Pub Date : 2023-10-18DOI: 10.1142/s0217732323501377
A. Patkós
Oscillating and dissipative energy exchange between the electromagnetic and axion fields is investigated in an effective electro-magneto dynamical (EEMD) model theory, implying the coexistence of axions with hypothetic magnetic charges. An exact formula is presented for the energy transfer between the electromagnetic and axionic sectors. In a first example, we compute analytically the homogeneously oscillating electric and magnetic field configurations generated by the combined action of a constant static magnetic field and a periodically oscillating axion condensate. In the second example, the electromagnetic radiative energy loss of a gravitationally bound axion configuration is computed in the EEMD model. As a result, an asymptotic [Formula: see text] temporal increase of the clump size is found also in EEMD.
{"title":"Electromagnetic energy transfer processes in effective electro-magneto dynamics of axions","authors":"A. Patkós","doi":"10.1142/s0217732323501377","DOIUrl":"https://doi.org/10.1142/s0217732323501377","url":null,"abstract":"Oscillating and dissipative energy exchange between the electromagnetic and axion fields is investigated in an effective electro-magneto dynamical (EEMD) model theory, implying the coexistence of axions with hypothetic magnetic charges. An exact formula is presented for the energy transfer between the electromagnetic and axionic sectors. In a first example, we compute analytically the homogeneously oscillating electric and magnetic field configurations generated by the combined action of a constant static magnetic field and a periodically oscillating axion condensate. In the second example, the electromagnetic radiative energy loss of a gravitationally bound axion configuration is computed in the EEMD model. As a result, an asymptotic [Formula: see text] temporal increase of the clump size is found also in EEMD.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"1 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135884040","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}
Pub Date : 2023-10-17DOI: 10.1142/s0217732323501286
Yunshuang Du
Black hole thermodynamics, in which physical quantities are global, is well established. In realistic astrophysical processes, the quasi-local black hole thermodynamics (thermodynamics in a finite spacetime region) is an essential problem. We develop quasi-local black hole thermodynamics by using the quasi-local energies of gravitation. For the first time, we suggest the concept of gravitational pressure, i.e. the pressure of gravitational field itself in thermodynamics for black holes, and find that it is necessary for quasi-local black hole thermodynamics in asymptotic flat space. We extend quasi-local black hole thermodynamics to the cases of asymptotic de Sitter and anti-de Sitter spaces. This exploration presents new insights into quasi-local energy of gravity, and is much more closely related to realistic astrophysics.
{"title":"Quasi-local black hole thermodynamics and gravitational pressure","authors":"Yunshuang Du","doi":"10.1142/s0217732323501286","DOIUrl":"https://doi.org/10.1142/s0217732323501286","url":null,"abstract":"Black hole thermodynamics, in which physical quantities are global, is well established. In realistic astrophysical processes, the quasi-local black hole thermodynamics (thermodynamics in a finite spacetime region) is an essential problem. We develop quasi-local black hole thermodynamics by using the quasi-local energies of gravitation. For the first time, we suggest the concept of gravitational pressure, i.e. the pressure of gravitational field itself in thermodynamics for black holes, and find that it is necessary for quasi-local black hole thermodynamics in asymptotic flat space. We extend quasi-local black hole thermodynamics to the cases of asymptotic de Sitter and anti-de Sitter spaces. This exploration presents new insights into quasi-local energy of gravity, and is much more closely related to realistic astrophysics.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"8 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135992776","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}
Pub Date : 2023-10-17DOI: 10.1142/s0217732323501390
Matin Alipour, Rahime Sufiani
The thermal quantum correlations of a three-qubit spin chain of XY type under an in-homogeneous magnetic field have been investigated, where by considering magnetic fields with different magnitudes [Formula: see text], [Formula: see text] and [Formula: see text] for each spin, the quantum correlations between the adjacent and the non-adjacent qubits (spins) have been studied. For this purpose, the concurrence as an entanglement quantifier and the trace distance discord as a discord-like quantifier have been computed for the corresponding bipartite subsystems with the reduced density matrices [Formula: see text], [Formula: see text] and [Formula: see text]. The differences between the concurrence and the trace distance discord, are explained in detail. Their dependence on the parameters of the uniform magnetic field [Formula: see text], the temperature [Formula: see text], and the in-homogeneity parameter [Formula: see text] is discussed so that the thermal correlation decreases by increasing the mentioned parameters. Also, the results show that by changing and controlling the parameters [Formula: see text], [Formula: see text] and [Formula: see text], especially the in-homogeneous magnetic field [Formula: see text], it is possible that the correlation value between non-adjacent spins, i.e. [Formula: see text] can be reached to a greater value than the thermal correlations between adjacent spins, i.e. [Formula: see text] and [Formula: see text]. Moreover, it is shown that the trace distance [Formula: see text] between the non-adjacent spins has always a lower value than those of the adjacent spins [Formula: see text] and [Formula: see text]. Finally, the results show that in-homogeneous magnetic field b can be effective for improving thermal quantum correlation.
