ADVANCES IN HIGH ENERGY PHYSICS 发表了关于能量和物质的性质及其相互作用的理论和实验研究结果。考虑到原创研究和重点评论文章，该期刊欢迎小型研究小组和大型财团的投稿。

The journal "Advances in High Energy Physics" publishes theoretical and experimental research results on the properties of energy and matter and their interactions. It welcomes submissions of original research and focused review articles from both small research groups and large institutions.

《Advances in High Energy Physics》期刊发表关于能量和物质性质及其相互作用的理论和实验研究成果。该期刊欢迎小型研究团队和大型研究机构的原创研究和重点评论文章的投稿。

Advances in High Energy Physics

Microscaled devices receive great attention in microreactor systems for producing high renewable energy due to higher surface-to-volume, higher transport rates (heat or/and mass transfer rates), and other advantages over conventional-size reactors. In this paper, the two-phase liquid-liquid flow in a microchannel with various Y-shaped junctions has been studied numerically. Two kinds of immiscible liquids were injected into a microchannel from the Y-shaped junctions to generate the segment flow mode. The segment length was studied. The volume of fluid (VOF) method was used to track the liquid-liquid interface and the piecewise-liner interface construction (PLIC) technique was adopted to get a sharp interface. The interfacial tension was simulated with continuum surface force (CSF) model and the wall adhesion boundary condition was taken into consideration. The simulated flow pattern presents consistence with our experimental one. The numerical results show that a segmented flow mode appears in the main channel. Under the same inlet velocities of two liquids, the segment lengths of the two liquids are the same and depend on the inclined angles of two lateral channels. The effect of inlet velocity is studied in a typical T-shaped microchannel. It is found that the ratio between the lengths of two liquids is almost equal to the ratio between their inlet velocities.

Xian Wang

Hiroyuki Hirano

Gongnan Xie

Ding Xu

VOF Modeling and Analysis of the Segmented Flow in Y-Shaped Microchannels for Microreactor Systems

微反应器系统中Y形微通道分段流动的VOF建模与分析

This work presents the application of the q ‐algebra in the glueball spectrum. This algebra is implemented through Jackson’s derivatives in a Schrödinger‐like equation resulting from the gravity fluctuations around the braneworld scenario in five dimensions. In our prescription, we consider a four‐dimensional AdS 4 brane, living in AdS 5 bulk, that is also known for describing locally localized gravity via quasizero mode. At the appropriate limit, this background leads to confinement and allows us to find the shape of the q ‐deformed glueball spectrum in the AdS 5 /QCD 4 correspondence. The introduction of the q ‐deformation provides us with a richer glueball spectrum.

Fabiano F. Santos

F. A. Brito

<i>q</i>‐Deformed Glueball Spectrum in AdS/QCD Correspondence

AdS/QCD对应中的<i>q</i>变形胶球谱

Relativistic charged particle beam can be used as a destructive beam weapon in space for debris removal tasks. The trajectories of charged particles are affected by both electric and magnetic forces in the Earth’s magnetic field. In this paper, we firstly analyzed the correlation parameters of the charged particle beam as a weapon when it is propagated in the geomagnetic field. Then, the models were constructed based on COMSOL Multiphysics, and the IGRF model was adopted in the simulation. The gyroradius and the related uncertainty were analyzed by simulation of the charged particle transport in the geomagnetic field at different altitudes. The charged beam spot radius divergency was also simulated. The geomagnetic field can inhibite the diffusion of the electron beam.

Meihua Fang

Zheng Liang

Yingkui Gong

Jianfei Chen

Guiping Zhu

Ting Liu

Yu Tian

Yu Zhou

Study of the Gyro and Divergence Characteristics of Relativistic Charged Particle Beam Propagation in Earth’s Magnetic Field

相对论带电粒子束在地球磁场中传播的陀螺和发散特性研究

In this paper, thermodynamic properties of the Reissner-Nordstr\"om-de Sitter (RN-dS) black hole have been studied on the basis of the correlation between the black hole and cosmological horizons. It is found that the RN-dS black hole experiences a phase transition, when its state parameters satisfy certain conditions. From the analysis of the interaction between two horizons in RN-dS spacetime, we get the numerical solution of the interaction between two horizons. It makes us to realize the force between the black hole and cosmological horizons, which can be regarded as a candidate to explain our accelerating expansion universe. That provides a new window to explore the physical mechanism of the cosmic accelerating expansion.

