Pub Date : 2025-02-01DOI: 10.1016/j.nuclphysb.2025.116808
Leon J. Sieke , Mattis Harhoff , Sören Schlichting , Lorenz von Smekal
We study the critical dynamics of a scalar field theory with symmetry in the dynamic universality class of Model A in two and three spatial dimensions with classical-statistical lattice simulations. In particular, we measure the non-equilibrium behavior of the system under a quench protocol in which the symmetry-breaking external field is changed at a constant rate through the critical point. Using the well-established Kibble-Zurek scaling theory we compute non-equilibrium scaling functions of cumulants of the order parameter up to fourth order. Together with the static critical exponents and the dynamic critical exponent, these fully describe the universal non-equilibrium evolution of the system near the critical point. We further extend the analysis to include finite-size effects and observe good collapse of our data onto two-dimensional universal non-equilibrium and finite-size scaling functions.
{"title":"Universal non-equilibrium scaling of cumulants across a critical point","authors":"Leon J. Sieke , Mattis Harhoff , Sören Schlichting , Lorenz von Smekal","doi":"10.1016/j.nuclphysb.2025.116808","DOIUrl":"10.1016/j.nuclphysb.2025.116808","url":null,"abstract":"<div><div>We study the critical dynamics of a scalar field theory with <span><math><msub><mrow><mi>Z</mi></mrow><mrow><mn>2</mn></mrow></msub></math></span> symmetry in the dynamic universality class of Model A in two and three spatial dimensions with classical-statistical lattice simulations. In particular, we measure the non-equilibrium behavior of the system under a quench protocol in which the symmetry-breaking external field is changed at a constant rate through the critical point. Using the well-established Kibble-Zurek scaling theory we compute non-equilibrium scaling functions of cumulants of the order parameter up to fourth order. Together with the static critical exponents and the dynamic critical exponent, these fully describe the universal non-equilibrium evolution of the system near the critical point. We further extend the analysis to include finite-size effects and observe good collapse of our data onto two-dimensional universal non-equilibrium and finite-size scaling functions.</div></div>","PeriodicalId":54712,"journal":{"name":"Nuclear Physics B","volume":"1011 ","pages":"Article 116808"},"PeriodicalIF":2.5,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143177376","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-02-01DOI: 10.1016/j.nuclphysb.2024.116789
Sangeeta Dey, Mahadev Patgiri
In this work, we carry out a systematic investigation of thirty six possible structures of neutrino mass matrix, having textures of one zero element and one vanishing sub-trace taking the latest 3σ neutrino data. Correlation plots of the ratio of solar to atmospheric mass splittings, and the Dirac CP phase, δ for each texture are examined and found only fourteen textures phenomenologically viable with 3σ range. The restricted ranges of δ for allowed textures are used to predict theoretically the Majorana CP Phases (α and β) which are yet to be measured experimentally. With these results, we also calculate the Majorana mass term, on which the neutrinoless double beta decay rate depends, and the Jarlskog invariant, for the strength of CP violation and also study the correlations between the CP phases and the mixing angle . Besides them, we also checked the experimental compatibilities for the parameters effective electron neutrino mass , total ‘sum’ of neutrino masses, . The consistency of mass orderings of textures is checked with , and phenomenological identification of textures having no octant degeneracy for is done. Finally, the flavor symmetry realization of textures is done under the symmetry group, in Type II seesaw mechanism.