{"title":"Thermal quantum correlations in a three-qubit spin chain under an in-homogeneous magnetic field","authors":"Matin Alipour, Rahime Sufiani","doi":"10.1142/s0217732323501390","DOIUrl":"https://doi.org/10.1142/s0217732323501390","url":null,"abstract":"The thermal quantum correlations of a three-qubit spin chain of XY type under an in-homogeneous magnetic field have been investigated, where by considering magnetic fields with different magnitudes [Formula: see text], [Formula: see text] and [Formula: see text] for each spin, the quantum correlations between the adjacent and the non-adjacent qubits (spins) have been studied. For this purpose, the concurrence as an entanglement quantifier and the trace distance discord as a discord-like quantifier have been computed for the corresponding bipartite subsystems with the reduced density matrices [Formula: see text], [Formula: see text] and [Formula: see text]. The differences between the concurrence and the trace distance discord, are explained in detail. Their dependence on the parameters of the uniform magnetic field [Formula: see text], the temperature [Formula: see text], and the in-homogeneity parameter [Formula: see text] is discussed so that the thermal correlation decreases by increasing the mentioned parameters. Also, the results show that by changing and controlling the parameters [Formula: see text], [Formula: see text] and [Formula: see text], especially the in-homogeneous magnetic field [Formula: see text], it is possible that the correlation value between non-adjacent spins, i.e. [Formula: see text] can be reached to a greater value than the thermal correlations between adjacent spins, i.e. [Formula: see text] and [Formula: see text]. Moreover, it is shown that the trace distance [Formula: see text] between the non-adjacent spins has always a lower value than those of the adjacent spins [Formula: see text] and [Formula: see text]. Finally, the results show that in-homogeneous magnetic field b can be effective for improving thermal quantum correlation.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"26 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135992939","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}
Pub Date : 2023-10-12DOI: 10.1142/s0217732323501365
Amano, S., Aritomo, Y., Ohta, M.
The very early stage of the coalescence of two nuclei is studied and used to estimate the nuclear viscosity. The time evolution of the neck region has been simulated by the unified Langevin equation method, which is used in the analysis of heavy-ion collisions from the approaching stage to the fusion-fission stage. It is found that the transition from viscous to inertial coalescence that appeared in the neck growth of macroscopic drops can also be seen in the present simulation in nucleus–nucleus collisions. The dynamics of neck growth is analyzed in terms of the hydrodynamical formula and the viscosity coefficient of nuclear matter is estimated using the analogy of macroscopic drops.
