Superstrong Magnetic Field Research Articles

Hydrogen-like atom in a superstrong magnetic field: Photon emission and relativistic energy level shift

Following our previous work, additional arguments are presented that in superstrong magnetic fields B ≫ (Zα)2 B 0, B 0 = m 2 c 3/eħ ≈ 4.41 × 1013 G, the Dirac equation and the Schrodinger equation for an electron in the nucleus field following from it become spatially one-dimensional with the only z coordinate along the magnetic field, “Dirac” spinors become two-component, while the 2 × 2 matrices operate in the {0; 3} subspace. Based on the obtained solution of the Dirac equation and the known solution of the “onedimensional” Schrodinger equation by ordinary QED methods extrapolated to the {0; 3} subspace, the probability of photon emission by a “one-dimensional” hydrogen-like atom is calculated, which, for example, for the Lyman-alpha line differs almost twice from the probability in the “three-dimensional” case. Similarly, despite the coincidence of nonrelativistic energy levels, the calculated relativistic corrections of the order of (Zα)4 substantially differ from corrections in the absence of a magnetic field. A conclusion is made that, by analyzing the hydrogen emission spectrum and emission spectra at all, we can judge in principle about the presence or absence of superstrong magnetic fields in the vicinity of magnetars (neutron stars and probably brown dwarfs). Possible prospects of applying the proposed method for calculations of multielectron atoms are pointed out and the possibility of a more reliable determination of the presence of superstrong magnetic fields in magnetars by this method is considered.

On the Possibility of Determining the Magnitude of the Magnetic Field of Magnetars from the Emission Spectra of Hydrogen-Like Atoms

The widths of the spectral emission lines of a hydrogen-like atom in a superstrong magnetic field B >> (Zα)2 B 0, B 0 = m e 2 / e ≈ 4.41·1013 G, have been calculated. Specifically, the width of the α-line of the Lyman series is roughly 2 times smaller than in the absence of a magnetic field. Along with linear polarization of radiation, this makes it possible to determine the magnitude of the magnetic field of magnetars within the limits of the inequality B >> (Zα)2 B 0 from an analysis of the hydrogen emission spectrum. The general expression, so obtained, for the spectral width for an n → n′ transition with emission of a photon allows one in principle to calculate the width of any line of the emission spectrum of hydrogen in such a field with expansion of the possibilities of experimental identification of the latter.

A novel method of omnidirectional defects detection by MFL testing under single axial magnetization at the production stage of lathy ferromagnetic materials

Aiming to the current situation that single axial magnetization can hardly qualified for omnidirectional defects detection, meanwhile, conventional complex magnetization method features with low speed and low efficiency. Thus, a novel method of magnetic flux leakage (MFL) testing for omnidirectional defects based on super-strong single axial magnetization as well as the corresponding detection apparatus were proposed. First, principles of single axial magnetization method were introduced, where a through-coil with high direct current was mainly used to generate the super-strong magnetic field. Then, methods of omnidirectional defects detection through magneto sensor arrays were concretely presented. What’s more, details of equation sets for lateral and longitudinal defects detection and classification were given. Additionally, a summation and comparison combination method was put forward and different defect signal amplitudes were compensated. Naturally, a unified judgment for omnidirectional defects inspection with same sensitivity or accuracy was formed. Most importantly, series of simulations and experiments were conducted, and finally, the feasibility and reliability of the new MFL testing method were demonstrated by those results. The obvious advantages for the suggested method are that it not only makes the detection for omnidirectional defects under single axial magnetization possible, but also the low economic cost, high speed and high efficiency detection for both lateral and longitudinal defects adaptable for various shaped ferromagnetic objects with great application promise in engineering is ultimately accomplished.

Preliminary risks analysis of the IGNITOR Project realization phase

In the framework of the joint Russian – Italian collaboration on the development of the IGNITOR project some preliminary estimates of the risk factors that may be occurring during the realization of the project were recently carried out.A distinctive feature of the IGNITOR project is the fact that it contains some innovative solutions in the areas of research, engineering and technology, often having no analogues not only in industry but also outside the specific laboratories and research centers responsible for the development of necessary components.In addition, it is necessary to point out several peculiarities of the IGNITOR project, which distinguish it from other large-scale scientific projects in the sphere of controlled thermonuclear fusion with magnetic confinement, implemented on the basis of the tokamak technology, and which are risk-related in terms of the project realization:1. The super strong magnetic fields (up to 13 T);2. The high plasma current discharge (up to 11 MA);3. Ohmic heating as the main mechanism of ignition of the thermonuclear fusion reaction.During of the risk analysis investigation the following categories of risks were identified:● political;● economical;● achievement of the main goal of the project;● technical and technological risks;● risks of implementation of the scientific research program;● environmental, safety and socio-economical risks.The different impact factors on the realization phase of the IGNITOR project are shown and analyzed.The conclusions of the risks analysis that were obtained are summarized in the joint Table, where the risk category, the description of the problem, circumstances, risk mitigation method and comments are displayed.