Yang Zhang

Yu-bo Ma

Yun-zhi Du

Huai-fan Li

Li-chun Zhang

Phase Transition and Entropic Force in Reissner-Nordström-de Sitter Spacetime

Reissner-Nordström-de Sitter时空中的相变与熵力

We propose the generalized uncertainty principle (GUP) with an additional term of quadratic momentum motivated by string theory and black hole physics as a quantum mechanical framework for the minimal length uncertainty at the Planck scale. We demonstrate that the GUP parameter, $\beta_0$, could be best constrained by the the gravitational waves observations; GW170817 event. Also, we suggest another proposal based on the modified dispersion relations (MDRs) in order to calculate the difference between the group velocity of gravitons and that of photons. We conclude that the upper bound reads $\beta_0 \simeq 10^{60}$. Utilizing features of the UV/IR correspondence and the obvious similarities between GUP (including non-gravitating and gravitating impacts on Heisenberg uncertainty principle) and the discrepancy between the theoretical and the observed cosmological constant $\Lambda$ (apparently manifesting gravitational influences on the vacuum energy density), known as {\it catastrophe of non-gravitating vacuum}, we suggest a possible solution for this long-standing physical problem, $\Lambda \simeq 10^{-47}~$GeV$^4/\hbar^3 c^3$.

Abdel Magied Diab

Abdel Nasser Tawfik

A Possible Solution of the Cosmological Constant Problem Based on GW170817 and Planck Observations with Minimal Length Uncertainty

