Pub Date : 2023-12-09DOI: 10.1142/s0217732323501626
A. Maireche
In this paper, the modified Dirac equation (MDE) has been solved approximately for improved Manning–Rosen plus quasi-Hellman potentials (IMRQHPs), including the improved Yukawa tensor interaction under new spin symmetry and pseudospin symmetry for arbitrary spin–orbit number [Formula: see text], an appropriate approximation employed on the centrifugal terms in the symmetries of three-dimensional extended relativistic quantum mechanics (3D-ERQM). This potential is a superposition of Manning–Rosen plus quasi-Hellman potentials and some other exponential terms. Through the application of both new approximations to deal with the centrifugal term, Bopp’s shift method and the independent-time perturbation theory method, the recent modified approximate energy corrections under IMRQHPs are obtained for nuclei [Formula: see text]O and [Formula: see text]F and (O2, I2, N2, H2, LiH, CO and NO) diatomic molecules in 3D-ERQM and three-dimensional extended non-relativistic quantum mechanics (3D-ENRQM) symmetries. The recent values that we get appear sensitive to [Formula: see text], which are known as the discrete atomic quantum numbers, the mixed potential depths ([Formula: see text], [Formula: see text]) and [Formula: see text], the range of the potential [Formula: see text] and non-commutativity parameters [Formula: see text]. In both 3D-ERQM and 3D-ENRQM symmetries, we show that the recent corrections obtained on the new bound states under IMRQHPs are infinitesimal to the principal part of energy in the ordinary cases of 3D-RQM and 3D-NRQM symmetries. In the new symmetries of 3D-ERQM symmetries, it is not possible to get the exact analytical solutions [Formula: see text] and [Formula: see text], only the approximate solutions are possible. In addition, we discussed in detail the non-relativistic study of the studied mixed potentials. Four special cases, i.e. we investigated some special cases in the context of modified Schrödinger theories. In the framework of known relativistic quantum mechanics, we have clearly demonstrated that the modified Schrödinger equation can be represented as the Dirac equation under the influence of IMRQHPs.
{"title":"New spin and p-spin symmetries of the deformed Dirac equation for the IMRQHPs including the improved YLT interaction in three-dimensional extended relativistic quantum mechanics symmetries","authors":"A. Maireche","doi":"10.1142/s0217732323501626","DOIUrl":"https://doi.org/10.1142/s0217732323501626","url":null,"abstract":"In this paper, the modified Dirac equation (MDE) has been solved approximately for improved Manning–Rosen plus quasi-Hellman potentials (IMRQHPs), including the improved Yukawa tensor interaction under new spin symmetry and pseudospin symmetry for arbitrary spin–orbit number [Formula: see text], an appropriate approximation employed on the centrifugal terms in the symmetries of three-dimensional extended relativistic quantum mechanics (3D-ERQM). This potential is a superposition of Manning–Rosen plus quasi-Hellman potentials and some other exponential terms. Through the application of both new approximations to deal with the centrifugal term, Bopp’s shift method and the independent-time perturbation theory method, the recent modified approximate energy corrections under IMRQHPs are obtained for nuclei [Formula: see text]O and [Formula: see text]F and (O2, I2, N2, H2, LiH, CO and NO) diatomic molecules in 3D-ERQM and three-dimensional extended non-relativistic quantum mechanics (3D-ENRQM) symmetries. The recent values that we get appear sensitive to [Formula: see text], which are known as the discrete atomic quantum numbers, the mixed potential depths ([Formula: see text], [Formula: see text]) and [Formula: see text], the range of the potential [Formula: see text] and non-commutativity parameters [Formula: see text]. In both 3D-ERQM and 3D-ENRQM symmetries, we show that the recent corrections obtained on the new bound states under IMRQHPs are infinitesimal to the principal part of energy in the ordinary cases of 3D-RQM and 3D-NRQM symmetries. In the new symmetries of 3D-ERQM symmetries, it is not possible to get the exact analytical solutions [Formula: see text] and [Formula: see text], only the approximate solutions are possible. In addition, we discussed in detail the non-relativistic study of the studied mixed potentials. Four special cases, i.e. we investigated some special cases in the context of modified Schrödinger theories. In the framework of known relativistic quantum mechanics, we have clearly demonstrated that the modified Schrödinger equation can be represented as the Dirac equation under the influence of IMRQHPs.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"373 1","pages":""},"PeriodicalIF":1.4,"publicationDate":"2023-12-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138983175","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 : 2023-12-09DOI: 10.1142/s0217732323501675
Riccardo Fantoni
We prove through path integral Monte Carlo that the covariant Euclidean scalar field theory, [Formula: see text], where [Formula: see text] denotes the power of the interaction term and [Formula: see text] with [Formula: see text] as the spatial dimension and 1 adds imaginary time, such that [Formula: see text], [Formula: see text] can be acceptably quantized using scaled affine quantization (AQ) and the resulting theory is nontrivial, unlike what happens using canonical quantization which finds it trivial.