{"title":"Nuclear viscosity estimated by dynamics of neck formation in the early stage of nuclear collision","authors":"Amano, S., Aritomo, Y., Ohta, M.","doi":"10.1142/s0217732323501365","DOIUrl":"https://doi.org/10.1142/s0217732323501365","url":null,"abstract":"The very early stage of the coalescence of two nuclei is studied and used to estimate the nuclear viscosity. The time evolution of the neck region has been simulated by the unified Langevin equation method, which is used in the analysis of heavy-ion collisions from the approaching stage to the fusion-fission stage. It is found that the transition from viscous to inertial coalescence that appeared in the neck growth of macroscopic drops can also be seen in the present simulation in nucleus–nucleus collisions. The dynamics of neck growth is analyzed in terms of the hydrodynamical formula and the viscosity coefficient of nuclear matter is estimated using the analogy of macroscopic drops.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"15 20 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135923421","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}
Pub Date : 2023-10-09DOI: 10.1142/s0217732323501353
Anupam Singh
Dark energy is the largest fraction of the energy density of our universe — yet it remains one of the enduring enigmas of our times. Here we show that dark energy can be used to solve 2 tantalizing mysteries of the observable universe. We build on existing models of dark energy linked to neutrino masses. In these models, dark energy can undergo phase transitions and form black holes. Here we look at the implications of the family structure of neutrinos for the phase transitions in dark energy and associated peaks in black hole formation. It has been previously shown that one of these peaks in black hole formation is associated with the observed peak in quasar formation at redshifts [Formula: see text]. Here, we predict that there will also be an earlier peak in the dark energy black holes at high redshifts [Formula: see text]. These dark energy black holes formed at high redshifts are Intermediate Mass Black Holes (IMBHs). These dark energy black holes at large redshift can help explain both the EDGES observations and the observations of large Supermassive Black Holes (SMBHs) at redshifts of 7 or larger. This work directs us to actively look for these dark energy black holes at these high redshifts as predicted here through targeted searches for these black holes at the redshifts [Formula: see text] near 18. There is a slight dependence of the location of the peak on the lightest neutrino mass. This may enable a measurement of the lightest neutrino mass — something which has eluded us so far. Finding these dark energy black holes of Intermediate Mass should be within the reach of upcoming observations — particularly with the James Webb Space Telescope — but perhaps also through the use of other innovative techniques focusing specifically on the redshifts [Formula: see text] around 18.
{"title":"Dark energy black holes with intermediate masses at high redshifts: An earlier generation of quasars and observations","authors":"Anupam Singh","doi":"10.1142/s0217732323501353","DOIUrl":"https://doi.org/10.1142/s0217732323501353","url":null,"abstract":"Dark energy is the largest fraction of the energy density of our universe — yet it remains one of the enduring enigmas of our times. Here we show that dark energy can be used to solve 2 tantalizing mysteries of the observable universe. We build on existing models of dark energy linked to neutrino masses. In these models, dark energy can undergo phase transitions and form black holes. Here we look at the implications of the family structure of neutrinos for the phase transitions in dark energy and associated peaks in black hole formation. It has been previously shown that one of these peaks in black hole formation is associated with the observed peak in quasar formation at redshifts [Formula: see text]. Here, we predict that there will also be an earlier peak in the dark energy black holes at high redshifts [Formula: see text]. These dark energy black holes formed at high redshifts are Intermediate Mass Black Holes (IMBHs). These dark energy black holes at large redshift can help explain both the EDGES observations and the observations of large Supermassive Black Holes (SMBHs) at redshifts of 7 or larger. This work directs us to actively look for these dark energy black holes at these high redshifts as predicted here through targeted searches for these black holes at the redshifts [Formula: see text] near 18. There is a slight dependence of the location of the peak on the lightest neutrino mass. This may enable a measurement of the lightest neutrino mass — something which has eluded us so far. Finding these dark energy black holes of Intermediate Mass should be within the reach of upcoming observations — particularly with the James Webb Space Telescope — but perhaps also through the use of other innovative techniques focusing specifically on the redshifts [Formula: see text] around 18.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"36 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135146932","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}
Pub Date : 2023-10-07DOI: 10.1142/s0217732323501328
Parada T. P. Hutauruk
In this exploratory study, I present, for the first time, the implications of the charge symmetry breaking (CSB) that arise from the [Formula: see text] and [Formula: see text] quark-mass differences on gluon and sea quark distribution functions of the pion and kaon in the framework of the Nambu–Jona-Lasino (NJL) model, which is a quark-level chiral effective theory of QCD, with the help of the proper-time regularization scheme to simulate color confinement of QCD. From the analysis, one finds that the charge symmetry (CS) gluon distribution for the pion has a good agreement with the prediction results obtained from the recent lattice QCD simulation and JAM global fit QCD analysis at a higher scale of [Formula: see text][Formula: see text]GeV 2 . The size of the CSB effects on gluon and sea quark distributions for the pion with the realistic ratios of [Formula: see text] at [Formula: see text][Formula: see text]GeV 2 are, respectively, estimated by 1.3% and 2.0% at [Formula: see text] in comparison with those for [Formula: see text], while those for the kaon are approximately about 0.3% and 0.5% at [Formula: see text], respectively. A remarkable result is found that the CSB effects on gluon distribution for the kaon are smaller than that for the pion, which has a similar prediction result as that for the CS case.
