Mass Nuclei Research Articles

Revealing the influence of dark matter on the nature of motion and the families of orbits in axisymmetric galaxy models

An axially symmetric galactic gravitational model composed of a dense, massive and spherical nucleus with an additional dark matter halo component was used, to distinguish between the regular and chaotic character of orbits of stars that move in the meridional plane (R,z). We investigated two different cases: (i) a flat-disk galaxy (ii) an elliptical galaxy. It is of particular interest to reveal how the portion of the dark matter inside the main body of the galaxy influences the ordered or chaotic nature of motion. Varying the ratio of dark matter to stellar mass, we monitored the evolution not only of the percentage of chaotic orbits, but also of the percentages of orbits that compose the main regular resonant families, by classifying regular orbits into different families. Moreover we tried, to reveal how the starting position of the parent periodic orbits of each regular family changes with respect to the fractional portion of dark matter. We compared our results with previous similar work.

Mapping quasifission characteristics and timescales in heavy element formation reactions

Background: The formation of superheavy elements by fusion of two massive nuclei is severely inhibited by the competing quasifission process.Purpose: Through extensive mass-angle distribution measurements, we map out the systematic dependence of quasifission characteristics as a function of the identity of the colliding nuclei.Methods: The Australian National University's Heavy Ion Accelerator Facility and CUBE spectrometer have been used to measure mass-angle distributions for 42 reactions forming heavy elements. Beam energies above their respective capture barriers were used to minimize the known influence of nuclear structure effects.Results: Different mappings of mass-angle distribution characteristics (including timescales) over the nuclear landscape show a systematic dependence on entrance channel and compound nucleus fissilities.Conclusions: The results provide an empirical baseline to assess effects of nuclear structure at lower beam energies, and motivate the testing and validation of complete dynamical models of heavy element fusion through comparison of mass-angle distributions.

Determining the nature of orbits in disk galaxies with non-spherical nuclei

We investigate the regular or chaotic nature of orbits of stars moving in the meridional plane $(R,z)$ of an axially symmetric galactic model with a flat disk and a central, non spherical and massive nucleus. In particular, we study the influence of the flattening parameter of the central nucleus on the nature of orbits, by computing in each case the percentage of chaotic orbits, as well as the percentages of orbits of the main regular families. In an attempt to maximize the accuracy of our results upon distinguishing between regular and chaotic motion, we use both the Fast Lyapunov Indicator (FLI) and the Smaller ALingment Index (SALI) methods to extensive samples of orbits obtained by integrating numerically the equations of motion as well as the variational equations. Moreover, a technique which is based mainly on the field of spectral dynamics that utilizes the Fourier transform of the time series of each coordinate is used for identifying the various families of regular orbits and also to recognize the secondary resonances that bifurcate from them. Varying the value of the flattening parameter, we study three different cases: (i) the case where we have a prolate nucleus (ii) the case where the central nucleus is spherical and (iii) the case where an oblate massive nucleus is present. Furthermore, we present some additional findings regarding the reliability of short time (fast) chaos indicators, as well as a new method to define the threshold between chaos and regularity for both FLI and SALI, by using them simultaneously. Comparison with early related work is also made.

Main restrictions in the synthesis of new superheavy elements: Quasifission and/or fusion fission

The synthesis of superheavy elements stimulates the effort to study the peculiarities of the complete fusion with massive nuclei and to improve theoretical models in order to extract knowledge about reaction mechanism in heavy ion collisions at low energies. We compare the theoretical results of the compound nucleus (CN) formation and evaporation residue (ER) cross sections obtained for the $^{48}$Ca+$^{248}$Cm and $^{58}$Fe+$^{232}$Th reactions leading to the formation of the isotopes A=296 and A=290, respectively, of the new superheavy element Lv (Z=116). The ER cross sections, which can be measured directly, are determined by the complete fusion and survival probabilities of the heated and rotating compound nucleus. That probabilities can not be measured unambiguously but the knowledge about them is important to study the formation mechanism of the observed products. For this aim, the $^{48}$Ca+$^{249}$Cf and $^{64}$Ni+$^{232}$Th reactions have been considered too. The use of the mass values of superheavy nuclei calculated in the framework of the macroscopic-microscopic model by Warsaw group leads to smaller ER cross section for all of the reactions (excluding the $^{64}$Ni+$^{232}$Th reaction) in comparison with the case of using the masses calculated by Peter M\"oller {\it et al}.

