Understanding the properties of atomic nuclei and their connection to astrophysical phenomena requires reliable theoretical models together with increasingly precise experimental constraints. In this seminar, I will present some of my recent work spanning nuclear structure, nuclear astrophysics, and data-driven nuclear modelling. I will first discuss the electric dipole response of finite nuclei and how dipole polarizability can provide constraints on the density dependence of the nuclear symmetry energy and on neutron-star properties. I will then address low-energy electric dipole strength in neutron-rich nuclei and its impact on astrophysical neutron-capture and photodisintegration reaction rates, with particular emphasis on the role of strength near the particle-emission threshold. Finally, I will present recent applications of machine-learning and quantum-machine-learning methods to nuclear mass predictions, including ensemble-based approaches and physics-informed feature representations. These studies illustrate complementary ways in which nuclear observables, microscopic models, and modern computational methods can be combined to improve the predictive description of nuclei across the nuclear chart.

50 years ago I defended my PhD Thesis entitled ”Un modelo nuclear de capas globalmenteautoconsistente”. In this work a very simple mean field potential was built up based on a density-dependent effective force within the Hartree approximation. The parameters of the interactions were fitted to nuclear matter and finite nuclei data. In spite of the strong simplifications introduced, this very simple model was able to describe properties of magic nuclei in good agreement with the experiment and with a quality similar to that predicted by other more sophysticated mean field models available in the early seventies.

The second part of this talk is devoted to my most recent research about the behaviour of the Gogny force at finite temperature. Using specially the most recent versions of the Gogny interaction, namely D3G3M and D2, I revise different thermal properies of nuclear matter across varying temperatures, densities and isospin asymmetries. The liquid-gas phase transition and the instability regions in asymmetric nuclear matter are also discussed. The ability of these Gogny forces to nuclear astrophysics is also explored in teo particluar scenarios, merger matter and protoneutron stars.

How much energy does a quantum computer consume? Are they more efficient than their classical counterparts? In this work, we make a step towards answering these questions. We define the energy efficiency of a quantum computer as the ratio of the number of algorithms it can perform during a given time over the energy consumed by the hardware during this time. We analyze the most representative physical platforms currently envisioned to be used as building blocks of quantum computers: superconducting qubits, silicon spin qubits, trapped ions, neutral atoms and photonic qubits. Including insights from experts in all these technologies and taking into account algorithm compilation constraints, we discuss the advantages and inconveniences of each platform from an energy standpoint. Beyond providing concrete values of the energy consumption of current quantum computers, we lay the foundation of a framework to benchmark the energy efficiency of any future quantum computing architecture.

The existence limit of nuclei and the origin of the heavy elements are fundamental problems in modern science. The relativistic density functional theory starts from a universal density functional and has achieved great successes in describing many nuclear phenomena. In this talk, the predictive power of PC-PK1 is demonstrated, physics around the neutron drip line and N=Z nuclei are discussed, the DRHBc mass table collaboration is introduced. The quasiparticle finite amplitude method based on DRHBc theory has been developed for the nuclear level density , gamma strength function, Neutron capture rates and beta-decay lifetimes. Relativistic density functional theory in 3D lattice and its time-dependent version for Linear-chain, Chiral dynamics, Fission, etc. are briefly mentioned.

The theoretical prediction of the muon anomalous magnetic moment aµ depends crucially on the Hadronic Vacuum Polarization (HVP), and the tension between its dispersive and lattice-QCD determinations remains unresolved. We show that part of this puzzle can be addressed in the heavy-quark sector, where both descriptions are theoretically clean, by recognizing that the heavy-quark mass and its contribution to aµ are not independent quantities: both follow from in-tegrals of the same hadronic spectral function, differing only in their integration kernel. Promoting this kernel to a free choice within the relativistic QCD Sum Rules used to determine heavy-quark masses, we break with the conventional notion of a single valid sum rule and instead determine the mass and its HVP contribution simultaneously, from a common, self-consistent framework. This intrinsic construction exploits the anticorrelation between the two quantities to sharpen the final uncertainty, and turns the residual disagreement between the perturbative and hadronic descriptions of the observable into a direct observable-specific diagnostic of residual theory/model dependence, including duality-violation and continuum-modeling effects, unavailable to a determination of the mass alone. We obtain a HVPc+b,LOµ = (14.46(13) + 0.3009(17)) ×10−10 at leading HVPc+b ,NLOa,b and aµ = (−0.5738(95)−0.01822(13))×10−10 at next-to-leading order, for charm and bottom contributions, respectively. We compare our next-to-leading-order results with its first available lattice determination, finding good agreement in the charm sector. As a byproduct, we obtain mc= 1267.1(6.8) MeV and mb = 4182.3(7.2) MeV, with unprecedented phenomenological precision. Beyond these results, the construction introduced here defines a general strategy, appli cable to any observable expressible as a kernel-weighted dispersive integral, for extracting correlated hadronic quantities from a single, unified sum rule.