Spatial structure of the modified Coulomb potential in a superstrong magnetic field

The modification of the Coulomb potential due to the enhancement of loop corrections in a superstrong magnetic field is studied numerically. We calculate the modified potential with high precision and obtain the pattern of equipotential lines. The results confirm the general features known from previous studies, however we emphasize some differences in potential structure that can be important for problems with spatially distributed charges.

Neutrino decay to electron andWboson in a superstrong magnetic field in the Early Universe

An intense electromagnetic field makes possible the process of the neutrino decay into electron and W boson that is kinematically forbidden in a vacuum. The exact formula for the probability of ultra high energy neutrino decay in a superstrong magnetic field via the representation for the propagators of the charged particles expanded as sums over Landau levels is derived. The obtained function clarifies previously known approximate formula. The neutrino mean free path is estimated. It is shown, that the resonance peaks present in the decay width for certain neutrino energies correspond to the electron and the W boson creation at specific Landau levels. Some interesting possible manifestations of the process in the conditions of the Early Universe are briefly discussed.

Beta decay of nuclides 56Fe, 62Ni, 64Ni and 68Ni in the crust of magnetars

By introducing the Dirac δ-function and Pauli exclusion principle in the presence of superstrong magnetic fields (SMFs), we investigate the influence of SMFs on beta decay and the change rates of electron fraction (CREF) of nuclides 56Fe, 62Ni, 64Ni and 68Ni in magnetars, which are powered by magnetic field energy. We find that the magnetic fields have a great influence on the beta decay rates, and the beta decay rates can decrease by more than six orders of magnitude in the presence of SMFs. The CREF also decreases by more than seven orders of magnitude in the presence of SMFs.

Carbon-oxygen-neon mass nuclei in superstrong magnetic fields

The properties of $^{12}\mathrm{C},\phantom{\rule{0.16em}{0ex}}^{16}\mathrm{O}$, and $^{20}\mathrm{Ne}$ nuclei in strong magnetic fields $B\ensuremath{\simeq}{10}^{17}$ G are studied in the context of strongly magnetized neutron stars and white dwarfs. The sky3d code is extended to incorporate the interaction of nucleons with the magnetic field and is utilized to solve the time-independent Hartree-Fock equations with a Skyrme interaction on a Cartesian three-dimensional grid. The numerical solutions demonstrate a number of phenomena, which include a splitting of the energy levels of spin-up and -down nucleons, spontaneous rearrangement of energy levels in $^{16}\mathrm{O}$ at a critical field, which leads to jump-like increases of magnetization and proton current in this nucleus, and evolution of the intrinsically deformed $^{20}\mathrm{Ne}$ nucleus toward a more spherical shape under increasing field strength. Many of the numerical features can be understood within a simple analytical model based on the occupation by the nucleons of the lowest states of the harmonic oscillator in a magnetic field.

Magnetars and white dwarf pulsars

The anomalous X-ray pulsars (AXPs) and soft gamma-ray repeaters (SGRs) are a class of pulsars understood as neutron stars (NSs) with super strong surface magnetic fields, namely [Formula: see text][Formula: see text]G, and for that reason are known as magnetars. However, in the last years, some SGRs/AXPs with low surface magnetic fields [Formula: see text]–[Formula: see text][Formula: see text]G have been detected, challenging the magnetar description. Moreover, some fast and very magnetic white dwarfs (WDs) have also been observed, and at least one showed X-ray energy emission as an ordinary pulsar. Following this fact, an alternative model based on WDs pulsars has been proposed to explain this special class of pulsars. In this model, AXPs and SGRs as dense and magnetized WDs can have surface magnetic field [Formula: see text]–[Formula: see text] G and rotate very fast with frequencies [Formula: see text][Formula: see text]rad/s, consistent with the observed rotation periods [Formula: see text]–12)[Formula: see text]s.