基于GW170817和普朗克观测的宇宙常数问题可能解决方案：最小长度不确定性

The neutrino mass hierarchy determination ( <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" id="M2"><a:mi>ν</a:mi></a:math> MHD) is one of the main goals of the major current and future neutrino experiments. The statistical analysis usually proceeds from a standard method, a single-dimensional estimator <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" id="M3"><c:mfenced open="(" close=")"><c:mrow><c:mn>1</c:mn><c:mtext>D</c:mtext><c:mo>−</c:mo><c:mi>Δ</c:mi><c:msup><c:mrow><c:mi>χ</c:mi></c:mrow><c:mrow><c:mn>2</c:mn></c:mrow></c:msup></c:mrow></c:mfenced></c:math> that shows some drawbacks and concerns, together with a debatable strategy. The drawbacks and considerations of the standard method will be explained through the following three main issues. The first issue corresponds to the limited power of the standard method. The <g:math xmlns:g="http://www.w3.org/1998/Math/MathML" id="M4"><g:mi>Δ</g:mi><g:msup><g:mrow><g:mi>χ</g:mi></g:mrow><g:mrow><g:mn>2</g:mn></g:mrow></g:msup></g:math> estimator provides us with different results when different simulation procedures were used. Regarding the second issue, when <i:math xmlns:i="http://www.w3.org/1998/Math/MathML" id="M5"><i:msubsup><i:mrow><i:mi>χ</i:mi></i:mrow><i:mrow><i:mi mathvariant="normal">min</i:mi><i:mfenced open="(" close=")"><i:mrow><i:mtext>NH</i:mtext></i:mrow></i:mfenced></i:mrow><i:mrow><i:mn>2</i:mn></i:mrow></i:msubsup></i:math> and <n:math xmlns:n="http://www.w3.org/1998/Math/MathML" id="M6"><n:msubsup><n:mrow><n:mi>χ</n:mi></n:mrow><n:mrow><n:mi mathvariant="normal">min</n:mi><n:mfenced open="(" close=")"><n:mrow><n:mtext>IH</n:mtext></n:mrow></n:mfenced></n:mrow><n:mrow><n:mn>2</n:mn></n:mrow></n:msubsup></n:math> are drawn in a 2D map, their strong positive correlation manifests <s:math xmlns:s="http://www.w3.org/1998/Math/MathML" id="M7"><s:msup><s:mrow><s:mi>χ</s:mi></s:mrow><s:mrow><s:mn>2</s:mn></s:mrow></s:msup></s:math> as a bidimensional variable, instead of a single-dimensional estimator. The overlapping between the <u:math xmlns:u="http://www.w3.org/1998/Math/MathML" id="M8"><u:msup><u:mrow><u:mi>χ</u:mi></u:mrow><u:mrow><u:mn>2</u:mn></u:mrow></u:msup></u:math> distributions of the two hypotheses leads to an experiment sensitivity reduction. The third issue corresponds to the robustness of the standard method. When the JUNO sensitivity is obtained using different procedures, either with <w:math xmlns:w="http://www.w3.org/1998/Math/MathML" id="M9"><w:mi>Δ</w:mi><w:msup><w:mrow><w:mi>χ</w:mi></w:mrow><w:mrow><w:mn>2</w:mn></w:mrow></w:msup></w:math> as one-dimensional or <y:math xmlns:y="http://www.w3.org/1998/Math/MathML" id="M10"><y:msup><y:mrow><y:mi>χ</y:mi></y:mrow><y:mrow><y:mn>2</y:mn></y:mrow></y:msup></y:math> as two-dimensional estimator, the experimental sensitivity varies with the different values of the atmospheric mass, the input parameter. We computed the oscillation of <ab:math xmlns:ab="http://www.w3.org/1998/Math/MathML" id="M11"><ab:mfenced open="|" close="|"><ab:mrow><ab:mover accent="false"><ab:mrow><ab:mi>Δ</ab:mi><ab:msup><ab:mrow><ab:mi>χ</ab:mi></ab:mrow><ab:mrow><ab:mn>2</ab:mn></ab:mrow></ab:msup></ab:mrow><ab:mrow><ab:mo>¯</ab:mo></ab:mrow></ab:mover></ab:mrow></ab:mfenced></ab:math> with the input parameter values, <fb:math xmlns:fb="http://www.w3.org/1998/Math/MathML" id="M12"><fb:msub><fb:mrow><fb:mfenced open="|" close="|"><fb:mrow><fb:mi>Δ</fb:mi><fb:msup><fb:mrow><fb:mi>m</fb:mi></fb:mrow><fb:mrow><fb:mn>2</fb:mn></fb:mrow></fb:msup></fb:mrow></fb:mfenced></fb:mrow><fb:mrow><fb:mtext>input</fb:mtext></fb:mrow></fb:msub></fb:math> . The MH significance using the standard method, <jb:math xmlns:jb="http://www.w3.org/1998/Math/MathML" id="M13"><jb:mi>Δ</jb:mi><jb:msup><jb:mrow><jb:mi>χ</jb:mi></jb:mrow><jb:mrow><jb:mn>2</jb:mn></jb:mrow></jb:msup></jb:math> , strongly depends on the values of the parameter <lb:math xmlns:lb="http://www.w3.org/1998/Math/MathML" id="M14"><lb:msub><lb:mrow><lb:mfenced open="|" close="|"><lb:mrow><lb:mi>Δ</lb:mi><lb:msup><lb:mrow><lb:mi>m</lb:mi></lb:mrow><lb:mrow><lb:mn>2</lb:mn></lb:mrow></lb:msup></lb:mrow></lb:mfenced></lb:mrow><lb:mrow><lb:mtext>input</lb:mtext></lb:mrow></lb:msub></lb:math> . Consequently, the experiment sensitivity depends on the precision of the atmospheric mass. This evaluation of the standard method confirms the drawbacks.

F. Sawy

L. Stanco

Statistical Issues on the Neutrino Mass Hierarchy with <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" id="M1"><a:mi>Δ</a:mi><a:msup><a:mrow><a:mi>χ</a:mi></a:mrow><a:mrow><a:mn>2</a:mn></a:mrow></a:msup></a:math>

关于中微子质量层次的统计问题与Δχ²

In this paper, we solve the bound state problem for the Varshni-Hellmann potential via a useful technique. In our technique, we obtain the bound state solution of the Schrödinger equation for the Varshni-Hellmann potential via ansatz method. We obtain the energy eigenvalues and the corresponding eigenfunctions. Also, the behavior of the energy spectra for both the ground and the excited state of the two body systems is illustrated graphically. The similarity of our results to the accurate numerical values is indicative of the efficiency of our technique.