在这一探索性研究中，我首次提出了由[公式:见文]和[公式:见文]夸克质量差异对量子cd夸克级手性有效理论nambujana - jona - lasino (NJL)模型框架下介子和介子的胶子和海夸克分布函数产生的电荷对称破缺(CSB)的含义，并借助固有时正则化方案来模拟量子cd的色限。通过分析，发现介子的电荷对称(CS)胶子分布与最近的晶格QCD模拟和JAM全局拟合QCD分析的预测结果在更高尺度[公式:见文][公式:见文]GeV 2上有很好的一致性。在[公式:见文][公式:见文][公式:见文]gev2的实际比率下，CSB对介子和海夸克分布的影响大小在[公式:见文][公式:见文]分别比[公式:见文][公式:见文]估计在[公式:见文]时约为1.3%和2.0%，而介子的影响大小在[公式:见文]时约为0.3%和0.5%。一个显著的结果是，CSB对介子胶子分布的影响小于介子，与CS的预测结果相似。
{"title":"Impact of charge symmetry breaking on gluon and sea quark distributions in the pion and kaon","authors":"Parada T. P. Hutauruk","doi":"10.1142/s0217732323501328","DOIUrl":"https://doi.org/10.1142/s0217732323501328","url":null,"abstract":"In this exploratory study, I present, for the first time, the implications of the charge symmetry breaking (CSB) that arise from the [Formula: see text] and [Formula: see text] quark-mass differences on gluon and sea quark distribution functions of the pion and kaon in the framework of the Nambu–Jona-Lasino (NJL) model, which is a quark-level chiral effective theory of QCD, with the help of the proper-time regularization scheme to simulate color confinement of QCD. From the analysis, one finds that the charge symmetry (CS) gluon distribution for the pion has a good agreement with the prediction results obtained from the recent lattice QCD simulation and JAM global fit QCD analysis at a higher scale of [Formula: see text][Formula: see text]GeV 2 . The size of the CSB effects on gluon and sea quark distributions for the pion with the realistic ratios of [Formula: see text] at [Formula: see text][Formula: see text]GeV 2 are, respectively, estimated by 1.3% and 2.0% at [Formula: see text] in comparison with those for [Formula: see text], while those for the kaon are approximately about 0.3% and 0.5% at [Formula: see text], respectively. A remarkable result is found that the CSB effects on gluon distribution for the kaon are smaller than that for the pion, which has a similar prediction result as that for the CS case.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"298 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135301110","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}
Pub Date : 2023-10-07DOI: 10.1142/s0217732323501316
Naman Kumar
A microscopic derivation of the Bekenstein–Hawking entropy for the Schwarzschild black hole was presented earlier by using a nontrivial phase space. It was argued that the Schwarzschild black hole behaves like a [Formula: see text] quantum mechanical system. In this paper, we show that if we assume the phase space to obey the holographic principle and take the microscopic particles inside the quantum gravitational system to be ideal bosonic gas, we can derive the Bekenstein–Hawking entropy. The assumption of the phase space to follow the holographic principle such that the Schwarzschild black hole behaves as a [Formula: see text] system is very much in the spirit of our understanding of black holes than their behavior as a [Formula: see text] system. However, the argument suggests that the black hole be treated as a system with the equation of state [Formula: see text].