Influence of super-strong magnetic fields on beta decay of nuclide Co 59 ${}^{59}\mbox{Co}$ in magnetar surface

Based on the relativistic theory in super-strong magnetic fields (SMFs), we investigate the influence of SMFs on beta decay and the change rates of electron fraction (CREF) of nuclei ${}^{59}\mbox{Co}$ in magnetars. Firstly, we find the magnetic fields have a slight influence on the beta decay rates for a given temperature when $\rho_{7}<1$ . However, the beta decay rates decrease greatly by more than five orders of magnitude when $\rho_{7}>1$ . Secondly, our results show that this effect of SMFs can increase beta reaction rates by two orders magnitude when $10 \leq B_{12} \leq 10^{4}~\mbox{G}$ . For instance, the beta decay rate for ${}^{56}\mbox{Co}$ increases from $4.797\times10^{-3}$ to $3.284\times10^{-1}$ at $\rho_{7}=4.32$ . Finally, we find that the CREF increases about by two orders of magnitude in SMFs and the enhancement factor will be high as 95.95 for $\rho_{7}=4.32$ .

A NEW INSIGHT INTO NEUTRINO ENERGY LOSS BY ELECTRON CAPTURE OF IRON GROUP NUCLEI IN MAGNETAR SURFACES

ABSTRACT Based on the relativistic mean-field effective interactions theory, and the Lai dong model, we discuss the influences of superstrong magnetic fields (SMFs) on electron Fermi energy, nuclear blinding energy, and single-particle level structure in magnetar surfaces. Using the Shell-Model Monte Carlo method and the Random Phase Approximation theory, we analyze the neutrino energy loss rates (NELRs) by electron capture for iron group nuclei in SMFs. First, when B 12 &lt; 100, we find that the SMFs have a slight influence on the NELRs for most nuclides at relativistic low temperatures (e.g., T 9 = 0.233); nevertheless, the NELRs increase by more than four orders of magnitude at relativistic high temperatures (e.g., T 9 = 15.53). When B 12 &gt; 100, the NELRs decrease by more than three orders of magnitude (e.g., at T 9 = 15.53 for 52–61Fe, 55–60Co, and 56–63Ni). Second, for a certain value of magnetic field and temperature, the NELRs increase by more than four orders of magnitude when , but as the density increases (i.e., when ), there is almost no influence on the density of NELRs. For the density around , there is an abrupt increase in NELRs when B 12 ≥ 103.5. Such jumps are an indication that the underlying shell structure has changed due to single-particle behavior by SMFs. Finally, we compare our NELRs with those of Fuller et al. (FFN) and Nabi &amp; Klapdor-Kleingrothaus (NKK). For the case without SMFs, one finds that our rates for certain nuclei are close to about five orders of magnitude lower than FFN and NKK at relativistic low temperatures (e.g., T 9 = 1). However, at a relativistic high temperature (e.g., T 9 = 3), our results are in good agreement with NKK, but about one order of magnitude lower than FFN. For the case with SMFs, our NELRs for some iron group nuclei can be about five orders of magnitude higher than those of FFN and NKK. (Note that B 12, T 9, and ρ 7 are in units of 1012 G, 109 K, and , respectively.)

The Physics of Magnetars II - The Electron Fermi Energy of and the Origin of High X-ray Luminosity of Magnetars

In this paper we discuss in detail the quantization of Landau energy levels of a strongly magnetized and completely degenerate relativistic electron gas in neutron stars. In particular, we focus on the Fermi energy dependence of the magnetic field for a relativistic electron gas in the superstrong magnetic field of magnetars. We would like to point out that some of the results concerning the microscopic number density of states of a strongly magnetized electron gas given by well known statistical physics text books are incorrect. The repeated use of these results in the last five decades probably seriously affects the physics of neutron stars and magnetars. The quantization of Landau energy levels is accurately delineated in terms of the Dirac -δ function. Relatively simple calculation shows that the Fermi energy of a relativistic electron gas in magnetars with superstrong magnetic fields (B>B cr , here B cr is the Landau critical magnetic field, B cr = 4.414 × 10 13 gauss ) increases with magnetic field strength as B 1/4 . On the basis of this simple but important new result we are leading naturally to propose a new mechanism for the production of high X-ray luminosity from magnetars.