The primordial end calculus of prime numbers and mathematics

This Manuscript on the end primordial calculus of mathematics is a new discovery of the spiral nature of the entire mathematical grid at 1:3 by the precise and absolute concordance of regular number spirals and the Prime number spirals based on numbers and their spaces by grid. It is exclusive to IJAMR which has published 8 papers of the author on this new mathematics. The manuscript has NOT been offered to any other journal in the world .The editorial board of Princeton University, USA, Annals of mathematics had been duly informed by letter of the new discovery of the concordance of prime numbers spirals with regular number spirals, but for the sake of fidelity. Mathematics is not complexity, but simplicity, the configuration of 1 is spiral .The relationship between pure mathematical numbers and empty space is a primordial relationship, and well defined by gaps, plus it has been validated by the author by the Publishing of the pure continuous Den-Otter Prime number sieve at 1/6 and 5/6 ( and 1/3 and 2/3),and these prime sieves are reversible .Thus the relationship of the configuration of 1 is in two planes that expand in the frame of (5/6 and 1/6 ) and (1/3 and 2/3)are represented by spiral configuration , expressed by these numbers, as in :All prime numbers spirals are assigned infinitely by the simple -1 offset of the two spiral numbers cords 1/3+2/3=1 5/6+1/6=1 1/3-1/6=1/6 5/6-2/3=1/6 1/3+1/6=0.5 5/6+2/3=1.5 1.5/0.5=3 Note: the above is also confirmed by Arabian numerical shown below. Primordial mathematics as created by the creator is absolute and precise whilst the mathematics invented by man is approximate .Current Mathematics of a thousand years has accomplished much by approximate theory, and it is very possible to land a man on the moon by approximate mathematics, but to precisely understand mass and energy, the nucleus of mass and the vastness of space, one must understand the precise nature and curvature of space. Space and mathematics are curved precisely at 1:3 from primordial times( the basis for the π as shown under the publication Unified Theorem), and the warping of space is related to the 1:3 separation at precise 19 correct degrees separation and the precise right angled separation at 1:3 is at 360/19 degrees. This mathematics is about the curved lay of the grid of mathematics and cannot be understood by the current linear obsession of mathematics, but the readers are immediately referred to the 8 published papers of the author as referenced below. The calculus below virtually negates the current mathematics ideas of linear ascension theories of the past 500 years. This calculus is true for all prime numbers. This involves a precise “combing” of all prime number spirals around a half line. This is clearly and singularly the solution to prime number spiral calculus, which is fairly simple after this discovery. The ruminations of George Riemann and others of the past 500 years in linear ascension mathematics of prime numbers are nonfunctional irrelevant mathematics, just collateral observations of the correct mathematics which is presented here as “Primum movens” of mathematics. In Mathematics there is only a single best resolution, whilst collateral equations abound, as they have for 500 years for prime numbers which we have proved are basically by two chords and ascend by a half-line. Einstein’s observations and ruminations likewise are collateral and not central to the fact that the universe is precisely curved, and ascension of prime numbers are by two spiral chords.