{"title":"A statistical derivation of Bekenstein–Hawking entropy for Schwarzschild black holes","authors":"Naman Kumar","doi":"10.1142/s0217732323501316","DOIUrl":"https://doi.org/10.1142/s0217732323501316","url":null,"abstract":"A microscopic derivation of the Bekenstein–Hawking entropy for the Schwarzschild black hole was presented earlier by using a nontrivial phase space. It was argued that the Schwarzschild black hole behaves like a [Formula: see text] quantum mechanical system. In this paper, we show that if we assume the phase space to obey the holographic principle and take the microscopic particles inside the quantum gravitational system to be ideal bosonic gas, we can derive the Bekenstein–Hawking entropy. The assumption of the phase space to follow the holographic principle such that the Schwarzschild black hole behaves as a [Formula: see text] system is very much in the spirit of our understanding of black holes than their behavior as a [Formula: see text] system. However, the argument suggests that the black hole be treated as a system with the equation of state [Formula: see text].","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"16 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135301312","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}
Pub Date : 2023-09-22DOI: 10.1142/s021773232350102x
Qi Sun, Qian Li, Yu Zhang, Qi-Quan Li
We study the quasinormal modes, Hawking radiation and absorption cross-section of the Bardeen black hole surrounded by perfect fluid dark matter for a massless scalar field. Our results show that the oscillation frequency of quasinormal modes is enhanced as magnetic charge [Formula: see text] or the dark matter parameter [Formula: see text] increases. For damping rate of quasinormal modes, the influence of them is different. Specifically, the increase of dark matter parameter [Formula: see text] makes the damping rate increasing at first and then decreasing. While the damping rate is continuously decreasing with the increase of the magnetic charge [Formula: see text]. Moreover, we find that the increase of the dark matter parameter [Formula: see text] enhances the power emission spectrum whereas magnetic charge [Formula: see text] suppresses it. This means that the lifespan of black holes increases for smaller value of [Formula: see text] and larger value of [Formula: see text] when other parameters are fixed. Finally, the absorption cross-section of the considered black hole is calculated with the help of the partial wave approach. Our results suggest that the absorption cross-section decreases with the dark matter parameter [Formula: see text] or the magnetic charge [Formula: see text] increasing.
{"title":"Quasinormal modes, Hawking radiation and absorption of the massless scalar field for Bardeen black hole surrounded by perfect fluid dark matter","authors":"Qi Sun, Qian Li, Yu Zhang, Qi-Quan Li","doi":"10.1142/s021773232350102x","DOIUrl":"https://doi.org/10.1142/s021773232350102x","url":null,"abstract":"We study the quasinormal modes, Hawking radiation and absorption cross-section of the Bardeen black hole surrounded by perfect fluid dark matter for a massless scalar field. Our results show that the oscillation frequency of quasinormal modes is enhanced as magnetic charge [Formula: see text] or the dark matter parameter [Formula: see text] increases. For damping rate of quasinormal modes, the influence of them is different. Specifically, the increase of dark matter parameter [Formula: see text] makes the damping rate increasing at first and then decreasing. While the damping rate is continuously decreasing with the increase of the magnetic charge [Formula: see text]. Moreover, we find that the increase of the dark matter parameter [Formula: see text] enhances the power emission spectrum whereas magnetic charge [Formula: see text] suppresses it. This means that the lifespan of black holes increases for smaller value of [Formula: see text] and larger value of [Formula: see text] when other parameters are fixed. Finally, the absorption cross-section of the considered black hole is calculated with the help of the partial wave approach. Our results suggest that the absorption cross-section decreases with the dark matter parameter [Formula: see text] or the magnetic charge [Formula: see text] increasing.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"256 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136099111","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}
Pub Date : 2023-09-21DOI: 10.1142/s0217732323501109
Mikhail K. Volkov, Kanat Nurlan, Aleksey A. Pivovarov
The branching fractions of [Formula: see text] and [Formula: see text] are calculated within the chiral NJL model. Features of the axial-vector [Formula: see text] meson which play an important role in describing the [Formula: see text] decays are discussed. Permissible values for the mass and width of the [Formula: see text] meson are considered in accordance with the latest experiments.
