Robert J Buenker Buenker
Robert J Buenker Buenker
Institution: Faculty of C-Mathematics and Natural Sciences, Bergische Universität Wuppertal,
Email: rjbuenker@gmail.com
A number of the most often cited results of relativity theory deal with the relationships between energy, momentum and inertial mass. The history of how Einstein and Planck came to these conclusions is reviewed. It is pointed out that considerations of how the speed of light is affected by the motio...
More
A number of the most often cited results of relativity theory deal with the relationships between energy, momentum and inertial mass. The history of how Einstein and Planck came to these conclusions is reviewed. It is pointed out that considerations of how the speed of light is affected by the motion of the Earth played a determining role in these developments. After the Michelson-Morley null-interference result became available, Voigt introduced a new space-time transformation by amending the classical Galilean transformation so that the speed of light in free space has the same value of c regardless of the state of motion of both the light source and the observer. This led to the Lorentz transformation which has been the cornerstone of relativity theory for
the past century. A thought experiment is presented which proves, however, that there are many situations for which the measured speed of light is NOT equal to c. Furthermore, it is pointed out that the rate of an inertial clock cannot change spontaneously, which result is perfectly compatible with Newton’s First Law of Kinetics (Law of Inertia). This result contradicts the space-time mixing characteristic of the Lorentz transformation and leads to the conclusion that events which are spontaneous for one inertial frame will also be so for every other one. The uniform scaling procedure is a generalization of this result for all other physical properties than elapsed times. Its application shows that the commonly accepted relationships between energy and momentum are
only special cases in which it is assumed that the observer is stationary in the rest frame in which force has been applied to cause the object’s acceleration
Less
Posted 2 years ago
Berov G Lyubomir
Berov G Lyubomir
Institution: Engineer, Independent Innovative Ideas Researcher, Smolyan 4700,
Email: my_kaly1@mbox.contact.bg
The present, at any particular moment, is the realization of one of the many intentions of the All-creating Intellect. Here "realization" specifically means the materialization or the appearance of an object in the material world, which had not existed until now. This newly born material object exis...
More
The present, at any particular moment, is the realization of one of the many intentions of the All-creating Intellect. Here "realization" specifically means the materialization or the appearance of an object in the material world, which had not existed until now. This newly born material object exists only for the duration of the moment of "now". This moment is infinitely short, or, if we use a concept from calculus, it is infinitesimal in duration. In my hypothesis, this new object is a product of a specific energy field of the All-creating Intellect. We call this particular energy field Time.
Less
Posted 2 years ago
It is widely believed that Hawking radiation originates from excitations near the horizons of black holes [1,2,3]. However, Giddings [2] proposed that the Hawking radiation spectrum that characterizes evaporating semi-classical black holes originates from a quantum “atmosphere”, which extends be...
More
It is widely believed that Hawking radiation originates from excitations near the horizons of black holes [1,2,3]. However, Giddings [2] proposed that the Hawking radiation spectrum that characterizes evaporating semi-classical black holes originates from a quantum “atmosphere”, which extends beyond the horizon of a black hole. Although several research projects have been conducted in this field, they have not yet taken into account the effect of Rényi entropy. In the present article, we will therefore consider the effect of Rényi entropy on Hawking radiation power. We assume that if the effect of Rényi entropy is very small, we suggest that the Hawking radiation should originate from the quantum “atmosphere” which extends beyond the black hole’s horizon for finite dimensions. That is, that Giddings’ suggestion is the more likely of the above possibilities. However, for infinite dimensions, both suggestions are equally credible. We briefly consider the very large effect of Rényi entropy on Hawking radiation power as well. We find that if the effect of Rényi entropy is very large and ω/TBH is very small, then the power spectral density SR is proportional to the power spectral density SBH.
Less
Posted 2 years ago
Kamila Sieja
Kamila Sieja
Institution: Institute Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (CNRS, UMR7178),
Email: la.sieja@iphc.cnrs.fr
Neutron-rich Sr nuclei around N = 60 exhibit a sudden shape transition from a spherical ground state to strongly prolate-deformed. Recently, much new insight into the structure of Sr isotopes in this region has been gained through experimental studies of the excited levels, transition strengths, and...
