A Bose-Einstein Condensate (BEC) of a nonzero momentum Cooper pair constitutes a composite boson or simply a boson. Previously, it has been shown that the quantum coherence of the two-component BEC (boson and fermion condensates) is controlled by plasmons where < 1 % of plasmon energy mediates the charge pairing but most of the plasmon energy is used to overcome the modes that compete against superconductivity such as phonons, charge density waves, antiferromagnetism, and damping effects. The dependence of plasmon frequency on the material of a superconductor reveals that modes within a specific range of frequency enhance superconductivity and therefore affect the critical temperature of a particular superconducting material. Against this background, we study the effect on doping on boson-fermion pairing energy and hence the critical temperature. While most hole doping agents are atoms lighter than copper, many of the electron doping agents are materials heavier than copper. This property defines the doping effect on the plasma frequency. Heavier dopants lower the critical temperature while lighter dopants increase the critical temperature of a superconductor. The number density of electrons is also found to be proportional to the square of critical temperature T c while the size of a boson-fermion pair condensate (BFPC) is proportional to T c − 2 / 3 . The size of a BFPC particle is less than boson-fermion (BF) coherence length by almost an order.
{"title":"Electron Number Density and Coherence Length of Boson-Fermion Pair in HTSC","authors":"A. Mukubwa","doi":"10.1155/2022/8198401","DOIUrl":"https://doi.org/10.1155/2022/8198401","url":null,"abstract":"A Bose-Einstein Condensate (BEC) of a nonzero momentum Cooper pair constitutes a composite boson or simply a boson. Previously, it has been shown that the quantum coherence of the two-component BEC (boson and fermion condensates) is controlled by plasmons where \u0000 \u0000 <\u0000 1\u0000 %\u0000 \u0000 of plasmon energy mediates the charge pairing but most of the plasmon energy is used to overcome the modes that compete against superconductivity such as phonons, charge density waves, antiferromagnetism, and damping effects. The dependence of plasmon frequency on the material of a superconductor reveals that modes within a specific range of frequency enhance superconductivity and therefore affect the critical temperature of a particular superconducting material. Against this background, we study the effect on doping on boson-fermion pairing energy and hence the critical temperature. While most hole doping agents are atoms lighter than copper, many of the electron doping agents are materials heavier than copper. This property defines the doping effect on the plasma frequency. Heavier dopants lower the critical temperature while lighter dopants increase the critical temperature of a superconductor. The number density of electrons is also found to be proportional to the square of critical temperature \u0000 \u0000 \u0000 \u0000 \u0000 \u0000 T\u0000 \u0000 \u0000 c\u0000 \u0000 \u0000 \u0000 \u0000 \u0000 while the size of a boson-fermion pair condensate (BFPC) is proportional to \u0000 \u0000 \u0000 \u0000 T\u0000 \u0000 \u0000 c\u0000 \u0000 \u0000 −\u0000 2\u0000 /\u0000 3\u0000 \u0000 \u0000 \u0000 . The size of a BFPC particle is less than boson-fermion (BF) coherence length by almost an order.","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" ","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-03-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"48147899","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}
By adding a three-dimensional manifold to an eleven-dimensional manifold in supergravity, we obtain the action of -gravity and find that it is anomaly-free. We calculate the scale factor of the inflationary universe in this model and observe that it is related to the slow-roll parameters. The tensor-scalar ratio is in good agreement with experimental data.