Exploring the origin, the nature, and the dynamical behavior of distant stars in galaxy models

We explore the regular or chaotic nature of orbits moving in the meridional plane of an axially symmetric galactic gravitational model with a disk, a dense spherical nucleus and some additional perturbing terms corresponding to influence from nearby galaxies. In order to obtain this we use the Smaller ALingment Index (SALI) technique integrating extensive samples of orbits. Of particular interest is the study of distant, remote stars moving in large galactocentric orbits. Our extensive numerical experiments indicate that the majority of the distant stars perform chaotic orbits. However, there are also distant stars displaying regular motion as well. Most distant stars are ejected into the galactic halo on approaching the dense and massive nucleus. We study the influence of some important parameters of the dynamical system, such as the mass of the nucleus and the angular momentum, by computing in each case the percentage of regular and chaotic orbits. A second order polynomial relationship connects the mass of the nucleus and the critical angular momentum of the distant star. Some heuristic semi-theoretical arguments to explain and justify the numerically derived outcomes are also given. Our numerical calculations suggest that the majority of distant stars spend their orbital time in the halo where it is easy to be observed. We present evidence that the main cause for driving stars to distant orbits is the presence of the dense nucleus combined with the perturbation caused by nearby galaxies. The origin of young O and B stars observed in the halo is also discussed.

Nuclear weak interactions, supernova nucleosynthesis and neutrino oscillation

We study the nuclear weak response in light-to-heavy mass nuclei and calculate neutrino-nucleus cross sections. We apply these cross sections to the explosive nucleosynthesis in core-collapse supernovae and find that several isotopes of rare elements 7Li, 11B, 138La, 180Ta and several others are predominantly produced by the neutrino-process nucleosynthesis. We discuss how to determine the suitable neutrino spectra of three different flavors and their anti-particles in order to explain the observed solar system abundances of these isotopes, combined with Galactic chemical evolution of the light nuclei and the heavy r-process elements. Light-mass nuclei like 7Li and 11B, which are produced in outer He-layer, are strongly affected by the neutrino flavor oscillation due to the MSW (Mikheyev-Smirnov-Wolfenstein) effect, while heavy-mass nuclei like 138La, 180Ta and r-process elements, which are produced in the inner O-Ne-Mg layer or the atmosphere of proto-neutron star, are likely to be free from the MSW effect. Using such a different nature of the neutrino-process nucleosynthesis, we study the neutrino oscillation effects on their abundances, and propose a new novel method to determine the unknown neutrino oscillation parameters, θ13 and mass hierarchy, simultaneously. There is recent evidence that some SiC X grains from the Murchison meteorite may contain supernova-produced neutrino-process 11B and 7Li encapsulated in the grains. Combining the recent experimental constraints on θ13, we show that although the uncertainties are still large, our method hints at a marginal preference for an inverted neutrino mass hierarchy for the first time.

Numerical Analyses of CERN 200 GeV/A Heavy-Ion Collisions Based on a Hydrodynamical Model with Phase Transition

We numerically analyze recent high energy heavy-ion collision experiments based on a hydrodynamical model with phase transition and discuss a systematic change of initial state of QGP-fluid depending on colliding-nuclei's mass. In a previous paper, we formulated a (3+l)-dimensional hydrodynamical model for quark-gluon plasma with phase transition and discussed numerically the space-time evolution in detail. We here compare the numerical solution with the hadronic distributions given by CERN WA80 and NA35. Systematic analyses of the experiments with various colliding nuclei enable us to discuss the dependences of the initial parameters of the hydrodynamical model on colliding nuclei's mass. Furthermore, extrapolating the present experiments, we derive the possible hadronic distributions for lead-lead 150 GeV/A collision.

What perspectives for the synthesis of heavier superheavy nuclei? Results and comparison with models

The possibility to synthesize heavier superheavy elements in massive nuclei reactions is strongly limited by the hindrance to complete fusion of reacting nuclei: due to the onset of the quasifission process in the entrance channel, which competes with complete fusion, and by strong increase of the fission yield along the de-excitation cascade of the compound nucleus in comparison to the evaporation residue formation. We present a wide and detailed procedure allowing us to describe the experimental results (evaporation residue nuclei and fissionlike products) in the mass asymmetric and symmetric reactions. Very reliable estimations and perspectives for the synthesis of superheavy elements in many massive nuclei reactions up to Z = 120 and eventually also for Z > 120 have been obtained.