{"title":"Scaled affine quantization of φ312 is nontrivial","authors":"Riccardo Fantoni","doi":"10.1142/s0217732323501675","DOIUrl":"https://doi.org/10.1142/s0217732323501675","url":null,"abstract":"We prove through path integral Monte Carlo that the covariant Euclidean scalar field theory, [Formula: see text], where [Formula: see text] denotes the power of the interaction term and [Formula: see text] with [Formula: see text] as the spatial dimension and 1 adds imaginary time, such that [Formula: see text], [Formula: see text] can be acceptably quantized using scaled affine quantization (AQ) and the resulting theory is nontrivial, unlike what happens using canonical quantization which finds it trivial.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"271 1","pages":""},"PeriodicalIF":1.4,"publicationDate":"2023-12-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138983150","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 : 2023-12-09DOI: 10.1142/s0217732323501717
M. Ilyas, A. R. Athar
In this paper, we introduced the deceleration parameter [Formula: see text] in a different manner by proposing a modern law. According to this law, we suggested a time-periodic [Formula: see text]. Furthermore, we used this law to develop a model in which the universe oscillates with quintom matter in a four-dimensional FLRW metric background. Using this model, we obtained the oscillating Hubble parameter [Formula: see text], which remains positive. Consequently, the universe undergoes decelerating expansion and accelerating expansion periodically, avoiding singularities.
{"title":"Oscillating quintom scenario with time-dependent periodic deceleration parameter","authors":"M. Ilyas, A. R. Athar","doi":"10.1142/s0217732323501717","DOIUrl":"https://doi.org/10.1142/s0217732323501717","url":null,"abstract":"In this paper, we introduced the deceleration parameter [Formula: see text] in a different manner by proposing a modern law. According to this law, we suggested a time-periodic [Formula: see text]. Furthermore, we used this law to develop a model in which the universe oscillates with quintom matter in a four-dimensional FLRW metric background. Using this model, we obtained the oscillating Hubble parameter [Formula: see text], which remains positive. Consequently, the universe undergoes decelerating expansion and accelerating expansion periodically, avoiding singularities.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"381 1","pages":""},"PeriodicalIF":1.4,"publicationDate":"2023-12-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138983169","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 : 2023-11-29DOI: 10.1142/s021773232350150x
M. K. Dutta, G. Biswas, B. Modak
In this paper, we present some analytical solutions of wormhole in four-dimensional Robertson–Walker Euclidean background considering Einstein–Gauss–Bonnet dilaton interaction with a [Formula: see text]-essence field for [Formula: see text]. The solutions are obtained assuming some restrictions on coupling function with a form of potential or with the ratio of kinetic to potential energy of the dilaton field. Euclidean wormhole, in one case, evolves through early transient inflationary era and after graceful exit from inflation, it asymptotically yields a radiation dominated era or a matter dominated era. In another solution, initial Euclidean wormhole is accompanied by oscillation of scale factor in Euclidean time at some late era which asymptotically yields exponential expansion. The violation of the null energy condition can be avoided asymptotically. The potential is also found to decay sharply.