{"title":"Inflationary Universe from Anomaly-Free <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 </mrow>\u0000 ","authors":"A. Beesham, K. Bamba","doi":"10.1155/2022/9056096","DOIUrl":"https://doi.org/10.1155/2022/9056096","url":null,"abstract":"<jats:p>By adding a three-dimensional manifold to an eleven-dimensional manifold in supergravity, we obtain the action of <jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M2\">\u0000 <mi>F</mi>\u0000 <mfenced open=\"(\" close=\")\">\u0000 <mrow>\u0000 <mi>R</mi>\u0000 </mrow>\u0000 </mfenced>\u0000 </math>\u0000 </jats:inline-formula>-gravity and find that it is anomaly-free. We calculate the scale factor of the inflationary universe in this model and observe that it is related to the slow-roll parameters. The tensor-scalar ratio <jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M3\">\u0000 <mfenced open=\"(\" close=\")\">\u0000 <mrow>\u0000 <msub>\u0000 <mrow>\u0000 <mi>R</mi>\u0000 </mrow>\u0000 <mrow>\u0000 <mtext>tensor</mtext>\u0000 <mo>−</mo>\u0000 <mtext>scalar</mtext>\u0000 </mrow>\u0000 </msub>\u0000 </mrow>\u0000 </mfenced>\u0000 </math>\u0000 </jats:inline-formula> is in good agreement with experimental data.</jats:p>","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" ","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-03-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49323080","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}
<jats:p>We review the two- and three-body baryonic <jats:inline-formula> <math xmlns="http://www.w3.org/1998/Math/MathML" id="M2"> <mi>B</mi> </math> </jats:inline-formula> decays with the dibaryon (<jats:inline-formula> <math xmlns="http://www.w3.org/1998/Math/MathML" id="M3"> <mi mathvariant="bold">B</mi> <mover accent="true"> <mrow> <mi mathvariant="bold">B</mi> <mo>′</mo> </mrow> <mo stretchy="true">¯</mo> </mover> </math> </jats:inline-formula>) as the final states. Accordingly, we summarize the experimental data of the branching fractions, angular asymmetries, and <jats:inline-formula> <math xmlns="http://www.w3.org/1998/Math/MathML" id="M4"> <mtext>CP</mtext> </math> </jats:inline-formula> asymmetries. Using the <jats:inline-formula> <math xmlns="http://www.w3.org/1998/Math/MathML" id="M5"> <mi>W</mi> </math> </jats:inline-formula>-boson annihilation (exchange) mechanism, the branching fractions of <jats:inline-formula> <math xmlns="http://www.w3.org/1998/Math/MathML" id="M6"> <mi>B</mi> <mo>⟶</mo> <mi mathvariant="bold">B</mi> <mover accent="true"> <mrow> <mi mathvariant="bold">B</mi> <mo>′</mo> </mrow> <mo stretchy="true">¯</mo> </mover> </math> </jats:inline-formula> are shown to be interpretable. In the approach of perturbative QCD counting rules, we study the three-body decay channels. In particular, we review the <jats:inline-formula> <math xmlns="http://www.w3.org/1998/Math/MathML" id="M7"> <mtext>CP</mtext> </math> </jats:inline-formula> asymmetries of <jats:inline-formula> <math xmlns="http://www.w3.org/1998/Math/MathML" id="M8"> <mi>B</mi> <mo>⟶</mo> <mi mathvariant="bold">B</mi> <mover accent="true"> <mrow> <mi mathvariant="bold">B</mi> <mo>′</mo> </mrow> <mo stretchy="true">¯</mo> </mover> <mi>M</mi>
我们回顾了二体和三体重子B的衰变，最终态是双重子B′¯。因此，我们总结了分支分数、角不对称和CP不对称的实验数据。利用W -玻色子湮灭(交换)机制，B的分支分数是可以解释的。在微扰QCD计数规则的方法中，我们研究了三体衰变通道。特别地，我们回顾了B / B B′¯M的CP不对称性，它们有望通过LHCb和Belle II实验来测量。最后,我们注意到解释B−B - p的理论挑战P¯ρ−andB B−p¯μ−ν¯μ .
