their final fates. We use the stellar evolution code MESA, infer the outcome of core-collapse using a neutrino-driven SN model, and apply a rapid-accretion model. Our models cover initial masses from 11 to 70 Msun and the accreted mass ranges from 10-200% of the initial mass. We find that mass accretion in particular onto post-main-sequence (post-MS) stars can lead to a long-lived blue supergiant (BSG) phase. In comparison to genuine single stars, post-MS accretors have small core-to-total mass ratios, regardless of whether they end their lives as BSGs or cool supergiants (CSGs), and they can have genuinely different pre-SN core structures. As in single and binary-stripped stars, we find black-hole (BH) formation for the same characteristic CO core masses M_CO of ~7 Msun and >13 Msun. In models with the largest mass accretion, the BH-formation landscape as a function of M_CO is shifted by about 0.5 Msun to lower masses. We find a tight relation between our neutron-star (NS) masses and the central entropy of the pre-SN models, suggesting a universal relation that is independent of the evolutionary history of stars. Post-MS accretors explode both as BSGs and CSGs, and we show how to understand their pre-SN locations in the Hertzsprung--Russell diagram. Some BSGs that avoid the luminous-blue-variable (LBV) regime are predicted to collapse into BHs of up to 50 Msun while others explode in supernovae and eject up to 40 Msun, greatly exceeding ejecta masses from single stars. These masses can be even higher at lower metallicities, and they may fall into the pair-instability-supernova mass gap. [abridged]

    ↳ astro-ph.SRastro-ph.HEhep-phAstron.Astrophys.(2024)·54 citations
18. 18*

    Deep Generative Models for Ultra-High Granularity Particle Physics Detector Simulation: A Voyage From Emulation to Extrapolation

    Baran Hashemi🇩🇪

    Simulating ultra-high-granularity detector responses in Particle Physics represents a critical yet computationally demanding task. This thesis aims to overcome this challenge for the Pixel Vertex Detector (PXD) at the Belle II experiment, which features over 7.5M pixel channels-the highest spatial resolution detector simulation dataset ever analysed with generative models. This thesis starts off by a comprehensive and taxonomic review on generative models for simulating detector signatures. Then, it presents the Intra-Event Aware Generative Adversarial Network (IEA-GAN), a new geometry-aware generative model that introduces a relational attentive reasoning and Self-Supervised Learning to approximate an "event" in the detector. This study underscores the importance of intra-event correlation for downstream physics analyses. Building upon this, the work drifts towards a more generic approach and presents YonedaVAE, a Category Theory-inspired generative model that tackles the open problem of Out-of-Distribution (OOD) simulation. YonedaVAE introduces a learnable Yoneda embedding to capture the entirety of an event based on its sensor relationships, formulating a Category theoretical language for intra-event relational reasoning. This is complemented by introducing a Self-Supervised learnable prior for VAEs and an Adaptive Top-q sampling mechanism, enabling the model to sample point clouds with variable intra-category cardinality in a zero-shot manner. Variable Intra-event cardinality has not been approached before and is vital for simulating irregular detector geometries. Trained on an early experiment data, YonedaVAE can reach a reasonable OOD simulation precision of a later experiment with almost double luminosity. This study introduces, for the first time, the results of using deep generative models for ultra-high granularity detector simulation in Particle Physics.

    ↳ physics.ins-detcs.AIcs.LGhep-ex+110 citations

* Reconstructed cohort: no mailing for this day survives in the archive. Papers are grouped by their submission times and arXiv's announcement cut-off, assuming announcement without delay; positions follow identifier order. Validated at ~91% exact-day agreement against the archived era.