The standing wave model of the mesons and baryons

Only photons are needed to explain the masses of the pi(0), eta, Lambda, Sigma(0), Xi(0), Omega(-), Lambda(c,+), Sigma(c,0), Xi(c,0), and Omega(c,0) mesons and baryons. Only neutrinos are needed to explain the mass of the pi(+-) mesons. Neutrinos and photons are needed to explain the masses of the K-mesons, the neutron and D-mesons. Surprisingly the mass of the mu-meson can also be explained by the oscillation energies and rest masses of a neutrino lattice. From the difference of the masses of the pi(+-) mesons and mu(+-) mesons follows that the rest mass of the muon-neutrino is 47.5 milli-eV. From the difference of the masses of the neutron and proton follows that the rest mass of the electron-neutrino is 0.55 milli-eV. The potential of the weak force that holds the lattices of the particles together can be determined with Born's lattice theory. From the weak force follows automatically the existence of a strong force between the sides of two lattices. The strong nuclear force is the sum of the unsaturated weak forces at the sides of each lattice and is therefore 10^6 times stronger than the weak force.Comment: 41 pages, 6 figure

Interaction Between Convection and Pulsation

This article reviews our current understanding of modelling convection dynamics in stars. Several semi-analytical time-dependent convection models have been proposed for pulsating one-dimensional stellar structures with different formulations for how the convective turbulent velocity field couples with the global stellar oscillations. In this review we put emphasis on two, widely used, time-dependent convection formulations for estimating pulsation properties in one-dimensional stellar models. Applications to pulsating stars are presented with results for oscillation properties, such as the effects of convection dynamics on the oscillation frequencies, or the stability of pulsation modes, in classical pulsators and in stars supporting solar-type oscillations.Comment: Invited review article for Living Reviews in Solar Physics. 88 pages, 14 figure

CEBPA-mutated leukemia is sensitive to genetic and pharmacological targeting of the MLL1 complex

The gene encoding the transcription factor C/EBP alpha is mutated in 10-15% of acute myeloid leukemia (AML) patients. N-terminal CEBPA mutations cause ablation of full-length C/EBP alpha without affecting the expression of a shorter oncogenic isoform, termed p30. The mechanistic basis of p30-induced leukemogenesis is incompletely understood. Here, we demonstrate that the MLL1 histone-methyltransferase complex represents a critical actionable vulnerability in CEBPA-mutated AML. Oncogenic C/EBP alpha p30 and MLL1 show global co-localization on chromatin and p30 exhibits robust physical interaction with the MLL1 complex. CRISPR/Cas9-mediated mutagenesis of MLL1 results in proliferation arrest and myeloid differentiation in C/EBP alpha p30-expressing cells. In line, CEBPA-mutated hematopoietic progenitor cells are hypersensitive to pharmacological targeting of the MLL1 complex. Inhibitor treatment impairs proliferation and restores myeloid differentiation potential in mouse and human AML cells with CEBPA mutations. Finally, we identify the transcription factor GATA2 as a direct critical target of the p30-MLL1 interaction. Altogether, we show that C/EBP alpha p30 requires the MLL1 complex to regulate oncogenic gene expression and that CEBPA-mutated AML is hypersensitive to perturbation of the MLL1 complex. These findings identify the MLL1 complex as a potential therapeutic target in AML with CEBPA mutations

Experimental dynamics in magnetic field-driven flows compared to thermoconvective convection

We compare the dynamics obtained in two intermediate aspect ratio (diameter over height) experiments. These systems have rotational symmetry and consist of fluid layers that are destabilized using two different methods. The first one is a classical Bénard–Marangoni experiment, where the destabilizing forces, buoyancy and surface tension, are created by temperature gradients. The second system consists of a large drop of liquid metal destabilized using oscillating magnetic fields. In this configuration, the instability is generated by a radial Lorentz force acting on the conducting fluid. Although there are many important differences between the two configurations, the dynamics are quite similar: the patterns break the rotational symmetry, and different azimuthal and radial wavenumbers appear depending on the experimental control parameters. These patterns in most cases are stationary, but for some parameters they exhibit different dynamical behaviours: rotations, transitions between different solutions or cyclic connections between different patterns