{"title":"Baryonic <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M1\">\u0000 <mi>B</mi>\u0000 </math> Meson Decays","authors":"Xiaotao Huang, Yu-Kuo Hsiao, Jike Wang, Liang Sun","doi":"10.1155/2022/4343824","DOIUrl":"https://doi.org/10.1155/2022/4343824","url":null,"abstract":"<jats:p>We review the two- and three-body baryonic <jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M2\">\u0000 <mi>B</mi>\u0000 </math>\u0000 </jats:inline-formula> decays with the dibaryon (<jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M3\">\u0000 <mi mathvariant=\"bold\">B</mi>\u0000 <mover accent=\"true\">\u0000 <mrow>\u0000 <mi mathvariant=\"bold\">B</mi>\u0000 <mo>′</mo>\u0000 </mrow>\u0000 <mo stretchy=\"true\">¯</mo>\u0000 </mover>\u0000 </math>\u0000 </jats:inline-formula>) as the final states. Accordingly, we summarize the experimental data of the branching fractions, angular asymmetries, and <jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M4\">\u0000 <mtext>CP</mtext>\u0000 </math>\u0000 </jats:inline-formula> asymmetries. Using the <jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M5\">\u0000 <mi>W</mi>\u0000 </math>\u0000 </jats:inline-formula>-boson annihilation (exchange) mechanism, the branching fractions of <jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M6\">\u0000 <mi>B</mi>\u0000 <mo>⟶</mo>\u0000 <mi mathvariant=\"bold\">B</mi>\u0000 <mover accent=\"true\">\u0000 <mrow>\u0000 <mi mathvariant=\"bold\">B</mi>\u0000 <mo>′</mo>\u0000 </mrow>\u0000 <mo stretchy=\"true\">¯</mo>\u0000 </mover>\u0000 </math>\u0000 </jats:inline-formula> are shown to be interpretable. In the approach of perturbative QCD counting rules, we study the three-body decay channels. In particular, we review the <jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M7\">\u0000 <mtext>CP</mtext>\u0000 </math>\u0000 </jats:inline-formula> asymmetries of <jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M8\">\u0000 <mi>B</mi>\u0000 <mo>⟶</mo>\u0000 <mi mathvariant=\"bold\">B</mi>\u0000 <mover accent=\"true\">\u0000 <mrow>\u0000 <mi mathvariant=\"bold\">B</mi>\u0000 <mo>′</mo>\u0000 </mrow>\u0000 <mo stretchy=\"true\">¯</mo>\u0000 </mover>\u0000 <mi>M</mi>\u0000 ","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" ","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-03-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"43149609","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}
<jats:p>We study neutrino mass matrices with one texture equality and the neutrino mixing matrix having either its first (<jats:inline-formula> <math xmlns="http://www.w3.org/1998/Math/MathML" id="M1"> <mtext>T</mtext> <msub> <mrow> <mtext>M</mtext> </mrow> <mrow> <mn>1</mn> </mrow> </msub> </math> </jats:inline-formula>) or second (<jats:inline-formula> <math xmlns="http://www.w3.org/1998/Math/MathML" id="M2"> <mtext>T</mtext> <msub> <mrow> <mtext>M</mtext> </mrow> <mrow> <mn>2</mn> </mrow> </msub> </math> </jats:inline-formula>) column identical to that of the tribimaximal mixing matrix. We found that out of total fifteen possible neutrino mass matrices with one texture equality, only six textures are compatible with <jats:inline-formula> <math xmlns="http://www.w3.org/1998/Math/MathML" id="M3"> <mtext>T</mtext> <msub> <mrow> <mtext>M</mtext> </mrow> <mrow> <mn>1</mn> </mrow> </msub> </math> </jats:inline-formula> mixing and six textures are compatible with <jats:inline-formula> <math xmlns="http://www.w3.org/1998/Math/MathML" id="M4"> <mtext>T</mtext> <msub> <mrow> <mtext>M</mtext> </mrow> <mrow> <mn>2</mn> </mrow> </msub> </math> </jats:inline-formula> mixing in the light of the current neutrino oscillation data. These textures have interesting implications for the presently unknown parameters such as the neutrino mass scale, effective Majorana neutrino mass, effective neutrino mass, the atmospheric mixing, and the Dirac- and Majorana-type CP violating phases. We, also, present the <jats:inline-formula> <math xmlns="http://www.w3.org/1998/Math/MathML" id="M5"> <msub> <mrow> <mi>S</mi> </mrow> <mrow>