{"title":"Study of texture zero neutrino models with vanishing sub-trace and their flavor structures","authors":"Sangeeta Dey, Mahadev Patgiri","doi":"10.1016/j.nuclphysb.2024.116789","DOIUrl":"10.1016/j.nuclphysb.2024.116789","url":null,"abstract":"<div><div>In this work, we carry out a systematic investigation of thirty six possible structures of neutrino mass matrix, <span><math><msub><mrow><mi>M</mi></mrow><mrow><mi>ν</mi></mrow></msub></math></span> having textures of one zero element and one vanishing sub-trace taking the latest 3<em>σ</em> neutrino data. Correlation plots of the ratio of solar to atmospheric mass splittings, <span><math><msub><mrow><mi>R</mi></mrow><mrow><mi>ν</mi></mrow></msub></math></span> and the Dirac CP phase, <em>δ</em> for each texture are examined and found only fourteen textures phenomenologically viable with 3<em>σ</em> range. The restricted ranges of <em>δ</em> for allowed textures are used to predict theoretically the Majorana CP Phases (<em>α</em> and <em>β</em>) which are yet to be measured experimentally. With these results, we also calculate the Majorana mass term, <span><math><mo>|</mo><msub><mrow><mi>m</mi></mrow><mrow><mi>e</mi><mi>e</mi></mrow></msub><mo>|</mo></math></span> on which the neutrinoless double beta decay rate depends, and the Jarlskog invariant, <span><math><msub><mrow><mi>J</mi></mrow><mrow><mi>c</mi><mi>p</mi></mrow></msub></math></span> for the strength of CP violation and also study the correlations between the CP phases and the mixing angle <span><math><msub><mrow><mi>θ</mi></mrow><mrow><mn>23</mn></mrow></msub></math></span>. Besides them, we also checked the experimental compatibilities for the parameters effective electron neutrino mass <span><math><msub><mrow><mi>m</mi></mrow><mrow><msub><mrow><mi>ν</mi></mrow><mrow><mi>e</mi></mrow></msub></mrow></msub></math></span>, total ‘sum’ of neutrino masses, <span><math><msub><mrow><mi>Σ</mi></mrow><mrow><mi>ν</mi></mrow></msub></math></span>. The consistency of mass orderings of textures is checked with <span><math><mfrac><mrow><msub><mrow><mi>m</mi></mrow><mrow><mn>3</mn></mrow></msub></mrow><mrow><msub><mrow><mi>m</mi></mrow><mrow><mn>1</mn></mrow></msub></mrow></mfrac></math></span>, and phenomenological identification of textures having no octant degeneracy for <span><math><msub><mrow><mi>θ</mi></mrow><mrow><mn>23</mn></mrow></msub></math></span> is done. Finally, the flavor symmetry realization of textures is done under the symmetry group, <span><math><msub><mrow><mi>S</mi></mrow><mrow><mn>3</mn></mrow></msub><mo>×</mo><msub><mrow><mi>Z</mi></mrow><mrow><mn>4</mn></mrow></msub></math></span> in Type II seesaw mechanism.</div></div>","PeriodicalId":54712,"journal":{"name":"Nuclear Physics B","volume":"1011 ","pages":"Article 116789"},"PeriodicalIF":2.5,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143177401","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-02-01DOI: 10.1016/j.nuclphysb.2025.116806
Faizuddin Ahmed , Ahmad Al-Badawi , İzzet Sakallı , Abdelmalek Bouzenada
This paper aims to explore the quasinormal modes (QNMs) and effective potential profiles of massless and rotating BTZ black holes within the frameworks of and Ricci-Inverse () modified gravity theories, which, while producing similar space-time structures, exhibit variations due to distinct cosmological constants, . We derive wave equations for these black hole perturbations and analyze the behavior of the effective potential under different values of mass m, cosmological constant , and modified gravity parameters , , , , and γ. The findings indicate that increasing mass and parameter values results in a raised potential barrier, implying stronger confinement of perturbations and impacting black hole stability. Incorporating the generalized uncertainty principle, we also study its effect on the thermodynamics of rotating BTZ black holes, demonstrating how GUP modifies black hole radiation, potentially observable in QNM decay rates. Additionally, we investigate the motion of particles through null and timelike geodesics in static BTZ space-time, observing asymptotic behaviors for null geodesics and parameter-dependent shifts in potential for timelike paths. The study concludes that modified gravity parameters significantly influence QNM frequencies and effective potential profiles, offering insights into black hole stability and suggesting that these theoretical predictions may be tested through gravitational wave observations.