Computer-aided modeling of physicochemical characteristics of various energy sources

The authors’ review presents original methodical development works and integrates the research on the modeling of processes and estimation of physicochemical characteristics of natural (hydrocarbons) and chemical (energetic materials) energy sources. A fundamentally new method of energy generation based on transition of excited helium atoms to the superstable state in superstrong magnetic fields is described. A hypothetical possibility for these states to exist was predicted by one of the authors and confirmed by calculations.

Strong screening effects on resonant nuclear reaction 23Mg (p, γ) 24Al in the surface of magnetars

Based on the theory of relativistic superstrong magnetic fields (SMFs), by using the method of Thomas-Fermi-Dirac approximations, we investigate the problem of strong electron screening (SES) in SMFs and the influence of SES on the nuclear reaction of 23Mg (p, γ)24Al. Our calculations show that the nuclear reaction will be markedly effected by the SES in SMFs in the surface of magnetars. Our calculated screening rates can increase two orders of magnitude due to SES in SMFs.

Dynamics of plasma−dust structures formed in a trap created in the narrowing of a current channel in a magnetic field

The geometry and dynamics of plasma−dust structures in a longitudinal magnetic field is studied experimentally. The structures are formed in a glow-discharge trap created in the double electric layer produced as a result of discharge narrowing by means of a dielectric insert introduced in the discharge tube. Studies of structures formed in the new type of glow-discharge trap are of interest from the standpoint of future experiments with complex plasmas in superstrong magnetic fields in which the dust component is magnetized. Different types of dielectric inserts were used: conical and plane ones with symmetric and asymmetric apertures. Conditions for the existence of stable dust structures are determined for dust grains of different density and different dispersity. According to the experimental results, the angular velocity of dust rotation is ≥10 s–1, which is the fastest type of dust motion for all types of discharges in a magnetic field. The rotation is interpreted by analyzing the dynamics of individual dust grains.

Landau-level stability of electrons in superstrong magnetic fields and its influences on electron Fermi energy

Landau-level stability of electrons in superstrong magnetic fields and its influences on electron Fermi energy

Spindown of magnetars: quantum vacuum friction?

Magnetars are proposed to be peculiar neutron stars which could power their X-ray radiation by super-strong magnetic fields as high as ≳ 1014 G. However, no direct evidence for such strong fields has been obtained till now, and the recent discovery of low magnetic field magnetars even indicates that some more efficient radiation mechanism than magnetic dipole radiation should be included. In this paper, quantum vacuum friction (QVF) is suggested to be a direct consequence of super-strong surface fields, therefore the magnetar model could then be tested further through QVF braking. The high surface magnetic field of a pulsar interacting with the quantum vacuum results in a significantly high spindown rate (Ṗ). It is found that a QVF dominates the energy loss of pulsars when the pulsar's rotation period and its first derivative satisfy the relationship P3 Ṗ > 0.63 × 10−16 ξ−4 s2, where ξ is the ratio of the surface magnetic field over the dipole magnetic field. In the “QVF + magnetodipole” joint braking scenario, the spindown behavior of magnetars should be quite different from that in the pure magnetodipole model. We are expecting these results could be tested by magnetar candidates, especially low magnetic field cases, in the future.

Neutrino Spin and Dispersion in Magnetized Medium

The full energy shift of a massive Dirac neutrino in magnetized electron-positron plasma was investigated using the Matsubara imaginary time and real time formalisms. The neutrino dispersion in the magnetized medium was analyzed as a function of the neutrino spin and mass. It was shown that in a superstrong magnetic field the CP-symmetric plasma contribution to the neutrino energy greatly exceeds the analogous correction in the field-free case. The contribution of plasma to the anomalous magnetic moment of a neutrino was obtained.

Nonlinear diffusion waves in high magnetic fields

The nonlinear diffusion of a magnetic field and the large-scale instabilities arising upon an electrical explosion of conductors in a superstrong (2-3 MG) magnetic field were investigated experimentally on the MIG high-current generator (up to 2.5 peak current, 100 ns current rise time). It was observed that in the nonlinear stage of the process, the wavelength of thermal instabilities (striations) increased with a rate of 1.5-3 km/s.

Comment on “Strongly magnetized cold degenerate electron gas: Mass-radius relation of the magnetized white dwarf”

The supermassive white dwarf models proposed by Das and Mukhopadhyaya [Phys. Rev. D 86, 042001 (2012)], based on modifying the equation of state by a superstrong magnetic field in the center, are very far from equilibrium because of the neglect of Lorentz forces, as has recently been shown by Nityananda and Konar [Phys. Rev. D 89, 103017 (2014].