{"title":"Phenomenology of Trimaximal Mixing with One Texture Equality","authors":"S. Dev, Desh Raj","doi":"10.1155/2022/4952562","DOIUrl":"https://doi.org/10.1155/2022/4952562","url":null,"abstract":"<jats:p>We study neutrino mass matrices with one texture equality and the neutrino mixing matrix having either its first (<jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M1\">\u0000 <mtext>T</mtext>\u0000 <msub>\u0000 <mrow>\u0000 <mtext>M</mtext>\u0000 </mrow>\u0000 <mrow>\u0000 <mn>1</mn>\u0000 </mrow>\u0000 </msub>\u0000 </math>\u0000 </jats:inline-formula>) or second (<jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M2\">\u0000 <mtext>T</mtext>\u0000 <msub>\u0000 <mrow>\u0000 <mtext>M</mtext>\u0000 </mrow>\u0000 <mrow>\u0000 <mn>2</mn>\u0000 </mrow>\u0000 </msub>\u0000 </math>\u0000 </jats:inline-formula>) column identical to that of the tribimaximal mixing matrix. We found that out of total fifteen possible neutrino mass matrices with one texture equality, only six textures are compatible with <jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M3\">\u0000 <mtext>T</mtext>\u0000 <msub>\u0000 <mrow>\u0000 <mtext>M</mtext>\u0000 </mrow>\u0000 <mrow>\u0000 <mn>1</mn>\u0000 </mrow>\u0000 </msub>\u0000 </math>\u0000 </jats:inline-formula> mixing and six textures are compatible with <jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M4\">\u0000 <mtext>T</mtext>\u0000 <msub>\u0000 <mrow>\u0000 <mtext>M</mtext>\u0000 </mrow>\u0000 <mrow>\u0000 <mn>2</mn>\u0000 </mrow>\u0000 </msub>\u0000 </math>\u0000 </jats:inline-formula> mixing in the light of the current neutrino oscillation data. These textures have interesting implications for the presently unknown parameters such as the neutrino mass scale, effective Majorana neutrino mass, effective neutrino mass, the atmospheric mixing, and the Dirac- and Majorana-type CP violating phases. We, also, present the <jats:inline-formula>\u0000 <math xmlns=\"http://www.w3.org/1998/Math/MathML\" id=\"M5\">\u0000 <msub>\u0000 <mrow>\u0000 <mi>S</mi>\u0000 </mrow>\u0000 <mrow>\u0000 ","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":"1 1","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-02-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"41480361","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}
H. Vargas-Rodríguez, H. Rosu, M. G. Medina–Guevara, A. Gallegos, M. A. Muñiz-Torres
We consider electromagnetic fields having an angular momentum density in a locally nonrotating reference frame in Schwarzschild, Kerr, and Kerr-Newman spacetimes. The nature of such fields is assessed with two families of observers, the locally nonrotating ones and those of vanishing Poynting flux. The velocity fields of the vanishing-Poynting observers in the locally nonrotating reference frames are determined using the 3 + 1 decomposition formalism. From a methodological point of view and considering a classification of the electromagnetic field based on its invariants, it is convenient to separate the consideration of the vanishing-Poynting observers into two cases corresponding to the pure and nonpure fields; additionally, if there are regions where the field rotates with the speed of light (light surfaces), it becomes necessary to split these observers into two subfamilies. We present several examples of relevance in astrophysics and general relativity, such as pure rotating dipolar-like magnetic fields and the electromagnetic field of the Kerr-Newman solution. For the latter example, we see that vanishing-Poynting observers also measure a vanishing super-Poynting vector, confirming recent results in the literature. Finally, for all nonnull electromagnetic fields, we present the 4-velocity fields of vanishing Poynting observers in an arbitrary spacetime.