N. Tazimi

Determination of the Energy Eigenvalues of the Varshni-Hellmann Potential

Varshni-Hellmann势能本征值的确定

The measurements of the total cross section of the <math xmlns="http://www.w3.org/1998/Math/MathML" id="M2"><msup><mrow><mi>e</mi></mrow><mrow><mo>+</mo></mrow></msup><msup><mrow><mi>e</mi></mrow><mrow><mo>−</mo></mrow></msup><mo>⟶</mo><mi>γ</mi><mi>γ</mi><mfenced open="(" close=")"><mrow><mi>γ</mi></mrow></mfenced></math> reaction from the VENUS, TOPAS, OPAL, DELPHI, ALEPH, and L3 collaborations, collected between 1989 and 2003, are used to perform a <math xmlns="http://www.w3.org/1998/Math/MathML" id="M3"><msup><mrow><mi>χ</mi></mrow><mrow><mn>2</mn></mrow></msup></math> test to validate the current quantum electrodynamics (QED) theory and search for possible deviations with the direct contact term annihilation. By observing a deviation from the QED predictions on the total cross section of the <math xmlns="http://www.w3.org/1998/Math/MathML" id="M4"><msup><mrow><mi>e</mi></mrow><mrow><mo>+</mo></mrow></msup><msup><mrow><mi>e</mi></mrow><mrow><mo>−</mo></mrow></msup><mo>⟶</mo><mi>γ</mi><mi>γ</mi><mfenced open="(" close=")"><mrow><mi>γ</mi></mrow></mfenced></math> reaction above <math xmlns="http://www.w3.org/1998/Math/MathML" id="M5"><msqrt><mrow><mi>s</mi></mrow></msqrt><mo>=</mo><mn>180.0</mn></math> GeV, a non-QED direct contact term is introduced following the dimension 6 effective theory to explain the deviation. In the non-QED direct contact term, a threshold energy scale <math xmlns="http://www.w3.org/1998/Math/MathML" id="M6"><mi>Λ</mi></math> is included and explained to the finite interaction length in direct contact term and in consequence the size of the electron involved in the annihilation area. The experimental data of the total cross section is compared to the QED cross section by a <math xmlns="http://www.w3.org/1998/Math/MathML" id="M7"><msup><mrow><mi>χ</mi></mrow><mrow><mn>2</mn></mrow></msup></math> test, which gives a best fit of the <math xmlns="http://www.w3.org/1998/Math/MathML" id="M8"><mi>Λ</mi></math> to be <math xmlns="http://www.w3.org/1998/Math/MathML" id="M9"><mn>1576</mn><mo>±</mo><mn>202</mn></math> GeV, corresponding to a finite interaction length of <math xmlns="http://www.w3.org/1998/Math/MathML" id="M10"><msub><mrow><mi>r</mi></mrow><mrow><mi>e</mi></mrow></msub><mo>=</mo><mfenced open="(" close=")"><mrow><mn>1.25</mn><mo>±</mo><mn>0.16</mn></mrow></mfenced><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>17</mn></mrow></msup></math> (cm). In the direct contact term annihilation, this interaction length is a measure of the size of an electron <math xmlns="http://www.w3.org/1998/Math/MathML" id="M11"><msub><mrow><mi>r</mi></mrow><mrow><mi>e</mi></mrow></msub></math> . By combining all the data results from the mentioned collaborations, we have at least 2 to 3 times more statistics than every single experiment at high <math xmlns="http://www.w3.org/1998/Math/MathML" id="M12"><msqrt><mrow><mi>s</mi></mrow></msqrt></math> region. This induces the best precision on <math xmlns="http://www.w3.org/1998/Math/MathML" id="M13"><msub><mrow><mi>r</mi></mrow><mrow><mi>e</mi></mrow></msub></math> compared to the previous measurements.