{"title":"Euclidean Wormhole with k-essence field in the presence of Gauss–Bonnet term","authors":"M. K. Dutta, G. Biswas, B. Modak","doi":"10.1142/s021773232350150x","DOIUrl":"https://doi.org/10.1142/s021773232350150x","url":null,"abstract":"In this paper, we present some analytical solutions of wormhole in four-dimensional Robertson–Walker Euclidean background considering Einstein–Gauss–Bonnet dilaton interaction with a [Formula: see text]-essence field for [Formula: see text]. The solutions are obtained assuming some restrictions on coupling function with a form of potential or with the ratio of kinetic to potential energy of the dilaton field. Euclidean wormhole, in one case, evolves through early transient inflationary era and after graceful exit from inflation, it asymptotically yields a radiation dominated era or a matter dominated era. In another solution, initial Euclidean wormhole is accompanied by oscillation of scale factor in Euclidean time at some late era which asymptotically yields exponential expansion. The violation of the null energy condition can be avoided asymptotically. The potential is also found to decay sharply.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"18 1","pages":""},"PeriodicalIF":1.4,"publicationDate":"2023-11-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139213829","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 : 2023-11-27DOI: 10.1142/s0217732323920025
M. Boboqambarova, B. Turimov, A. Abdujabbarov
{"title":"Erratum: Particle motion around Schwarzschild-MOG black hole","authors":"M. Boboqambarova, B. Turimov, A. Abdujabbarov","doi":"10.1142/s0217732323920025","DOIUrl":"https://doi.org/10.1142/s0217732323920025","url":null,"abstract":"","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"1 1","pages":""},"PeriodicalIF":1.4,"publicationDate":"2023-11-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139229391","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 : 2023-11-25DOI: 10.1142/s0217732323501183
Yuanyuan Liu, J. Manafian, K. Mahmoud, Baharak Eslami
In this paper, the M-lump solutions, the periodic type, and cross-kink wave solutions are acquired. Here, the Hirota bilinear operator is employed. By utilizing the symbolic computation and employing the utilized method, the (3+1)-dimensional Jimbo–Miwa (JM) equation is investigated. Based on the Hirota bilinear form, the soliton solution and periodic wave solution to the mentioned equation, respectively, are obtained. We gained plenty of multiple collisions of lumps. Next, the periodic wave and cross-kink wave have greatly enriched the existing literature on the JM equation. Through the three-dimensional designs, contour design, density design, and two-dimensional design by using Maple, the physical features of these soliton solutions are explained all right. The forms of the attained solutions are one-lump, two-lumps, and three-lumps wave solutions. Then, a class of rogue waves-type solutions to the (3+1)-dimensional JM equation within the frame of the bilinear equation is found. These results can help us better understand interesting physical phenomena and mechanisms.
本文获得了 M-lump 解法、周期型解法和交叉扭结波解法。这里使用了 Hirota 双线性算子。通过利用符号计算和所使用的方法，研究了 (3+1)-dimensional Jimbo-Miwa (JM) 方程。基于 Hirota 双线性形式，分别得到了上述方程的孤子解和周期波解。我们获得了大量块体的多重碰撞。接下来，周期波和交叉扭结波极大地丰富了有关 JM 方程的现有文献。通过使用 Maple 进行三维设计、轮廓设计、密度设计和二维设计，这些孤子解的物理特征得到了很好的解释。所得到的解的形式有一凸块波、二凸块波和三凸块波。然后，在双线性方程的框架内找到了 (3+1)-dimensional JM 方程的一类流氓波型解。这些结果有助于我们更好地理解有趣的物理现象和机制。
{"title":"On soliton solutions, periodic wave solutions, asymptotic analysis and interaction phenomena of the (3+1)-dimensional JM equation","authors":"Yuanyuan Liu, J. Manafian, K. Mahmoud, Baharak Eslami","doi":"10.1142/s0217732323501183","DOIUrl":"https://doi.org/10.1142/s0217732323501183","url":null,"abstract":"In this paper, the M-lump solutions, the periodic type, and cross-kink wave solutions are acquired. Here, the Hirota bilinear operator is employed. By utilizing the symbolic computation and employing the utilized method, the (3+1)-dimensional Jimbo–Miwa (JM) equation is investigated. Based on the Hirota bilinear form, the soliton solution and periodic wave solution to the mentioned equation, respectively, are obtained. We gained plenty of multiple collisions of lumps. Next, the periodic wave and cross-kink wave have greatly enriched the existing literature on the JM equation. Through the three-dimensional designs, contour design, density design, and two-dimensional design by using Maple, the physical features of these soliton solutions are explained all right. The forms of the attained solutions are one-lump, two-lumps, and three-lumps wave solutions. Then, a class of rogue waves-type solutions to the (3+1)-dimensional JM equation within the frame of the bilinear equation is found. These results can help us better understand interesting physical phenomena and mechanisms.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"1 1","pages":""},"PeriodicalIF":1.4,"publicationDate":"2023-11-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139236475","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 : 2023-11-23DOI: 10.1142/s0217732323501559