{"title":"The decay τ→3πντ and axial-vector meson a1 in the NJL model","authors":"Mikhail K. Volkov, Kanat Nurlan, Aleksey A. Pivovarov","doi":"10.1142/s0217732323501109","DOIUrl":"https://doi.org/10.1142/s0217732323501109","url":null,"abstract":"The branching fractions of [Formula: see text] and [Formula: see text] are calculated within the chiral NJL model. Features of the axial-vector [Formula: see text] meson which play an important role in describing the [Formula: see text] decays are discussed. Permissible values for the mass and width of the [Formula: see text] meson are considered in accordance with the latest experiments.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"22 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136237367","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}
Pub Date : 2023-09-19DOI: 10.1142/s0217732323501055
Abdelmadjid Maireche
Under the influence of the deformation space-space symmetries, the improved Mobius square plus generalized Yukawa potentials (IMSGYPs) have been employed to solve the deformed Klien–Gordon equation in three-dimensional noncommutative relativistic quantum space (3D-RNCQS) symmetries. Combined with the approximation approach suggested by Greene and Aldrich, we also employ the parametric Bopp’s shift approach and standard perturbation theory to derive novel relativistic energy eigenvalues. The new relativistic energy eigenvalues of (N 2 , K 2 , NI, ScI, and RbH) diatomic molecules under the IMSGYPs were shown to be sensitive to the atomic quantum numbers ([Formula: see text]), the mixed potential depths ([Formula: see text]), the screening parameter’s inverse [Formula: see text] and non-commutativity parameters ([Formula: see text], [Formula: see text], [Formula: see text]). In addition, we analyzed the new non-relativistic energy values in three-dimensional noncommutative non-relativistic quantum space (3D-NRNCQS) symmetries, by applying the well-known mapping in the literature. Furthermore, we studied many special cases useful to researchers in the framework of the new extended symmetries, such as the newly generalized Mobius square potential, the newly generalized Yukawa potential, and the newly generalized Deng-Fan potential. The study is further extended to calculate the mass spectra of mesons of the heavy quarkonium system, such as [Formula: see text], bottomonium [Formula: see text], [Formula: see text] and light mesons [Formula: see text] and [Formula: see text], that have the quark and antiquark flavors within the framework of the IMSGYPs model in 3D-NRNCQS symmetries.
{"title":"Effect of the non-commutativity of space on the improved Mobius square plus generalized Yukawa potentials of the Klein–Gordon and Schrödinger equations in 3D-RNCQS and 3D-NRNCQS symmetries","authors":"Abdelmadjid Maireche","doi":"10.1142/s0217732323501055","DOIUrl":"https://doi.org/10.1142/s0217732323501055","url":null,"abstract":"Under the influence of the deformation space-space symmetries, the improved Mobius square plus generalized Yukawa potentials (IMSGYPs) have been employed to solve the deformed Klien–Gordon equation in three-dimensional noncommutative relativistic quantum space (3D-RNCQS) symmetries. Combined with the approximation approach suggested by Greene and Aldrich, we also employ the parametric Bopp’s shift approach and standard perturbation theory to derive novel relativistic energy eigenvalues. The new relativistic energy eigenvalues of (N 2 , K 2 , NI, ScI, and RbH) diatomic molecules under the IMSGYPs were shown to be sensitive to the atomic quantum numbers ([Formula: see text]), the mixed potential depths ([Formula: see text]), the screening parameter’s inverse [Formula: see text] and non-commutativity parameters ([Formula: see text], [Formula: see text], [Formula: see text]). In addition, we analyzed the new non-relativistic energy values in three-dimensional noncommutative non-relativistic quantum space (3D-NRNCQS) symmetries, by applying the well-known mapping in the literature. Furthermore, we studied many special cases useful to researchers in the framework of the new extended symmetries, such as the newly generalized Mobius square potential, the newly generalized Yukawa potential, and the newly generalized Deng-Fan potential. The study is further extended to calculate the mass spectra of mesons of the heavy quarkonium system, such as [Formula: see text], bottomonium [Formula: see text], [Formula: see text] and light mesons [Formula: see text] and [Formula: see text], that have the quark and antiquark flavors within the framework of the IMSGYPs model in 3D-NRNCQS symmetries.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"32 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135011561","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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