Yutao Chen

Minghui Liu

Jürgen Ulbricht

Hint for a Minimal Interaction Length in <math xmlns="http://www.w3.org/1998/Math/MathML" id="M1"><msup><mrow><mi>e</mi></mrow><mrow><mo>+</mo></mrow></msup><msup><mrow><mi>e</mi></mrow><mrow><mo>−</mo></mrow></msup><mo>⟶</mo><mi>γ</mi><mi>γ</mi></math> Annihilation in Total Cross Section of Center-of-Mass Energies 55-207 GeV

<math xmlns="http://www.w3.org/1998/Math/MathML" id="M1"><msup><mrow><mi>e</mi></mrow><mrow><mo>+</mo></mrow></msup><msup><mrow><mi>e</mi></mrow><mrow><mo>−</mo></mrow></msup><mo>⟶</mo><mi>γ</mi><mi>γ</mi></math> 湮灭中总截面在质心能量55-207 GeV的最小相互作用长度提示

The analytical exact iteration method (AEIM) has been widely used to calculate <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" id="M4"><a:mi>N</a:mi></a:math> -dimensional radial Schrodinger equation with medium-modified form of Cornell potential and is generalized to the finite value of magnetic field (eB) with quasiparticle approach in hot quantum chromodynamics (QCD) medium. In <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" id="M5"><c:mi>N</c:mi></c:math> -dimensional space, the energy eigenvalues have been calculated for any states ( <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" id="M6"><e:mi>n</e:mi></e:math> , <g:math xmlns:g="http://www.w3.org/1998/Math/MathML" id="M7"><g:mi>l</g:mi></g:math> ). These results have been used to study the properties of quarkonium states (i.e, the binding energy and mass spectra, dissociation temperature, and thermodynamical properties in the <i:math xmlns:i="http://www.w3.org/1998/Math/MathML" id="M8"><i:mi>N</i:mi></i:math> -dimensional space). We have determined the binding energy of the ground states of quarkonium with magnetic field and dimensionality number. We have also determined the effects of magnetic field and dimensionality number on mass spectra for ground states of quarkonia. But the main result is quite noticeable for the values of dissociation temperature in terms of magnetic field and dimensionality number for ground states of quarkonia after using the criteria of dissociation energy. At last, we have also calculated the thermodynamical properties of QGP (i.e., pressure, energy density, and speed of sound) using the parameter eB with ideal equation of states (EoS). A preprint has previously been published (Solanki et al., 2023).

Siddhartha Solanki

Manohar Lal

Vineet Kumar Agotiya

Dissociation of <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" id="M1"><a:mi>J</a:mi><a:mo>/</a:mo><a:mi>ψ</a:mi></a:math> and <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" id="M2"><c:mi>Y</c:mi></c:math> Using Dissociation Energy Criteria in <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" id="M3"><e:mi>N</e:mi></e:math>-Dimensional Space

使用N维空间中的解离能标准解离J/ψ和Y

The paper is devoted to the study of cosmological models with time-varying cosmological term ( <math xmlns="http://www.w3.org/1998/Math/MathML" id="M2"><mi>Λ</mi></math> ) in the presence of creation field in the framework of Bianchi type III space-time. To obtain deterministic model of the universe, we have assumed <math xmlns="http://www.w3.org/1998/Math/MathML" id="M3"><mi>Λ</mi><mo>∝</mo><mn>1</mn><mo>/</mo><msup><mrow><mi>R</mi></mrow><mrow><mn>3</mn></mrow></msup></math> , where <math xmlns="http://www.w3.org/1998/Math/MathML" id="M4"><mi>R</mi></math> is the scale factor, for steady state cosmology and creation field, and shear ( <math xmlns="http://www.w3.org/1998/Math/MathML" id="M5"><mi>σ</mi></math> ) is proportion to expansion ( <math xmlns="http://www.w3.org/1998/Math/MathML" id="M6"><mi>θ</mi></math> ) which leads to <math xmlns="http://www.w3.org/1998/Math/MathML" id="M7"><mi>B</mi><mo>=</mo><msup><mrow><mi>C</mi></mrow><mrow><mi>n</mi></mrow></msup></math> , where <math xmlns="http://www.w3.org/1998/Math/MathML" id="M8"><mi>B</mi></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" id="M9"><mi>C</mi></math> are the metric potentials to explain small anisotropic behaviour of the universe and its isotropy. To obtain the results in terms of cosmic time <math xmlns="http://www.w3.org/1998/Math/MathML" id="M10"><mi>t</mi></math> , we have assumed <math xmlns="http://www.w3.org/1998/Math/MathML" id="M11"><mi>n</mi><mo>=</mo><mn>2</mn></math> . The model satisfies conservation equations, and creation field increases with time. The present model is free from singularity, has particle horizon, and provides a natural explanation for inflationary scenario and isotropization. Creation field and Einstein field equations are derived using principle of least action and Lagrangian formulation of variable cosmological term. For illustrative purposes, evolutionary behaviour of some cosmological parameters are shown graphically. The other physical aspects like accelerating behaviour of the model are also discussed. Thus, the model represents not only expanding universe but also accelerating which matches with the results of present-day observations.