{"title":"Vanishing Poynting Observers and Electromagnetic Field Classification in Kerr and Kerr-Newman Spacetimes","authors":"H. Vargas-Rodríguez, H. Rosu, M. G. Medina–Guevara, A. Gallegos, M. A. Muñiz-Torres","doi":"10.1155/2022/1066886","DOIUrl":"https://doi.org/10.1155/2022/1066886","url":null,"abstract":"We consider electromagnetic fields having an angular momentum density in a locally nonrotating reference frame in Schwarzschild, Kerr, and Kerr-Newman spacetimes. The nature of such fields is assessed with two families of observers, the locally nonrotating ones and those of vanishing Poynting flux. The velocity fields of the vanishing-Poynting observers in the locally nonrotating reference frames are determined using the \u0000 \u0000 3\u0000 +\u0000 1\u0000 \u0000 decomposition formalism. From a methodological point of view and considering a classification of the electromagnetic field based on its invariants, it is convenient to separate the consideration of the vanishing-Poynting observers into two cases corresponding to the pure and nonpure fields; additionally, if there are regions where the field rotates with the speed of light (light surfaces), it becomes necessary to split these observers into two subfamilies. We present several examples of relevance in astrophysics and general relativity, such as pure rotating dipolar-like magnetic fields and the electromagnetic field of the Kerr-Newman solution. For the latter example, we see that vanishing-Poynting observers also measure a vanishing super-Poynting vector, confirming recent results in the literature. Finally, for all nonnull electromagnetic fields, we present the 4-velocity fields of vanishing Poynting observers in an arbitrary spacetime.","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" ","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-02-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"41789060","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}
John D. Vergados, Paraskevi C. Divari, Hiroyasu Ejiri
The possibility of detection of 5.5 MeV and 14.4 keV solar axions by observing axion-induced nuclear and atomic transitions is investigated. The presence of nuclear transitions between spin orbit partners can be manifested by the subsequent deexcitation via gamma ray emissions. The transition rates can also be studied in the context of radiative axion absorption by a nucleus. The elementary interaction is obtained in the context of the axion-quark couplings predicted by existing axion models. Then, these couplings will be transformed to the nucleon level utilizing reasonable existing models, which lead to effective transition operators. Using these operators, we calculate the needed nuclear matrix elements employing wave functions obtained in the context of the nuclear shell model. With these ingredients, we discuss possibilities of experimental observation of the axion-induced nuclear gamma rays. In the second part, we will examine the axion-induced production of X-rays (axion-photon conversion) or ionization from deeply bound electron orbits. In this case, the axion electron coupling is predicted by existing axion models; no renormalization is needed. The experimental signal is the observation of directly produced electrons and/or the emission of hard X-rays and Auger electrons, following the deexcitation of the final atom. Critical discussion is made on the experimental feasibility of detecting the solar axions by using multiton scale NaI detectors.
{"title":"Calculated Event Rates for Axion Detection via Atomic and Nuclear Processes","authors":"John D. Vergados, Paraskevi C. Divari, Hiroyasu Ejiri","doi":"10.1155/2022/7373365","DOIUrl":"https://doi.org/10.1155/2022/7373365","url":null,"abstract":"The possibility of detection of 5.5 MeV and 14.4 keV solar axions by observing axion-induced nuclear and atomic transitions is investigated. The presence of nuclear transitions between spin orbit partners can be manifested by the subsequent deexcitation via gamma ray emissions. The transition rates can also be studied in the context of radiative axion absorption by a nucleus. The elementary interaction is obtained in the context of the axion-quark couplings predicted by existing axion models. Then, these couplings will be transformed to the nucleon level utilizing reasonable existing models, which lead to effective transition operators. Using these operators, we calculate the needed nuclear matrix elements employing wave functions obtained in the context of the nuclear shell model. With these ingredients, we discuss possibilities of experimental