By using the generalized fractional analytical iteration method (GF-AEIM), the single, the double, and the triple heavy baryons masses are calculated in the hyper-central model in the two cases. In the first case, the potential is a combination of Coulombic potential, the linear confining potential, and the harmonic oscillator potential. In the second case, we add the hyperfine interaction. The energy eigenvalues and the baryonic wave function are obtained in the fractional forms. The present results are a good agreement with experimental data and are improved with other recent works.
{"title":"Masses of Single, Double, and Triple Heavy Baryons in the Hyper-Central Quark Model by Using GF-AEIM","authors":"M. Abu-shady, H. M. Fath-Allah","doi":"10.1155/2022/4539308","DOIUrl":"https://doi.org/10.1155/2022/4539308","url":null,"abstract":"By using the generalized fractional analytical iteration method (GF-AEIM), the single, the double, and the triple heavy baryons masses are calculated in the hyper-central model in the two cases. In the first case, the potential is a combination of Coulombic potential, the linear confining potential, and the harmonic oscillator potential. In the second case, we add the hyperfine interaction. The energy eigenvalues and the baryonic wave function are obtained in the fractional forms. The present results are a good agreement with experimental data and are improved with other recent works.","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" ","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-06-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49558271","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Transverse momentum, , spectra are of prime importance in order to extract crucial information about the evolution dynamics of the system of particles produced in the collider experiments. In this work, the transverse momentum spectra of charged hadrons produced in collision at TeV have been analyzed using different distribution functions in order to gain strong insight into the information that can be extracted from the spectra. We have also discussed the applicability of the unified statistical framework on the spectra of charged hadron at TeV
{"title":"Model Comparison of the Transverse Momentum Spectra of Charged Hadrons Produced in Collision at TeV","authors":"Rohit Gupta, Satyajit Jena","doi":"10.1155/2022/5482034","DOIUrl":"https://doi.org/10.1155/2022/5482034","url":null,"abstract":"Transverse momentum, <span><svg height=\"10.2124pt\" style=\"vertical-align:-3.42943pt\" version=\"1.1\" viewbox=\"-0.0498162 -6.78297 13.9009 10.2124\" width=\"13.9009pt\" xmlns=\"http://www.w3.org/2000/svg\" xmlns:xlink=\"http://www.w3.org/1999/xlink\"><g transform=\"matrix(.013,0,0,-0.013,0,0)\"></path></g><g transform=\"matrix(.0091,0,0,-0.0091,7.384,3.132)\"></path></g></svg>,</span> spectra are of prime importance in order to extract crucial information about the evolution dynamics of the system of particles produced in the collider experiments. In this work, the transverse momentum spectra of charged hadrons produced in <svg height=\"9.49473pt\" style=\"vertical-align:-0.2063999pt\" version=\"1.1\" viewbox=\"-0.0498162 -9.28833 28.572 9.49473\" width=\"28.572pt\" xmlns=\"http://www.w3.org/2000/svg\" xmlns:xlink=\"http://www.w3.org/1999/xlink\"><g transform=\"matrix(.013,0,0,-0.013,0,0)\"><use xlink:href=\"#g113-81\"></use></g><g transform=\"matrix(.013,0,0,-0.013,8.157,0)\"><use xlink:href=\"#g113-99\"></use></g><g transform=\"matrix(.013,0,0,-0.013,14.127,0)\"><use xlink:href=\"#g113-81\"></use></g><g transform=\"matrix(.013,0,0,-0.013,22.284,0)\"><use xlink:href=\"#g113-99\"></use></g></svg> collision at <svg height=\"8.55521pt\" style=\"vertical-align:-0.2063904pt\" version=\"1.1\" viewbox=\"-0.0498162 -8.34882 21.8649 8.55521\" width=\"21.8649pt\" xmlns=\"http://www.w3.org/2000/svg\" xmlns:xlink=\"http://www.w3.org/1999/xlink\"><g transform=\"matrix(.013,0,0,-0.013,0,0)\"><use xlink:href=\"#g113-54\"></use></g><g transform=\"matrix(.013,0,0,-0.013,6.24,0)\"><use