Revealing the Character of Orbits in a Binary System Consisting of a Primary Galaxy and a Satellite Companion

AbstractIn this article, we present a galactic gravitational model of three degrees of freedom (3D), in order to study and reveal the character of the orbits of the stars, in a binary stellar system composed of a primary quiet or active galaxy and a small satellite companion galaxy. Our main dynamical analysis will be focused on the behaviour of the primary galaxy. We investigate in detail the regular or chaotic nature of motion, in two different cases: (i) the time-independent model in both 2D and 3D dynamical systems and (ii) the time-evolving 3D model. For the description of the structure of the 2D system, we use the classical method of the Poincaré (x, px), y = 0, py < 0 phase plane. In order to study the structure of the phase space of the 3D system, we take sections in the plane y = 0 of the 3D orbits, whose initial conditions differ from the plane parent periodic orbits, only by the z component. The set of the four-dimensional points in the (x, px, z, pz) phase space is projected on the (z, pz) plane. The maximum Lyapunov characteristic exponent is used in order to make an estimation of the chaoticity of our galactic system, in both 2D and 3D dynamical models. Our numerical calculations indicate that the percentage of the chaotic orbits increases when the primary galaxy has a dense and massive nucleus. The presence of the dense galactic core also increases the stellar velocities near the center of the galaxy. Moreover, for small values of the distance R between the two bodies, low-energy stars display chaotic motion, near the central region of the galaxy, while for larger values of the distance R, the motion in active galaxies is entirely regular for low-energy stars. Our simulations suggest that in galaxies with a satellite companion, the chaotic nature of motion is not only a result of the galactic interaction between the primary galaxy and its companion, but also a result caused by the presence of the dense nucleus in the core of the primary galaxy. Theoretical arguments are presented in order to support and interpret the numerically derived outcomes. Furthermore, we follow the 3D evolution of the primary galaxy, when mass is transported adiabatically from the disk to the nucleus. Our numerical results are in satisfactory agreement with observational data obtained from the M51-type binary stellar systems. A comparison between the present research and similar and earlier work is also made.

Unveiling the Influence of Dark Matter in Axially Symmetric Galaxies

AbstractWe investigate the regular or chaotic nature of orbits of stars moving in the meridional plane (R,z) of an axially symmetric galactic model with a dense, massive spherical nucleus and a dark matter halo component. In particular, we study the influence of the fractional portion of the dark matter, by computing in each case the percentage of chaotic orbits, as well as the percentages of orbits of the main regular resonant families. In an attempt to distinguish between regular and chaotic motion, we use the fast Lyapunov indicator method to extensive samples of orbits obtained by integrating numerically the equations of motion as well as the variational equations. Furthermore, a technique which is based mainly on the field of spectral dynamics that utilises the Fourier transform of the time series of each coordinate is used for identifying the various families of regular orbits and also to recognise the secondary resonances that bifurcate from them. Two cases are studied in our work: (i) the case where we have a disk galaxy model and (ii) the case where our model represents an elliptical galaxy. A comparison with early related work is also made.

A dumbbell model with five parameters describing nuclear fusion or fission

We propose a five-parameter dumbbell model to describe the fusion and fission processes of massive nuclei, where the collective variables are: the distance ρ between the center-of-mass of two fusing nuclei, the neck parameter υ, asymmetry D, two deformation variables β1 and β2. The present model has macroscopic qualitative expression of polarization and nuclear collision of head to head, sphere to sphere, waist to waist and so on. The conception of the “projectile eating target" based on open mouth and swallow is proposed to describe the nuclear fusion process, and our understanding of the probability of fusion and quasi-fission is in agreement with some previous work. The calculated fission barriers of a lot of compound nuclei are compared with the experimental data.