observation of the axion-induced nuclear gamma rays. In the second part, we will examine the axion-induced production of X-rays (axion-photon conversion) or ionization from deeply bound electron orbits. In this case, the axion electron coupling is predicted by existing axion models; no renormalization is needed. The experimental signal is the observation of directly produced electrons and/or the emission of hard X-rays and Auger electrons, following the deexcitation of the final atom. Critical discussion is made on the experimental feasibility of detecting the solar axions by using multiton scale NaI detectors.","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":"34 7","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-02-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138520535","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}
Three-body <svg height="8.68572pt" style="vertical-align:-0.0498209pt" version="1.1" viewbox="-0.0498162 -8.6359 7.94191 8.68572" width="7.94191pt" 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="#g113-67"></use></g></svg> decays not only significantly broaden the study of <svg height="8.68572pt" style="vertical-align:-0.0498209pt" version="1.1" viewbox="-0.0498162 -8.6359 7.94191 8.68572" width="7.94191pt" 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="#g113-67"></use></g></svg> meson decay mechanisms but also provide information of resonant particles. Because of complicate dynamics, it is very hard for us to study the whole phase space in a specific approach. In this review, we take <span><svg height="13.0648pt" style="vertical-align:-2.268101pt" version="1.1" viewbox="-0.0498162 -10.7967 29.623 13.0648" width="29.623pt" 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="#g113-67"></use></g><g transform="matrix(.013,0,0,-0.013,11.445,0)"><use xlink:href="#g117-149"></use></g><g transform="matrix(.013,0,0,-0.013,17.221,0)"><use xlink:href="#g117-148"></use></g></svg><span></span><svg height="13.0648pt" style="vertical-align:-2.268101pt" version="1.1" viewbox="33.2821838 -10.7967 48.397 13.0648" width="48.397pt" xmlns="http://www.w3.org/2000/svg" xmlns:xlink="http://www.w3.org/1999/xlink"><g transform="matrix(.013,0,0,-0.013,33.332,0)"><use xlink:href="#g113-76"></use></g><g transform="matrix(.013,0,0,-0.013,43.149,0)"><use xlink:href="#g113-41"></use></g><g transform="matrix(.013,0,0,-0.013,47.647,0)"><use xlink:href="#g198-19"></use></g><g transform="matrix(.013,0,0,-0.013,63.551,0)"><use xlink:href="#g117-149"></use></g><g transform="matrix(.013,0,0,-0.013,69.327,0)"><use xlink:href="#g117-148"></use></g></svg><span></span><svg height="13.0648pt" style="vertical-align:-2.268101pt" version="1.1" viewbox="81.7561838 -10.7967 36.603 13.0648" width="36.603pt" xmlns="http://www.w3.org/2000/svg" xmlns:xlink="http://www.w3.org/1999/xlink"><g transform="matrix(.013,0,0,-0.013,81.806,0)"><use xlink:href="#g113-42"></use></g><g transform="matrix(.013,0,0,-0.013,86.304,0)"><use xlink:href="#g113-76"></use></g><g transform="matrix(.0091,0,0,-0.0091,96.122,-5.741)"><use xlink:href="#g54-36"></use></g><g transform="matrix(.013,0,0,-0.013,102.201,0)"><use xlink:href="#g113-76"></use></g><g transform="matrix(.0091,0,0,-0.0091,112.018,-5.741)"><use xlink:href="#g54-33"></use></g></svg></span> decays as examples and show the application of the perturbative QCD (PQCD) approach in studying the quasi-two-body <svg height="8.68572pt" style="vertical-align:-0.0498209pt" version="1.1" viewbox="-0.0498162 -8.6359 7.94191 8.68572" width="7.94191pt" xmlns="http://www.w3.org/2000/svg" xmlns:xlink="http://www
{"title":"Charmless Quasi-Two-Body Decays in Perturbative QCD Approach: Taking as Examples","authors":"Wen-Feng Liu, Zhi-Tian Zou, Ying Li","doi":"10.1155/2022/5287693","DOIUrl":"https://doi.org/10.1155/2022/5287693","url":null,"abstract":"Three-body <svg height=\"8.68572pt\" style=\"vertical-align:-0.0498209pt\" version=\"1.1\" viewbox=\"-0.0498162 -8.6359 7.94191 8.68572\" width=\"7.94191pt\" 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=\"#g113-67\"></use></g></svg> decays not only significantly broaden the study of <svg height=\"8.68572pt\" style=\"vertical-align:-0.0498209pt\" version=\"1.1\" viewbox=\"-0.0498162 -8.6359 7.94191 8.68572\" width=\"7.94191pt\" 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=\"#g113-67\"></use></g></svg> meson decay mechanisms but also provide information of resonant particles. Because of complicate dynamics, it is very hard for us to study the whole phase space in a specific approach. In this review, we take <span><svg