xlink:href=\"#g113-47\"></use></g><g transform=\"matrix(.013,0,0,-0.013,9.204,0)\"><use xlink:href=\"#g113-49\"></use></g><g transform=\"matrix(.013,0,0,-0.013,15.444,0)\"><use xlink:href=\"#g113-51\"></use></g></svg> TeV have been analyzed using different distribution functions in order to gain strong insight into the information that can be extracted from the spectra. We have also discussed the applicability of the unified statistical framework on the spectra of charged hadron at <svg height=\"8.55521pt\" style=\"vertical-align:-0.2063904pt\" version=\"1.1\" viewbox=\"-0.0498162 -8.34882 21.8649 8.55521\" width=\"21.8649pt\" xmlns=\"http://www.w3.org/2000/svg\" xmlns:xlink=\"http://www.w3.org/1999/xlink\"><g transform=\"matrix(.013,0,0,-0.013,0,0)\"><use xlink:href=\"#g113-54\"></use></g><g transform=\"matrix(.013,0,0,-0.013,6.24,0)\"><use xlink:href=\"#g113-47\"></use></g><g transform=\"matrix(.013,0,0,-0.013,9.204,0)\"><use xlink:href=\"#g113-49\"></use></g><g transform=\"matrix(.013,0,0,-0.013,15.444,0)\"><use xlink:href=\"#g113-51\"></use></g></svg> TeV","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" 45","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-06-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138514420","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In this paper, we study the constraint on brane tension and compactification scale for models with brane fluctuations using the results from the direct search of at 13 TeV LHC, with an integrated luminosity of , in the case for which branon forms the entire cold dark matter. The inclusion of these brane fluctuations suppresses the KK-mode couplings to brane localised matter fields. Unlike the rigid brane scenario, where the compactification scale gets constrained to TeV, here we show that compactification scales as small as TeV are allowed for brane tensions of similar strength.
在本文中，利用W′的直接搜索结果，研究了膜波动模型的膜张力和紧致尺度的约束在13 TeV LHC，积分光度为36.1fb-1，在这种情况下，branon形成了整个冷暗物质。这些膜波动的包含抑制了KK模式与膜局域物质场的耦合。与刚性膜场景不同，在刚性膜场景中，紧凑化尺度被限制为1/R>5.2 TeV，这里我们证明了紧致化标度小到~1 对于类似强度的膜张力，允许使用TeV。
{"title":"Relaxing the <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M1\">\u0000 <msup>\u0000 <mrow>\u0000 <mi>W</mi>\u0000 </mrow>\u0000 <mrow>\u0000 <mo>′</mo>\u0000 </mrow>","authors":"Mathew Thomas Arun","doi":"10.1155/2022/8784084","DOIUrl":"https://doi.org/10.1155/2022/8784084","url":null,"abstract":"<jats:p>In this paper, we study the constraint on brane tension and compactification scale for models with brane fluctuations using the results from the direct search of <jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M2\">\u0000 <msup>\u0000 <mrow>\u0000 <mi>W</mi>\u0000 </mrow>\u0000 <mrow>\u0000 <mo>′</mo>\u0000 </mrow>\u0000 </msup>\u0000 </math>\u0000 </jats:inline-formula> at 13 TeV LHC, with an integrated luminosity of <jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M3\">\u0000 <mn>36.1</mn>\u0000 <mi>f</mi>\u0000 <msup>\u0000 <mrow>\u0000 <mi>b</mi>\u0000 </mrow>\u0000 <mrow>\u0000 <mo>−</mo>\u0000 <mn>1</mn>\u0000 </mrow>\u0000 </msup>\u0000 </math>\u0000 </jats:inline-formula>, in the case for which branon forms the entire cold dark matter. The inclusion of these brane fluctuations suppresses the KK-mode couplings to brane localised matter fields. Unlike the rigid brane scenario, where the compactification scale gets constrained to <jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M4\">\u0000 <mfenced open=\"(\" close=\")\">\u0000 <mrow>\u0000 <mn>1</mn>\u0000 <mo>/</mo>\u0000 <mi>R</mi>\u0000 </mrow>\u0000 </mfenced>\u0000 <mo>></mo>\u0000 <mn>5.2</mn>\u0000 </math>\u0000 </jats:inline-formula> TeV, here we show that compactification scales as small as <jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M5\">\u0000 <mo>~</mo>\u0000 <mn>1</mn>\u0000 </math>\u0000 </jats:inline-formula> TeV are allowed for brane tensions of similar strength.