More
Neutron-rich Sr nuclei around N = 60 exhibit a sudden shape transition from a spherical ground state to strongly prolate-deformed. Recently, much new insight into the structure of Sr isotopes in this region has been gained through experimental studies of the excited levels, transition strengths, and spectroscopic factors. In this work, a “classic” shell model description of strontium
isotopes from N = 50 to N = 58 is provided, using a natural valence space outside the 78Ni core. Both even–even and even–odd isotopes are addressed. In particular, spectroscopic factors are computed to shed more light on the structure of low-energy excitations and their evolution along the Sr chain. The origin of deformation at N = 60 is mentioned in the context of the present and previous shell model and Monte Carlo shell model calculations.
Less
Posted 2 years ago
In this paper we consider the correspondence between the tachyon dark energy model and the Tsallis holographic dark energy scenario in an FRW universe. We demonstrate the Tsallis holographic description of tachyon dark energy in an FRW universe and reconstruct the potential and basic results of the ...
More
In this paper we consider the correspondence between the tachyon dark energy model and the Tsallis holographic dark energy scenario in an FRW universe. We demonstrate the Tsallis holographic description of tachyon dark energy in an FRW universe and reconstruct the potential and basic results of the dynamics of the scalar field which describe the tachyon cosmology. In a flat universe, in the tachyon model of Tsallis holographic dark energy, independently of the existence of interaction between dark energy and matter or not, T˙ 2 must always be zero. Therefore, the equation of state ωD is always −1 in such a flat universe. For a non-flat universe, T˙ 2 cannot be zero so that ωD 6= −1 which cannot be used to explain the origin of the cosmological constant. T˙ 2 monotonically decreases with the increasing of cos(Rh/a) and cosh(Rh/a) for different δs. In particular, for an open universe, T˙ 2 is always larger than zero while for a closed universe, T˙ 2 is always smaller than zero which is physically invalid. In addition, we conclude that with the increasing of cos(Rh/a) and cosh(Rh/a), T˙ 2 always decreases monotonically for irrespective of the value of b2.
Less
Posted 2 years ago
Anand K. Bhatia
Anand K. Bhatia
Institution: Heliophysics Science Division, NASA/Goddard Space Flight Center,
Email: d.k.bhatia@nasa.gov
The excitation cross-sections of the nS states of atomic hydrogen, n = 2 to 6, by electron
impact on the ground state of atomic hydrogen were calculated using the variational polarizedorbital method at various incident electron energies in the range 10 to 122 eV. Converged excitation
cross-sectio...
More
The excitation cross-sections of the nS states of atomic hydrogen, n = 2 to 6, by electron
impact on the ground state of atomic hydrogen were calculated using the variational polarizedorbital method at various incident electron energies in the range 10 to 122 eV. Converged excitation
cross-sections were obtained using sixteen partial waves (L = 0 to 15). Excitation cross-sections to
2S state, calculated earlier, were calculated at higher energies than before. Results obtained using
the hybrid theory (variational polarized orbital method) are compared to those obtained using other
approaches such as the Born–Oppenheimer, close-coupling, R-matrix, and complex-exterior scaling
methods using only the spherical symmetric wave functions. Phase shifts and elastic cross-sections
are given at various energies and angular momenta. Excitation rate coefficients were calculated at
various electron temperatures, which are required for plasma diagnostics in solar and astrophysics to
infer plasma parameters. Excitation cross-sections are compared with those obtained by positron
impact excitation.
Less
Posted 2 years ago
Genki Shibukawa
Genki Shibukawa
Institution: University
Email: info@res00.com
We present an explicit formula of the powers for the 2×2 quantum matrices, that is a natural quantum analogue of the powers of the
usual 2 × 2 matrices. As applications, we give some non-commutative relations of the entries of the powers for the 2 × 2 quantum matrices, which is a simple proof of...
More
We present an explicit formula of the powers for the 2×2 quantum matrices, that is a natural quantum analogue of the powers of the
usual 2 × 2 matrices. As applications, we give some non-commutative relations of the entries of the powers for the 2 × 2 quantum matrices, which is a simple proof of the results of Vokos-Zumino-Wess (1990).