Guangpu Lou, Jianwei Dong
In this paper, we study the analytical solutions to the isentropic Euler system with the logarithmic equation of state, which has been introduced for the dark energy fluid to investigate the dynamical evolution of a late-time universe. By using some ansatz, we construct some analytical solutions for one-dimensional case, [Formula: see text]-dimensional radially symmetric case and three-dimensional cylindrically symmetric case, respectively. The concentration and cavitation phenomena are investigated and some global analytical solutions are obtained under some conditions.
{"title":"Analytical solutions to the isentropic Euler system with the logarithmic equation of state","authors":"Guangpu Lou, Jianwei Dong","doi":"10.1142/s0217732323501559","DOIUrl":"https://doi.org/10.1142/s0217732323501559","url":null,"abstract":"In this paper, we study the analytical solutions to the isentropic Euler system with the logarithmic equation of state, which has been introduced for the dark energy fluid to investigate the dynamical evolution of a late-time universe. By using some ansatz, we construct some analytical solutions for one-dimensional case, [Formula: see text]-dimensional radially symmetric case and three-dimensional cylindrically symmetric case, respectively. The concentration and cavitation phenomena are investigated and some global analytical solutions are obtained under some conditions.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"64 2","pages":""},"PeriodicalIF":1.4,"publicationDate":"2023-11-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139244137","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 : 2023-11-22DOI: 10.1142/s0217732323501584
Chun-Zao Zhang, Hong-Yi Fan
For two operators [Formula: see text] and [Formula: see text] which obey [Formula: see text]we shall prove [Formula: see text]which means we want to merge two exponential operators’ product into one exponential operator. This kind of operator identity is useful for calculating the quantum entropy [Formula: see text] since [Formula: see text] when [Formula: see text] but [Formula: see text] thus the merging operator formula is demanded. In this way, several exponential operators’ product can also be merged. We shall employ the method of integration within normally ordered product (IWOP) to derive the merging operator identity.
{"title":"New method for merging several exponential operators’ product into one exponential operator","authors":"Chun-Zao Zhang, Hong-Yi Fan","doi":"10.1142/s0217732323501584","DOIUrl":"https://doi.org/10.1142/s0217732323501584","url":null,"abstract":"For two operators [Formula: see text] and [Formula: see text] which obey [Formula: see text]we shall prove [Formula: see text]which means we want to merge two exponential operators’ product into one exponential operator. This kind of operator identity is useful for calculating the quantum entropy [Formula: see text] since [Formula: see text] when [Formula: see text] but [Formula: see text] thus the merging operator formula is demanded. In this way, several exponential operators’ product can also be merged. We shall employ the method of integration within normally ordered product (IWOP) to derive the merging operator identity.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"629 ","pages":""},"PeriodicalIF":1.4,"publicationDate":"2023-11-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139248420","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 : 2023-11-22DOI: 10.1142/s0217732323501535
Himanshu Kumar Sudhanshu, S. Upadhyay, D. Singh, Y. Myrzakulov, K. Myrzakulov
In this paper, we provide a thermodynamical study of charged accelerating AdS black holes in the [Formula: see text]-metric. In this connection, we first determine the mass of the given black hole and study their dependence on horizon radius and acceleration. Furthermore, following black hole mechanics, we also derive various quantities like Hawking temperature, entropy, pressure, volume, internal energy, Gibbs energy and Helmholtz energy. With the help of a graph, we study the effect of acceleration on these thermal quantities. Here, we observe that the impact of acceleration becomes more significant on the large horizons. To discuss stability and phase transition, we calculate specific heat. The graphical analysis suggests multiple phase transitions occur for the charged accelerating black hole in AdS spacetime. The system changes state at the critical point, where phase transition occurs. For the small black holes, the critical point at which the phase transition occurs is independent of the acceleration parameter. However, the critical horizon radius for large black holes depends on the acceleration parameter. For fast-accelerating black holes, a phase transition occurs at a small horizon radius to that of slowly accelerating black holes.