</jats:p>","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" ","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49335251","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Erratum to “Superstring Backgrounds in String Geometry”","authors":"Masaki Honda, Matsuo Sato, Taiki Tohshima","doi":"10.1155/2022/9768247","DOIUrl":"https://doi.org/10.1155/2022/9768247","url":null,"abstract":"<jats:p />","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" ","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-05-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"42647911","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In this paper, we have investigated the density perturbations and cosmological evolution in the FLRW universe in the presence of a cosmic magnetic field, which may be assumed to mimic primordial magnetic fields. Such magnetic fields have sufficient strength to influence galaxy formation and cluster dynamics, thereby leaving an imprint on the CMB anisotropies. We have considered the FLRW universe as a representative of the isotropic cosmological model in the 1 + 3 covariant formalism for f R gravity. The propagation equations have been determined and analyzed, where we have assumed that the magnetic field is aligned uniformly along the x -direction, resulting in a diagonal shear tensor. Subsequently, the density perturbation evolution equations have been studied, and the results have been interpreted. We have also indicated how these results change in the general relativistic case and briefly mentioned the expected change in higher-order gravity theories.
{"title":"Density Perturbation and Cosmological Evolution in the Presence of Magnetic Field in <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M1\">\u0000 <mi>f</mi>\u0000 <mfenced open=\"(\" close=\")\">\u0000 <mrow>\u0000 <mi>R</mi>\u0000 ","authors":"S. Chakraborty, S. Guha","doi":"10.1155/2022/5195251","DOIUrl":"https://doi.org/10.1155/2022/5195251","url":null,"abstract":"In this paper, we have investigated the density perturbations and cosmological evolution in the FLRW universe in the presence of a cosmic magnetic field, which may be assumed to mimic primordial magnetic fields. Such magnetic fields have sufficient strength to influence galaxy formation and cluster dynamics, thereby leaving an imprint on the CMB anisotropies. We have considered the FLRW universe as a representative of the isotropic cosmological model in the \u0000 \u0000 1\u0000 +\u0000 3\u0000 \u0000 covariant formalism for \u0000 \u0000 f\u0000 \u0000 \u0000 R\u0000 \u0000 \u0000 \u0000 gravity. The propagation equations have been determined and analyzed, where we have assumed that the magnetic field is aligned uniformly along the \u0000 \u0000 x\u0000 \u0000 -direction, resulting in a diagonal shear tensor. Subsequently, the density perturbation evolution equations have been studied, and the results have been interpreted. We have also indicated how these results change in the general relativistic case and briefly mentioned the expected change in higher-order gravity theories.","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" ","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-05-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"47998277","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In this paper, the couple influence of axial magnetic field and the heat and mass transfer on two rotating cylinders of Walter’s B ′ viscoelastic fluids by using the potential flow theory of viscoelastic fluid has been investigated. The normal mode method is used to compute the growth rate of disturbance. The influence of gravity is ignored at the interface, while the effect of surface tension is present in the analysis. The effect of the parameters on the stability is studied. It is found that the rotation of the inner cylinder induces stability. Furthermore, the viscoelastic ratio of fluids has a stabilizing influence. The heat and mass transfer, magnetic permeability ratio, and Ohnesorge number have a stabilized influence, while viscosity ratio of fluids, density ratio of fluids, and axial magnetic field have destabilizing influence on the considered system.