height=\"13.0648pt\" style=\"vertical-align:-2.268101pt\" version=\"1.1\" viewbox=\"-0.0498162 -10.7967 29.623 13.0648\" width=\"29.623pt\" 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=\"#g113-67\"></use></g><g transform=\"matrix(.013,0,0,-0.013,11.445,0)\"><use xlink:href=\"#g117-149\"></use></g><g transform=\"matrix(.013,0,0,-0.013,17.221,0)\"><use xlink:href=\"#g117-148\"></use></g></svg><span></span><svg height=\"13.0648pt\" style=\"vertical-align:-2.268101pt\" version=\"1.1\" viewbox=\"33.2821838 -10.7967 48.397 13.0648\" width=\"48.397pt\" xmlns=\"http://www.w3.org/2000/svg\" xmlns:xlink=\"http://www.w3.org/1999/xlink\"><g transform=\"matrix(.013,0,0,-0.013,33.332,0)\"><use xlink:href=\"#g113-76\"></use></g><g transform=\"matrix(.013,0,0,-0.013,43.149,0)\"><use xlink:href=\"#g113-41\"></use></g><g transform=\"matrix(.013,0,0,-0.013,47.647,0)\"><use xlink:href=\"#g198-19\"></use></g><g transform=\"matrix(.013,0,0,-0.013,63.551,0)\"><use xlink:href=\"#g117-149\"></use></g><g transform=\"matrix(.013,0,0,-0.013,69.327,0)\"><use xlink:href=\"#g117-148\"></use></g></svg><span></span><svg height=\"13.0648pt\" style=\"vertical-align:-2.268101pt\" version=\"1.1\" viewbox=\"81.7561838 -10.7967 36.603 13.0648\" width=\"36.603pt\" xmlns=\"http://www.w3.org/2000/svg\" xmlns:xlink=\"http://www.w3.org/1999/xlink\"><g transform=\"matrix(.013,0,0,-0.013,81.806,0)\"><use xlink:href=\"#g113-42\"></use></g><g transform=\"matrix(.013,0,0,-0.013,86.304,0)\"><use xlink:href=\"#g113-76\"></use></g><g transform=\"matrix(.0091,0,0,-0.0091,96.122,-5.741)\"><use xlink:href=\"#g54-36\"></use></g><g transform=\"matrix(.013,0,0,-0.013,102.201,0)\"><use xlink:href=\"#g113-76\"></use></g><g transform=\"matrix(.0091,0,0,-0.0091,112.018,-5.741)\"><use xlink:href=\"#g54-33\"></use></g></svg></span> decays as examples and show the application of the perturbative QCD (PQCD) approach in studying the quasi-two-body <svg height=\"8.68572pt\" style=\"vertical-align:-0.0498209pt\" version=\"1.1\" viewbox=\"-0.0498162 -8.6359 7.94191 8.68572\" width=\"7.94191pt\" xmlns=\"http://www.w3.org/2000/svg\" xmlns:xlink=\"http://www","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":"15 1","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-02-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138542840","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 review, we discuss the calculation of the B ⟶ P , V form factors within the framework of the light-cone sum rules with the light-cone distribution amplitudes of the B -meson. A detailed introduction to the definition, scale evolution, and phenomenological models of the B -meson distribution amplitudes is presented. We show two equivalent approaches of calculating the next-to-leading order QCD corrections to the sum rules for the form factors, i.e., the method of regions and the step-by-step matching in the soft-collinear effective theory. The power suppressed corrections to the B ⟶ P , V form factors especially the contributions from the higher-twist B -meson distribution amplitudes are displayed. We also present numerical results of the form factors including both the QCD and the power corrections, and phenomenological applications of the predicted form factors such as the determination of the CKM matrix element V u b .
在这篇综述中，我们讨论了B介子的光锥分布振幅和光锥和规则框架内的B、P、V形因子的计算。详细介绍了B介子分布振幅的定义、尺度演化和现象学模型。我们给出了计算形状因子和规则的次领先阶QCD修正的两种等效方法，即软共线有效理论中的区域法和逐步匹配法。显示了对B、P、V形状因子的功率抑制修正，特别是高捻B介子分布幅度的贡献。我们还给出了形状因子的数值结果，包括QCD和功率校正，以及预测形状因子的现象学应用，如CKM矩阵元素V u b的确定。
{"title":"B\u0000 ⟶\u0000 P\u0000 ,\u0000 V\u0000 Form Factors with the \u0000 B\u0000 -Meson Light-Cone Sum Rules","authors":"Yue Shen, Yan-Bing Wei","doi":"10.1155/2022/2755821","DOIUrl":"https://doi.org/10.1155/2022/2755821","url":null,"abstract":"In this review, we discuss the calculation of the \u0000 \u0000 B\u0000 ⟶\u0000 P\u0000 ,\u0000 V\u0000 \u0000 form factors within the framework of the light-cone sum rules with the light-cone distribution amplitudes of the \u0000 \u0000 B\u0000 \u0000 -meson. A detailed introduction to the definition, scale evolution, and phenomenological models of the \u0000 \u0000 B\u0000 \u0000 -meson distribution amplitudes is presented. We show two equivalent approaches of calculating the next-to-leading order QCD corrections to the sum rules for the form factors, i.e., the method of regions and the step-by-step matching in the soft-collinear effective theory. The power suppressed corrections to the \u0000 \u0000 B\u0000 ⟶\u0000 P\u0000 ,\u0000 V\u0000 \u0000 form factors especially the contributions from the higher-twist \u0000 \u0000 