{"title":"Thermodynamics of charged accelerating AdS black hole","authors":"Himanshu Kumar Sudhanshu, S. Upadhyay, D. Singh, Y. Myrzakulov, K. Myrzakulov","doi":"10.1142/s0217732323501535","DOIUrl":"https://doi.org/10.1142/s0217732323501535","url":null,"abstract":"In this paper, we provide a thermodynamical study of charged accelerating AdS black holes in the [Formula: see text]-metric. In this connection, we first determine the mass of the given black hole and study their dependence on horizon radius and acceleration. Furthermore, following black hole mechanics, we also derive various quantities like Hawking temperature, entropy, pressure, volume, internal energy, Gibbs energy and Helmholtz energy. With the help of a graph, we study the effect of acceleration on these thermal quantities. Here, we observe that the impact of acceleration becomes more significant on the large horizons. To discuss stability and phase transition, we calculate specific heat. The graphical analysis suggests multiple phase transitions occur for the charged accelerating black hole in AdS spacetime. The system changes state at the critical point, where phase transition occurs. For the small black holes, the critical point at which the phase transition occurs is independent of the acceleration parameter. However, the critical horizon radius for large black holes depends on the acceleration parameter. For fast-accelerating black holes, a phase transition occurs at a small horizon radius to that of slowly accelerating black holes.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"33 4","pages":""},"PeriodicalIF":1.4,"publicationDate":"2023-11-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139249825","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 : 2023-11-22DOI: 10.1142/s0217732323501560
Coskun Aydin
By using the minimal extension of the standard model and considering the general relativistic effects near the surface of a static neutron star in the presence of quintessence fields, we drive analytical expressions for the cross-section and energy deposition rate of the process ([Formula: see text]). We have also obtained the ratio of energy deposition to total Newtonian energy deposition ([Formula: see text]). We have displayed that the contributions of the electron neutrino’s charge radius are more effective than the dipole moment in this process. The obtained solutions indicate that the contribution of the electron neutrino charge radius changes the results approximately (1–5)% depending on the [Formula: see text] value of the star.
{"title":"Energy deposition rate for neutrino pair annihilation in the presence of quintessence near neutron star","authors":"Coskun Aydin","doi":"10.1142/s0217732323501560","DOIUrl":"https://doi.org/10.1142/s0217732323501560","url":null,"abstract":"By using the minimal extension of the standard model and considering the general relativistic effects near the surface of a static neutron star in the presence of quintessence fields, we drive analytical expressions for the cross-section and energy deposition rate of the process ([Formula: see text]). We have also obtained the ratio of energy deposition to total Newtonian energy deposition ([Formula: see text]). We have displayed that the contributions of the electron neutrino’s charge radius are more effective than the dipole moment in this process. The obtained solutions indicate that the contribution of the electron neutrino charge radius changes the results approximately (1–5)% depending on the [Formula: see text] value of the star.","PeriodicalId":18752,"journal":{"name":"Modern Physics Letters A","volume":"1 1","pages":""},"PeriodicalIF":1.4,"publicationDate":"2023-11-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139249034","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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