{"title":"Linear Stability of Magneto Viscoelastic Walter’s <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M1\">\u0000 <msup>\u0000 <mrow>\u0000 <mi>B</mi>\u0000 </mrow>\u0000 <mrow>\u0000 <mo>′","authors":"D. Mostafa","doi":"10.1155/2022/6577512","DOIUrl":"https://doi.org/10.1155/2022/6577512","url":null,"abstract":"In this paper, the couple influence of axial magnetic field and the heat and mass transfer on two rotating cylinders of Walter’s \u0000 \u0000 \u0000 \u0000 B\u0000 \u0000 \u0000 ′\u0000 \u0000 \u0000 \u0000 viscoelastic fluids by using the potential flow theory of viscoelastic fluid has been investigated. The normal mode method is used to compute the growth rate of disturbance. The influence of gravity is ignored at the interface, while the effect of surface tension is present in the analysis. The effect of the parameters on the stability is studied. It is found that the rotation of the inner cylinder induces stability. Furthermore, the viscoelastic ratio of fluids has a stabilizing influence. The heat and mass transfer, magnetic permeability ratio, and Ohnesorge number have a stabilized influence, while viscosity ratio of fluids, density ratio of fluids, and axial magnetic field have destabilizing influence on the considered system.","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" ","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-05-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49263093","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The paper addresses the effects of the variations of the SUSY breaking scale m s in the range (2-14) TeV on the three neutrino masses and mixings, in running the renormalization group equations (RGEs) for different input values of high energy seesaw scale M R , and in both normal and inverted hierarchical neutrino mass models. The present investigation is a continuation of the earlier works based on the variation of m s scale. Two approaches are adopted one after another—bottom-up approach for running gauge and Yukawa couplings from low to high energy scale, followed by the top-down approach from high to low energy scale for running neutrino parameters defined at high energy scale, along with gauge and Yukawa couplings. A self-complementarity relation among three mixing angles is also employed in the analysis and it is found to be stable under radiative correction. Significant effect due to radiative corrections on neutrino parameters with the variation of SUSY breaking scale m s is observed. For comparison of the results, variation of tan β for different M R is also considered.
{"title":"Effects of Variations of SUSY Breaking Scale on Neutrino Parameters at Low Energy Scale under Radiative Corrections","authors":"Kh. Helensana Devi, K. Singh, N. Singh","doi":"10.1155/2022/5780441","DOIUrl":"https://doi.org/10.1155/2022/5780441","url":null,"abstract":"The paper addresses the effects of the variations of the SUSY breaking scale \u0000 \u0000 \u0000 \u0000 m\u0000 \u0000 \u0000 s\u0000 \u0000 \u0000 \u0000 in the range (2-14) TeV on the three neutrino masses and mixings, in running the renormalization group equations (RGEs) for different input values of high energy seesaw scale \u0000 \u0000 \u0000 \u0000 M\u0000 \u0000 \u0000 R\u0000 \u0000 \u0000 \u0000 , and in both normal and inverted hierarchical neutrino mass models. The present investigation is a continuation of the earlier works based on the variation of \u0000 \u0000 \u0000 \u0000 m\u0000 \u0000 \u0000 s\u0000 \u0000 \u0000 \u0000 scale. Two approaches are adopted one after another—bottom-up approach for running gauge and Yukawa couplings from low to high energy scale, followed by the top-down approach from high to low energy scale for running neutrino parameters defined at high energy scale, along with gauge and Yukawa couplings. A self-complementarity relation among three mixing angles is also employed in the analysis and it is found to be stable under radiative correction. Significant effect due to radiative corrections on neutrino parameters with the variation of SUSY breaking scale \u0000 \u0000 \u0000 \u0000 m\u0000 \u0000 \u0000 s\u0000 \u0000 \u0000 \u0000 is observed. For comparison of the results, variation of \u0000 \u0000 tan\u0000 β\u0000 \u0000 for different \u0000 \u0000 \u0000 \u0000 M\u0000 \u0000 \u0000 R\u0000 \u0000 \u0000 \u0000 is also considered.","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" ","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49248902","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In order to investigate the speed of gravitational signals travelling in air or through a different medium two experiments were designed. One of the experiments contains 2 masses rotating at very high speed and in the other experiment a sapphire bar will vibrate, in both cases they will emit a periodic tidal gravitational signal and one sapphire device that behaves as a detector, which are suspended in vacuum and cooled down to 4.2 K will act as a detector. The vibrational amplitude of the sapphire detector device is measured by an microwave signal with ultralow phase-noise that uses resonance in the whispering gallery modes inside the detector device. Sapphire has a quite high mechanical Q and electrical Q which implies a very narrow detection band thus reducing the detection sensitivity. A new detector shape for the detector device is presented in this work, yielding a detection band of about half of the device vibrational frequency. With the aid of a Finite Element Program the normal mode frequencies of the detector can be calculated with high precision. The results show a similar expected sensitivity between the two experimental setup, but the experiment with the vibration masses is more stable in frequency then it is chosen for the experimental setup to measure the speed of gravity in short distances. Then a more precise analysis is made with this experiment reaching a signal-noise ratio of 10 at a frequency of 5000 Hz.
