Balancing Asymmetric Dark Matter with Baryon Asymmetry and Dilution of Frozen Dark Matter by Sphaleron Transition

In this paper, we study the effect of electroweak sphaleron transition and electroweak phase transition (EWPT) in balancing the baryon excess and the excess stable quarks of the 4th generation. Sphaleron transitions between baryons, leptons and the 4th family of leptons and quarks establish a definite relationship between the value and sign of the 4th family excess and baryon asymmetry. This relationship provides an excess of stable U¯ antiquarks, forming dark atoms—the bound state of (U¯U¯U¯) the anti-quark cluster and primordial helium nucleus. If EWPT is of the second order and the mass of U quark is about 3.5 TeV, then dark atoms can explain the observed dark matter density. In passing by, we show the small, yet negligible dilution in the pre-existing dark matter density, due to the sphaleron transition.

Advanced Direct Digital Synthesis Generator Design for Transuranic Nuclide Alpha Spectrometry Pulses

Alpha energy spectrum measurement has been employed in the nuclear waste disposal of transuranic nuclides (such as 239Pu and 241Am), supervision, and disposal process. The alpha spectrum is made up of alpha particles, which have a fast-moving helium nucleus and an energy of 4–8 MeV with weak penetration ability. Removing alpha particles from radioactive nuclides is an important scientific issue. In this study, a transuranic nuclide alpha particle pulse generator that produces simulated alpha particle pulses similar to real particles was designed. Field programmable gate array (FPGA) was adopted as its core chip and we obtained the digital pulse waveform using software tracing points while simulating real alpha particles by random numbers. Accordingly, the alpha energy spectrum of a radioactive source 241Am was obtained using a passivated ion-implanted planar silicon (PIPS) detector. Afterward, the alpha particle was extracted from the energy spectrum and was then compared to the alpha particle pulse of the two methods, deriving a result. Here, both groupings of particle pulse waveforms were found to be very similar, and the periodic error of the particle was observed to be less than 1%. Furthermore, the amplitude and time interval of the particle were apparently similar to the actual spectrometry pulse.

Two methods to create free energy

Today, the best way to get free energy is nuclear, through fission, and hopefully soon through fusion. The best way to get clean and friendly energy in a sustainable way remains the start of the nuclear fusion reaction at an industrial scale. Nuclear fusion is the combination of two light nuclei in a heavier nucleus. Fusion or thermonuclear reaction of light elements are typical reactions that occur in the Sun and other stars. Indeed, in the Sun, every second, 657 million tons of hydrogen are converted into 653 million tons of helium. The 4 million tonnes missing are then converted to radiation - this phenomenon assuring the sun's shine. A fusion reaction in which a relatively large amount of energy (27.7 MeV) is released is one in which four protons interact leading to the formation of a helium nucleus (an alpha particle). The paper proposes two modern methods of obtaining free energy, one of which is somewhat strange, the capillarity. Until one of the two new ideas proposed, the first for the start of the nuclear fusion reaction, and the second one for the possible construction of capillary power plants in the future, it is still necessary to keep the green energy of any type already existing and nuclear fission.

Neutrino oscillations

The source of solar energy is such a nuclear process in which hydrogen nuclei fuse together to form Helium nucleus. In this process, energy is released along with positrons and neutrino. Scientists have absorbed and counted these neutrons thereby revealing many hidden mysteries of the universe and fundamental particles. Research work done in the field of Neutrino Astronomy has given information about three states of neutrino.

Dark atoms with nuclear shell: A status review

Among dark atom scenarios, the simplest and most predictive one is that of O-helium (OHe) dark atoms, in which a leptonlike doubly charged particle O–– is bound to a primordial helium nucleus, and is the main constituent of dark matter. The OHe cosmology has several successes: it leads to a warmer-than-cold-dark matter scenario for large-scale-structure formation, it can provide an explanation for the excess in positron annihilation line in the galactic bulge and it may explain the results of direct dark matter searches. This model liberates the physics of dark atoms from many unknown features of new physics, but it is still not free from astrophysical uncertainties. It also demands a deeper understanding of the details of known nuclear and atomic physics, which are still somewhat unclear in the case of nuclear interacting “atomic” shells. These potential problems of the OHe scenario are also discussed.

The Possibility of Quasi-Bound State Formation of η-Meson with Helium Isotopes

Necessary conditions of quasi-bound state formation of η-meson with isotopes3He,4He have been found within the framework of optical potential model. These conditions have been compared with the findings about helium nucleus densities and with the available information about ηN-scattering length. Thus, we have concluded that within the framework of discussed model η−3He quasi-bound state formation is not possible, but η−4He quasi-bound state formation is possible with great probability.

Decaying Dark Atom Constituents and Cosmic Positron Excess

We present a scenario where dark matter is in the form of dark atoms that can accommodate the experimentally observed excess of positrons in PAMELA and AMS-02 while being compatible with the constraints imposed on the gamma-ray ux from Fermi/LAT. This scenario assumes that the dominant component of dark matter is in the form of a bound state between a helium nucleus and a-2particle and a small component is in the form of a WIMP-like dark atom compatible with direct searches in underground detectors. One of the constituents of this WIMP-like state is a+2metastable particle with a mass of 1 TeV or slightly below that by decaying toe+e+,μ+μ+andτ+τ+produces the observed positron excess. These decays can naturally take place via GUT interactions. If it exists, such a metastable particle can be found in the next run of LHC. The model predicts also the ratio of leptons over baryons in the universe to be close to-3.