B\u0000 \u0000 -meson distribution amplitudes are displayed. We also present numerical results of the form factors including both the QCD and the power corrections, and phenomenological applications of the predicted form factors such as the determination of the CKM matrix element \u0000 \u0000 \u0000 \u0000 \u0000 \u0000 V\u0000 \u0000 \u0000 u\u0000 b\u0000 \u0000 \u0000 \u0000 \u0000 \u0000 .","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" ","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-02-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"43684631","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 work, we study thermodynamics of generalized Ayon-Beato and Garcia (ABG) black hole metric which contains three parameters named as mass m , magnetic charge q , and dimensionless coupling constant of nonlinear electrodynamics interacting field γ . We showed that central regions of this black hole behaves as dS (AdS) vacuum space by setting q < 2 m q > 2 m and in the case q = 2 m reaches to a flat Minkowski space. In the large distances, this black hole behaves as a Reissner-Nordstrom BH. However, an important role of the charge q appeared in the production of a formal variable cosmological parameter which will support pressure coordinate in the thermodynamic perspective of this black hole in our setup. We should point that this formal variable cosmological parameter is different with cosmological constant which comes from AdS/CFT correspondence, and it is effective at large distances as AdS space pressure. In our setup, the assumed pressure originated from the internal material of the black hole say q and m here. By calculating the Hawking temperature of this black hole, we obtain equation of state. Then, we plotted isothermal P-V curves and heat capacity at constant pressure. They show that the system participates in the small to large phase transition of the black hole or the Hawking-Page phase transition which is similar to the van der Waals phase transition in the ordinary thermodynamics systems. In fact in the Hawking-Page phase transition disequilibrium, evaporating generalized ABG black hole reaches to a vacuum AdS space finally.
{"title":"Thermodynamic Phase Transition of Generalized Ayon-Beato Garcia Black Holes","authors":"E. Ghasemi, H. Ghaffarnejad","doi":"10.1155/2023/6446767","DOIUrl":"https://doi.org/10.1155/2023/6446767","url":null,"abstract":"In this work, we study thermodynamics of generalized Ayon-Beato and Garcia (ABG) black hole metric which contains three parameters named as mass \u0000 \u0000 m\u0000 \u0000 , magnetic charge \u0000 \u0000 q\u0000 \u0000 , and dimensionless coupling constant of nonlinear electrodynamics interacting field \u0000 \u0000 γ\u0000 \u0000 . We showed that central regions of this black hole behaves as dS (AdS) vacuum space by setting \u0000 \u0000 q\u0000 <\u0000 2\u0000 m\u0000 \u0000 \u0000 q\u0000 >\u0000 2\u0000 m\u0000 \u0000 \u0000 \u0000 and in the case \u0000 \u0000 q\u0000 =\u0000 2\u0000 m\u0000 \u0000 reaches to a flat Minkowski space. In the large distances, this black hole behaves as a Reissner-Nordstrom BH. However, an important role of the charge\u0000 \u0000 q\u0000 \u0000 appeared in the production of a formal variable cosmological parameter which will support pressure coordinate in the thermodynamic perspective of this black hole in our setup. We should point that this formal variable cosmological parameter is different with cosmological constant which comes from AdS/CFT correspondence, and it is effective at large distances as AdS space pressure. In our setup, the assumed pressure originated from the internal material of the black hole say \u0000 \u0000 q\u0000 \u0000 and \u0000 \u0000 m\u0000 \u0000 here. By calculating the Hawking temperature of this black hole, we obtain equation of state. Then, we plotted isothermal P-V curves and heat capacity at constant pressure. They show that the system participates in the small to large phase transition of the black hole or the Hawking-Page phase transition which is similar to the van der Waals phase transition in the ordinary thermodynamics systems. In fact in the Hawking-Page phase transition disequilibrium, evaporating generalized ABG black hole reaches to a vacuum AdS space finally.","PeriodicalId":7498,"journal":{"name":"Advances in High Energy Physics","volume":" ","pages":""},"PeriodicalIF":1.7,"publicationDate":"2022-01-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"46224450","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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