89 INHIBITION OF MAPKK AND GSK3 SIGNALLING PROMOTES DEVELOPMENT AND EPIBLAST-SPECIFIC EXPRESSION OF PLURIPOTENCY MARKERS IN BOVINE BLASTOCYSTS

During blastocyst development, the inner cell mass segregates into the epiblast and the hypoblast. These 2 tissues form morphologically and molecularly distinct cell populations that subsequently develop into the embryo proper and some extraembryonic components, respectively. In mouse, isolated epiblast cells can be directly converted into pluripotent embryonic stem cells, capable of differentiating into all cell types of an adult animal. Epiblast pluripotency is promoted by pharmacological inhibition of mitogen-activated protein kinase kinase (Mapkk). This shields epiblast cells from secreted fibroblast growth factor (Fgf), which would otherwise instruct them to exit pluripotency and differentiate into extraembryonic lineages. Indirect stimulation of the Wnt pathway by inhibiting glycogen synthase kinase 3 (GSK3) further antagonises inductive Fgf/Mapkk signalling. Thus the double inhibition (2i) of Mapkk and Gsk3 effectively promotes pluripotency (Q. L. Ying et al. 2008 Nature 453, 519–523; J. Nichols et al. 2009 Development 136, 3215–3222). We investigated the effect of 2i culture on bovine blastocysts. The IVF embryos were cultured in the presence of dimethyl sulfoxide or inhibitors of MAPKK (0.4 µM PD0325901) and GSK3 (3 µM CHIR99021) from the zygote (Day 1) stage onward. Compared to vehicle controls, 2i increased the abundance of cumulus cells in bovine IVF cultures, compromising blastocyst formation in cumulus-intact (248/823 = 30% v. 211/824 = 26%, respectively, n = 10; P < 0.05) but not cumulus-free cultures (546/1653 = 33% v. 572/1674 = 34%, respectively, n = 15; P = 0.51). In all subsequent experiments, we therefore cultured cumulus-free zygotes in 2i v. dimethyl sulfoxide until the blastocyst stage. This treatment increased the proportion of hatching (19/433 = 4% v. 7/416 = 2%, respectively, n = 10; P < 0.05) at the expense of early blastocysts (70/433 = 16% v. 93/416 = 22%, respectively, n = 11; P < 0.05). Differential staining of expanded IETS grade 1 and 2 blastocysts showed that 2i culture increased putative inner cell mass, trophectoderm, and total cell nuclei numbers by about 30% compared with controls (57 v. 43, 89 v. 69, and 146 v. 112, respectively; P < 0.01). Accelerated development and increased cell numbers were accompanied by gene expression changes in grade 1 and 2 blastocysts. Under 2i conditions, mRNA abundance of putative epiblast markers NANOG and SOX2 was >3-fold increased (P < 0.0001 and P < 0.01, respectively), and the putative hypoblast marker GATA4 was 2-fold reduced (P < 0.05). Other lineage-related markers (POU5F1, KLF4, DPPA3, and CDX2) showed no significant changes. Using microsurgical blastocyst dissection, we found that the increase in NANOG and SOX2 levels was specific to the inner cell mass-containing portion (7-fold for NANOG and 3-fold for SOX2; P < 0.00005 and P < 0.05, respectively) and not due to ectopic expression in the trophoblast-containing part, which showed similarly low expression levels for both genes. In summary, 2i treatment primed bovine blastocysts for pluripotency in the epiblast. Supported by MSI C10X1002.