Less
Posted 2 years ago
Muhamed Amin
Muhamed Amin
Institution: Department of Sciences, University College Groningen, University of Groningen, Hoendiepskade
Email: m.a.a.amin@rug.nl
Serial Femtosecond Crystallography at the X-ray Free Electron Laser (XFEL) sources enabled the imaging
of the catalytic intermediates of the oxygen evolution reaction of Photosystem II. However, due to the
incoherent transition of the S-states, the resolved structures are a convolution from diff...
More
Serial Femtosecond Crystallography at the X-ray Free Electron Laser (XFEL) sources enabled the imaging
of the catalytic intermediates of the oxygen evolution reaction of Photosystem II. However, due to the
incoherent transition of the S-states, the resolved structures are a convolution from different catalytic states.
Here, we train Decision Tree Classifier and K-mean clustering models on Mn compounds obtained from
the Cambridge Crystallographic Database to predict the S-state of the X-ray, XFEL, and CryoEm structures
by predicting the Mn's oxidation states in the oxygen evolving complex (OEC). The model agrees mostly
with the XFEL structures in the dark S1 state. However, significant discrepancies are observed for the
excited XFEL states (S2, S3, and S0) and the dark states of the X-ray and CryoEm structures. Furthermore,
there is a mismatch between the predicted S-states within the two monomers of the same dimer, mainly in
the excited states. The model suggests that improving the resolution is crucial to precisely resolve the
geometry of the illuminated S-states to overcome the noncoherent S-state transition. In addition, significant
radiation damage is observed in X-ray and CryoEM structures, particularly at the dangler Mn center (Mn4).
Our model represents a valuable tool for investigating the electronic structure of the catalytic metal cluster
of PSII to understand the water splitting mechanism.
Less
Posted 2 years ago
In the article, the fireball formed in the collision of relativistic nuclei is considered as a quantum object. Based on this, an attempt is made to explain the difference in the measurements of hyperon yields in the two experiments - NA49 and NA57. Using the basic principles of quantum mechanics, it...
More
In the article, the fireball formed in the collision of relativistic nuclei is considered as a quantum object. Based on this, an attempt is made to explain the difference in the measurements of hyperon yields in the two experiments - NA49 and NA57. Using the basic principles of quantum mechanics, it was shown that a fireball can have two quantum states - with and without ignited Quark-Gluon Plasma (QGP). With an increase of the collision energy of heavy ions, the probability of QGP ignition increases. At the same time, the probability of the formation of a fireball without igniting the QGP also remains not zero
Less
Posted 2 years ago
Mohammad R. Garousi
Mohammad R. Garousi
Institution: Department of Physics, Faculty of Science, Ferdowsi University of Mashhad,
Email: garousi@um.ac.ir
Recently, using the assumption that the string theory effective action at the critical dimension is background independent, the classical on-shell effective action of the bosonic string theory at order α in a spacetime manifold without boundary has been reproduced, up to an overall parameter, by im...
More
Recently, using the assumption that the string theory effective action at the critical dimension is background independent, the classical on-shell effective action of the bosonic string theory at order α in a spacetime manifold without boundary has been reproduced, up to an overall parameter, by imposing the O(1, 1) symmetry when the background has a circle. In the presence of the boundary, we consider a background which has boundary and a circle such that the unit normal vector of the boundary is independent of the circle. Then the O(1, 1) symmetry can fix the bulk action without using the lowest order equation of motion. Moreover, the above constraints and the constraint from the principle of the least action in the presence of boundary can fix the boundary action, up to five boundary parameters. In the least action principle, we assume that not only the values
of the massless fields but also the values of their first derivatives are arbitrary on the boundary. We have also observed
that the cosmological reduction of the leading order action in the presence of the Hawking–Gibbons boundary term, produces zero cosmological boundary action. Imposing this as another constraint on the boundary couplings at order α, we find the boundary action up to two parameters. For a specific value for these two parameters, the gravity couplings in the boundary become the Chern–Simons gravity plus another term which has the Laplacian of the extrinsic curvature.
Less
Posted 2 years ago