Account Magnetic Effects Research Articles

Formation of Hydrogen Miniatoms in the Medium of Free Electrons–the Key to the Mechanism of Low-energy Nuclear Reactions

We have modeled the behavior of hydrogen atoms in the flow of free electrons in metals by the molecular dynamic method. The trajectories of the particles were calculated by numerically solving a system of differential equations of mechanics. Relativistic equations were used, and the interaction of particles was considered Coulombic without taking into account magnetic effects. About 104 stories were modeled, each of them containing up to 100 collisions of free electrons with a hydrogen atom. The total number of simulated atoms that experienced collisions was ∼ 106. Dynamic modeling revealed the formation of neutral particles consisting of protons (deuterons) with an electron rotating around them in nonstationary, close to elliptical orbits with an apogee to a distance of less than 10−11 cm and to a perigee of ∼ 10−12 cm. These particles, which are continuously changing in size and shape, are up to 3 to 4 orders of magnitude smaller than ordinary hydrogen atoms, and 1-2 orders of magnitude larger than neutrons. Such nonstationary hydrogen miniatoms can exist for a short time (on our estimate, up to ∼ 10−12 sec.) in the environment of free electrons of metals, easily move in them and, like neutrons, approach the nuclei of isotopes of hydrogen or other elements at a distance at which nuclear fusion reactions or transmutation of elements are possible due to the tunneling effect. Taking into account the formation of such hydrogen miniatoms the previously calculated rate of low-energy nuclear reactions in metals1−6 increases more than by 5 – 6 orders of magnitude, that is, to values corresponding to experimental data. Formation of hydrogen miniatoms in the medium of free electrons is of primary importance in the mechanism of low-energy nuclear reactions.

Determination of possible responses of Radon-222, magnetic effects, and total electron content to earthquakes on the North Anatolian Fault Zone, Turkiye: an ARIMA and Monte Carlo Simulation

Around the world, earthquake forecasting studies have become very important nowadays due to the increase in number of fatal earthquakes annually. This paper proposes to achieve a possible relationship between soil radon gas concentration and atmospheric total electron content (TEC) during earthquakes taking into account magnetic effects on the North Anatolian Fault Zone (NAFZ) in Turkiye. The ARIMA and Monte Carlo simulation (MCS) are employed for determining radon gas concentrations by taking into account magnetic effects as an innovative approach. In the study area, relatively small and medium-scale earthquakes have taken place during the observation period. As a result of the investigations, the relationships between each of the parameters and earthquakes are determined; hence, a good relationship is obtained between Rn gas anomaly and micro-seismic activity. In the ionosphere, geomagnetic activity has a primary impact and long duration on TEC distribution, but due to micro-seismic events it has rather small influence. The proposed ARIMA and MCS simulations to detect changes in soil Rn gas concentrations have significant results for detecting micro-seismic activity anomalies.

Photometric magnetic-activity metrics tested with the Sun: application toKeplerM dwarfs

The Kepler mission has been providing high-quality photometric data leading to many breakthroughs in the exoplanet search and in stellar physics. Stellar magnetic activity results from the interaction between rotation, convection, and magnetic field. Constraining these processes is important if we want to better understand stellar magnetic activity. Using the Sun, we want to test a magnetic activity index based on the analysis of the photometric response and then apply it to a sample of M dwarfs observed by Kepler. We estimate a global stellar magnetic activity index by measuring the standard deviation of the whole time series, Sph. Because stellar variability can be related to convection, pulsations or magnetism, we need to ensure that this index mostly takes into account magnetic effects. We define another stellar magnetic activity index as the average of the standard deviation of shorter subseries which lengths are determined by the rotation period of the star. This way we can ensure that the measured photometric variability is related to starspots crossing the visible stellar disc. This new index combined with a time-frequency analysis based on the Morlet wavelets allows us to determine the existence of magnetic activity cycles. We measure magnetic indexes for the Sun and for 34 M dwarfs observed by Kepler. As expected, we obtain that the sample of M dwarfs studied in this work is much more active than the Sun. Moreover, we find a small correlation between the rotation period and the magnetic index. Finally, by combining a time-frequency analysis with phase diagrams, we discover the presence of long-lived features suggesting the existence of active longitudes on the surface of these stars.