Transition between order and chaos in a composite disk galaxy model with a massive nucleus and a dark matter halo

We investigate the transition from regular to chaotic motion in a composite galaxy model with a disk-halo, a massive dense nucleus and a dark halo component. We obtain relationships connecting the critical value of the mass of the nucleus or the critical value of the angular momentum Lzc, with the mass Mh of the dark halo, where the transition from regular motion to chaos occurs. We also present 3D diagrams connecting the mass of nucleus the energy and the percentage of stars that can show chaotic motion. The fraction of the chaotic orbits observed in the (r,pr) phase plane, as a function of the mass of the dark halo is also computed. We use a semi-numerical method, that is a combination of theoretical and numerical procedure. The theoretical results obtained using the version 8.0 of the Mathematica package, while all the numerical calculations were made using a Bulirsch–Stöer FORTRAN routine in double precision. The results can be obtained in semi-numerical or numerical form and give good description for the connection of the physical quantities entering the model and the transition between regular and chaotic motion. We observe that the mass of the dark halo, the mass of the dense nucleus and the Lz component of the angular momentum, are important physical quantities, as they are linked to the regular or chaotic character of orbits in disk galaxies described by the model. Our numerical experiments suggest, that the amount of the dark matter plays an important role in disk galaxies represented by the model, as the mass of the halo affects, not only the regular or chaotic nature of motion but it is also connected with the existence of the different families of regular orbits. Comparison of the present results with earlier work is also presented.

Formation and propagation of MHD jets - relativistic jets, radiation pressure, and shock-induced rotation

We present recent results of magnetohydrodynamic (MHD) simulations of jet formation and propagation, discussing a variety of astrophysical setups. In the first approach the role of the disk magnetic flux profile and disk mass flux profile concerning the jet collimation degree is investigated. Our results suggest (and quantify) that in general magnetized outflows launched from a compact region close to the inner disk radius tend to be less collimated. The second setup considers simulation of relativistic MHD jet formation, considering jet launched from the surface of a Keplerian disks, demonstrating - for the first time - the self-collimating ability of relativistic MHD jets. We obtain Lorentz factors up to ≃ 10 while acquiring a high degree of collimation of about 1 degree. We then present MHD jet formation simulations taking into account radiation pressure of a central luminous source. We investigate radiative effects on jet collimation and propagation - an environment which is interesting for outflows from massive young stars and active galactic nuclei. Finally, we present a model which explains a possible jet rotation by shock compression of an intrinsic helical magnetic field.

Order and chaos in a galactic model with a strong nuclear bar

We use a composite gravitational galactic model consisting of a disk, a halo, a massive nucleus and a strong nuclear bar, in order to study the connections between global and local parameters in a realistic dynamical system. The local model is constructed from a two-dimensional perturbed harmonic oscillator and can be derived by expanding the global model in the vicinity of the central stable Lagrange equilibrium point. The frequencies of oscillations are not arbitrary, but they are connected with all the parameters involved with the global model. Moreover, the value of the local energy is also connected with the value of the global energy. Low and high energy stars in the global model display chaotic motion. Comparison with previous research reveals that the presence of the massive nucleus is responsible for the chaotic motion of the low energy stars. In the local motion, the low energy stars show interesting resonance phenomena, but the chaotic motion, if any, is negligible. On the contrary, the high energy stars do not show bounded motion in the local model. This is an indication of particular activity near the center of galaxies possessing massive nuclei.