Raj Bali

Seema Saraf

Creation Field Cosmological Model with Variable Cosmological Term (<math xmlns="http://www.w3.org/1998/Math/MathML" id="M1"><mi>Λ</mi></math>) in Bianchi Type III Space-Time

Bianchi III时空中的变宇宙项（<math xmlns="http://www.w3.org/1998/Math/MathML" id="M1"><mi>Λ</mi></math>）创生场宇宙模型

短名	Adv. High Energy Phys.
Journal Impact	1.69
国际分区	PHYSICS, PARTICLES & FIELDS(Q3)
期刊索引	SCI Q3中科院 4 区

ISSN	1687-7357, 1687-7365
h-index	47
国内分区	物理与天体物理(4区)物理与天体物理物理粒子与场物理(4区)

涉及主题	物理量子力学数学粒子物理学核物理学计算机科学数学物理天文几何学工程类天体物理学经典力学理论物理学热力学
出版信息	出版商: Hindawi Publishing Corporation，出版周期: ，期刊类型: journal，开源期刊: 是
基本数据	创刊年份: 2010，原创研究文献占比: 90.91%，自引率:6.70%， Gold OA占比: 100.00%
期刊费用	$1550详情
平均审稿周期	网友分享经验：较慢,6-12周

Advances in High Energy Physics

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VOF Modeling and Analysis of the Segmented Flow in Y-Shaped Microchannels for Microreactor Systems

q‐Deformed Glueball Spectrum in AdS/QCD Correspondence

Study of the Gyro and Divergence Characteristics of Relativistic Charged Particle Beam Propagation in Earth’s Magnetic Field

Phase Transition and Entropic Force in Reissner-Nordström-de Sitter Spacetime

A Possible Solution of the Cosmological Constant Problem Based on GW170817 and Planck Observations with Minimal Length Uncertainty

Statistical Issues on the Neutrino Mass Hierarchy with Δχ2

Determination of the Energy Eigenvalues of the Varshni-Hellmann Potential

Hint for a Minimal Interaction Length in $e^{+} e^{-} ⟶ γ γ$ Annihilation in Total Cross Section of Center-of-Mass Energies 55-207 GeV

Dissociation of J/ψ and Y Using Dissociation Energy Criteria in N-Dimensional Space

Creation Field Cosmological Model with Variable Cosmological Term ( $Λ$ ) in Bianchi Type III Space-Time

Advances in High Energy Physics

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VOF Modeling and Analysis of the Segmented Flow in Y-Shaped Microchannels for Microreactor Systems

q‐Deformed Glueball Spectrum in AdS/QCD Correspondence

Study of the Gyro and Divergence Characteristics of Relativistic Charged Particle Beam Propagation in Earth’s Magnetic Field

Phase Transition and Entropic Force in Reissner-Nordström-de Sitter Spacetime

A Possible Solution of the Cosmological Constant Problem Based on GW170817 and Planck Observations with Minimal Length Uncertainty

Statistical Issues on the Neutrino Mass Hierarchy with Δχ2

Determination of the Energy Eigenvalues of the Varshni-Hellmann Potential

Hint for a Minimal Interaction Length in e+e−⟶γγ Annihilation in Total Cross Section of Center-of-Mass Energies 55-207 GeV

Dissociation of J/ψ and Y Using Dissociation Energy Criteria in N-Dimensional Space

Creation Field Cosmological Model with Variable Cosmological Term (Λ) in Bianchi Type III Space-Time

Hint for a Minimal Interaction Length in $e^{+} e^{-} ⟶ γ γ$ Annihilation in Total Cross Section of Center-of-Mass Energies 55-207 GeV

Creation Field Cosmological Model with Variable Cosmological Term ( $Λ$ ) in Bianchi Type III Space-Time