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  • Improved constraints on Higgs boson self-couplings with quartic and cubic power dependencies of the cross section
    2025, 49(2): 023107-023107-8. doi: 10.1088/1674-1137/ad9d1d
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    Precise determination of the Higgs boson self-couplings is essential for understanding the mechanism underlying electroweak symmetry breaking. However, owing to the limited number of Higgs boson pair events at the LHC, only loose constraints have been established to date. Current constraints are based on the assumption that the cross section is a quadratic function of the trilinear Higgs self-coupling within the $\kappa$ framework. Incorporating higher-order quantum corrections from virtual Higgs bosons would significantly alter this functional form, introducing new quartic and cubic power dependencies on the trilinear Higgs self-coupling. To derive this new functional form, we propose a specialized renormalization procedure that tracks all Higgs self-couplings at each calculation step. Additionally, we introduce renormalization constants for coupling modifiers within the $\kappa$ framework to ensure the cancellation of all ultraviolet divergences. With new functional forms of the cross sections in both the gluon-gluon fusion and vector boson fusion channels, the upper limit of $\kappa_{\lambda_{{\rm{3H}}}}=\lambda_{{\rm{3H}}}/\lambda_{{\rm{3H}}}^{{\rm{SM}}}$ set by the ATLAS (CMS) collaboration is reduced from 6.6 (6.49) to 5.4 (5.37). However, extracting a meaningful constraint on the quartic Higgs self-coupling $\lambda_{{\rm{4H}}}$ from Higgs boson pair production data remains challenging. We also present the invariant mass distributions of the Higgs boson pair at different values of the self-couplings, which could assist in setting optimal cuts for experimental analysis.
  • Impact of nonextensivity on the transport coefficients of strongly interacting QCD matter
    2025, 49(2): 023108-023108-17. doi: 10.1088/1674-1137/ad99b1
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    Tsallis nonextensive statistics is applied to study the transport coefficients of strongly interacting matter within the Polyakov chiral $S U(3) $ quark mean field model (PCQMF). Nonextensivity is introduced within the PCQMF model through a dimensionless parameter q to examine the viscous properties, such as shear viscosity (η) and bulk viscosity ($\zeta_b$), and conductive properties, such as electrical conductivity ($\sigma_{el}$) and thermal conductivity (κ). Additionally, some key thermodynamic quantities relevant to the transport coefficients, such as the speed of sound ($c_{sq}^2$) and specific heat at constant volume ($c_{vq}$), are calculated. The temperature dependence of the transport coefficients is explored through a kinetic theory approach with the relaxation time approximation. The results are compared to those of the extensive case where q approaches 1. The nonextensive q parameter is found to have a significant effect on all transport coefficients. We find that the nonextensive behaviour of the medium enhances specific shear viscosity $\eta/s_q$, as well as conductive coefficients $\sigma_{el}/{\rm T}$ and $\kappa/{\rm T}^2$. In contrast, the normalized bulk viscosity $\zeta_b/s_q$ is found to decrease as the nonextensivity of the medium increases. We also studied the transport coefficients for finite values of chemical potentials. The magnitudes of η, $\sigma_{el}$, and κ increase at lower temperatures, while ζb is found to decrease for systems with non-zero chemical potential.
  • Anisotropic quark stars in ${\boldsymbol {f(R,L_m,T)} }$ gravity
    2025, 49(2): 025110-025110-12. doi: 10.1088/1674-1137/ad99b2
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    We investigated the impact of $f(R,L_m,T)$ gravity on the internal structure of compact stars, expecting this theory to manifest prominently in the high-density cores of such stars. We considered the algebraic function $f(R,L_m,T) = R + \alpha T L_m$, where α represents the matter-geometry coupling constant. We specifically chose the matter Lagrangian density $L_m= -\rho$ to explore compact stars with anisotropic pressure. To this end, we employed the MIT bag model as an equation of state. Subsequently, we numerically solved the hydrostatic equilibrium equations to obtain mass-radius relations for quark stars (QSs), examining static stability criteria, adiabatic index, and speed of sound. Finally, we used recent astrophysical data to constrain the coupling parameter α, which may lead to either larger or smaller masses for QSs, compared to their counterparts in general relativity.
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