{"title":"The Analysis of a Proposed Experiment to Measure the Speed of Gravity in Short Distances","authors":"C. Frajuca, Fabio da Silva Bortoli, N. Magalhaes","doi":"10.1155/2022/1991119","DOIUrl":"https://doi.org/10.1155/2022/1991119","url":null,"abstract":"In order to investigate the speed of gravitational signals travelling in air or through a different medium two experiments were designed. One of the experiments contains 2 masses rotating at very high speed and in the other experiment a sapphire bar will vibrate, in both cases they will emit a periodic tidal gravitational signal and one sapphire device that behaves as a detector, which are suspended in vacuum and cooled down to 4.2 K will act as a detector. The vibrational amplitude of the sapphire detector device is measured by an microwave signal with ultralow phase-noise that uses resonance in the whispering gallery modes inside the detector device. Sapphire has a quite high mechanical Q and electrical Q which implies a very narrow detection band thus reducing the detection sensitivity. A new detector shape for the detector device is presented in this work, yielding a detection band of about half of the device vibrational frequency. With the aid of a Finite Element Program the normal mode frequencies of the detector can be calculated with high precision. The results show a similar expected sensitivity between the two experimental setup, but the experiment with the vibration masses is more stable in frequency then it is chosen for the experimental setup to measure the speed of gravity in short distances. Then a more precise analysis is made with this experiment reaching a signal-noise ratio of 10 at a frequency of 5000 Hz.","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" ","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-04-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"47406887","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
A difference in electric potential in a static conductor inside a static magnetic field and an anisotropic and asymmetric distribution of neutrons emitted in nuclear reactions induced by ultrasound are assumed as marks of local Lorentz invariance (LLI) violation. The asymmetry of the two experiments is related to the asymmetry of the Cosmic Microwave Background Radiation (CMBR). As common directions of asymmetry are found in these three cases, a fundamental asymmetry of the interactions is suggested which can also shed new light on the question of symmetry breaking in the history of the Universe.
{"title":"The Asymmetry of the Cosmic Microwave Background Radiation as Signature of Local Lorentz Invariance Violation","authors":"G. Albertini, F. Cardone, S. Bellucci","doi":"10.1155/2022/6271119","DOIUrl":"https://doi.org/10.1155/2022/6271119","url":null,"abstract":"A difference in electric potential in a static conductor inside a static magnetic field and an anisotropic and asymmetric distribution of neutrons emitted in nuclear reactions induced by ultrasound are assumed as marks of local Lorentz invariance (LLI) violation. The asymmetry of the two experiments is related to the asymmetry of the Cosmic Microwave Background Radiation (CMBR). As common directions of asymmetry are found in these three cases, a fundamental asymmetry of the interactions is suggested which can also shed new light on the question of symmetry breaking in the history of the Universe.","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" ","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-04-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"45551494","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Yang Zhang, Yu-bo Ma, Yun-zhi Du, Huai-fan Li, Li-chun Zhang
In this paper, thermodynamic properties of the Reissner-Nordström-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.
{"title":"Phase Transition and Entropic Force in Reissner-Nordström-de Sitter Spacetime","authors":"Yang Zhang, Yu-bo Ma, Yun-zhi Du, Huai-fan Li, Li-chun Zhang","doi":"10.1155/2022/7376502","DOIUrl":"https://doi.org/10.1155/2022/7376502","url":null,"abstract":"In this paper, thermodynamic properties of the Reissner-Nordström-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.","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" ","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-04-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"48710590","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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