Exploring the nature of orbits in a galactic model with a massive nucleus

In the present article, we use an axially symmetric galactic gravitational model with a disk–halo and a spherical nucleus, in order to investigate the transition from regular to chaotic motion for stars moving in the meridian (r,z) plane. We study in detail the transition from regular to chaotic motion, in two different cases: the time independent model and the time evolving model. In both cases, we explored all the available range regarding the values of the main involved parameters of the dynamical system. In the time dependent model, we follow the evolution of orbits as the galaxy develops a dense and massive nucleus in its core, as mass is transported exponentially from the disk to the galactic center. We apply the classical method of the Poincaré (r,pr) phase plane, in order to distinguish between ordered and chaotic motion. The Lyapunov Characteristic Exponent is used, to make an estimation of the degree of chaos in our galactic model and also to help us to study the time dependent model. In addition, we construct some numerical diagrams in which we present the correlations between the main parameters of our galactic model. Our numerical calculations indicate, that stars with values of angular momentum Lz less than or equal to a critical value Lzc, moving near to the galactic plane, are scattered to the halo upon encountering the nuclear region and subsequently display chaotic motion. A linear relationship exists between the critical value of the angular momentum Lzc and the mass of the nucleus Mn. Furthermore, the extent of the chaotic region increases as the value of the mass of the nucleus increases. Moreover, our simulations indicate that the degree of chaos increases linearly, as the mass of the nucleus increases. A comparison is made between the critical value Lzc and the circular angular momentum Lz0 at different distances from the galactic center. In the time dependent model, there are orbits that change their orbital character from regular to chaotic and vise versa and also orbits that maintain their character during the galactic evolution. These results strongly indicate that the ordered or chaotic nature of orbits, depends on the presence of massive objects in the galactic cores of the galaxies. Our results suggest, that for disk galaxies with massive and prominent nuclei, the low angular momentum stars in the associated central regions of the galaxy, must be in predominantly chaotic orbits. Some theoretical arguments to support the numerically derived outcomes are presented. Comparison with similar previous works is also made.

Processes in massive nuclei reactions and the way to complete fusion of reactants. What perspectives for the synthesis of heavier superheavy elements?

By using the dinuclear system (DNS) model we determine the capture of reactants at the first stage of reaction, the competition between the DNS decay by the quasifission (QF) and the complete fusion (CF) process up to formation of the compound nucleus (CN) having compact shape. Further evolution of the CN is considered as its fission into two fragments or formation of evaporation residues (ER) by its cooling after emission of neutrons or/and charged light particles. Disappearance of the CN fission barrier due to its fast rotation leads to the fast fission (FF) by formation of fissionlike fragments. The results of calculations for the mass symmetric 136 Xe+ 136 Xe reaction, almost mass symmetric 108 Mo+ 144 Ba reaction, and mass asymmetric like 24 Mg+ 238 U and 34 S+ 248 Cm reactions are discussed. The fusion probability P CN calculated for many massive nuclei reactions leading to formation of superheavy nuclei have been analyzed. The reactions which can lead in perspective to the synthesis of superheavy elements in the Z = 120 − 126 range and, eventually, also to heaviest nuclei, are discussed.

Investigation and Simulation on Amorphous Formation and Growth

The amorphous formation mechanism was studied from the viewpoint of the crystallography. The experimental results showed that the heterogeneity atoms with chemical bonds had a higher capability of forming into compounds than that of congener atoms. It was proposed that the banded structure was induced by the variation of active atoms with a proper thickness, alternated depletion and enrichment of anions in the diffusion layer due to generation and evolution of hydrogen gas. The chemical force plays an important part in the formation. The factors working on chemical reaction affect the formation in the same. A number of steady motes are in a high speed movement, and collide with each other in all probability. The formation of amorphous alloys is the result of massive nucleus appearance, which was proposed from the crystallography in this paper. The cause of the chaotic distribution is of the suppression of each nucleus growth. The short-range order atomic structure is of the atomic nucleus growth orientation. And the long-range disorder structure is of the massive nucleus suppression growth.

Investigation and Simulation on Amorphous Formation and Growth

The amorphous formation mechanism was studied from the viewpoint of the crystallography. The experimental results showed that the heterogeneity atoms with chemical bonds had a higher capability of forming into compounds than that of congener atoms. It was proposed that the banded structure was induced by the variation of active atoms with a proper thickness, alternated depletion and enrichment of anions in the diffusion layer due to generation and evolution of hydrogen gas. The chemical force plays an important part in the formation. The factors working on chemical reaction affect the formation in the same. A number of steady motes are in a high speed movement, and collide with each other in all probability. The formation of amorphous alloys is the result of massive nucleus appearance, which was proposed from the crystallography in this paper. The cause of the chaotic distribution is of the suppression of each nucleus growth. The short-range order atomic structure is of the atomic nucleus growth orientation. And the long-range disorder structure is of the massive nucleus suppression growth.