{"title":"Quasinormal modes and GUP-corrected Hawking radiation of BTZ black holes within modified gravity frameworks","authors":"Faizuddin Ahmed , Ahmad Al-Badawi , İzzet Sakallı , Abdelmalek Bouzenada","doi":"10.1016/j.nuclphysb.2025.116806","DOIUrl":"10.1016/j.nuclphysb.2025.116806","url":null,"abstract":"<div><div>This paper aims to explore the quasinormal modes (QNMs) and effective potential profiles of massless and rotating BTZ black holes within the frameworks of <span><math><mi>f</mi><mo>(</mo><mi>R</mi><mo>)</mo></math></span> and Ricci-Inverse (<span><math><mi>RI</mi></math></span>) modified gravity theories, which, while producing similar space-time structures, exhibit variations due to distinct cosmological constants, <span><math><msub><mrow><mi>Λ</mi></mrow><mrow><mi>m</mi></mrow></msub></math></span>. We derive wave equations for these black hole perturbations and analyze the behavior of the effective potential <span><math><msub><mrow><mi>V</mi></mrow><mrow><mtext>eff</mtext></mrow></msub><mo>(</mo><mi>r</mi><mo>)</mo></math></span> under different values of mass <em>m</em>, cosmological constant <span><math><msub><mrow><mi>Λ</mi></mrow><mrow><mi>m</mi></mrow></msub></math></span>, and modified gravity parameters <span><math><msub><mrow><mi>α</mi></mrow><mrow><mn>1</mn></mrow></msub></math></span>, <span><math><msub><mrow><mi>α</mi></mrow><mrow><mn>2</mn></mrow></msub></math></span>, <span><math><msub><mrow><mi>β</mi></mrow><mrow><mn>1</mn></mrow></msub></math></span>, <span><math><msub><mrow><mi>β</mi></mrow><mrow><mn>2</mn></mrow></msub></math></span>, and <em>γ</em>. The findings indicate that increasing mass and parameter values results in a raised potential barrier, implying stronger confinement of perturbations and impacting black hole stability. Incorporating the generalized uncertainty principle, we also study its effect on the thermodynamics of rotating BTZ black holes, demonstrating how GUP modifies black hole radiation, potentially observable in QNM decay rates. Additionally, we investigate the motion of particles through null and timelike geodesics in static BTZ space-time, observing asymptotic behaviors for null geodesics and parameter-dependent shifts in potential for timelike paths. The study concludes that modified gravity parameters significantly influence QNM frequencies and effective potential profiles, offering insights into black hole stability and suggesting that these theoretical predictions may be tested through gravitational wave observations.</div></div>","PeriodicalId":54712,"journal":{"name":"Nuclear Physics B","volume":"1011 ","pages":"Article 116806"},"PeriodicalIF":2.5,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143176938","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-02-01DOI: 10.1016/j.nuclphysb.2025.116802
Ankit Das , Sarthak Duary , Utpal Sarkar
We explore the possibility of B and violating processes, specifically proton decay and neutron-antineutron oscillation, using explicit realization of operators in the grand unified theory with an orbifold space.
{"title":"n−n‾ oscillation in S1/Z2×Z2′ orbifold SU(5) GUT","authors":"Ankit Das , Sarthak Duary , Utpal Sarkar","doi":"10.1016/j.nuclphysb.2025.116802","DOIUrl":"10.1016/j.nuclphysb.2025.116802","url":null,"abstract":"<div><div>We explore the possibility of <em>B</em> and <span><math><mi>B</mi><mo>−</mo><mi>L</mi></math></span> violating processes, specifically proton decay and neutron-antineutron oscillation, using explicit realization of operators in the <span><math><mi>S</mi><mi>U</mi><mo>(</mo><mn>5</mn><mo>)</mo></math></span> grand unified theory with an <span><math><msup><mrow><mi>S</mi></mrow><mrow><mn>1</mn></mrow></msup><mo>/</mo><msub><mrow><mi>Z</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>×</mo><msubsup><mrow><mi>Z</mi></mrow><mrow><mn>2</mn></mrow><mrow><mo>′</mo></mrow></msubsup></math></span> orbifold space.</div></div>","PeriodicalId":54712,"journal":{"name":"Nuclear Physics B","volume":"1011 ","pages":"Article 116802"},"PeriodicalIF":2.5,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143177402","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-02-01DOI: 10.1016/j.nuclphysb.2025.116794
N.S. Kavya, C.S. Varsha, L. Sudharani, V. Venkatesha
A Casimir wormhole is a theoretical concept proposing the negative energy density, generated through the Casimir effect that could support the existence of a traversable wormhole. This article investigates the feasibility of a Casimir wormhole by unifying the Casimir effect and non-commutative geometry within the framework of gravity theory using Lorentzian distribution. In this study, we derive the shape function satisfying the throat condition and graphically verify all necessary conditions for a traversable wormhole by varying the gravitational mass μ. In addition to this we examine all the energy conditions and physical properties, to assess the wormhole's stability.
{"title":"Unifying non-commutative geometry with Casimir energy: A novel f(R) wormhole solution","authors":"N.S. Kavya, C.S. Varsha, L. Sudharani, V. Venkatesha","doi":"10.1016/j.nuclphysb.2025.116794","DOIUrl":"10.1016/j.nuclphysb.2025.116794","url":null,"abstract":"<div><div>A Casimir wormhole is a theoretical concept proposing the negative energy density, generated through the Casimir effect that could support the existence of a traversable wormhole. This article investigates the feasibility of a Casimir wormhole by unifying the Casimir effect and non-commutative geometry within the framework of <span><math><mi>f</mi><mo>(</mo><mi>R</mi><mo>)</mo></math></span> gravity theory using Lorentzian distribution. In this study, we derive the shape function satisfying the throat condition and graphically verify all necessary conditions for a traversable wormhole by varying the gravitational mass <em>μ</em>. In addition to this we examine all the energy conditions and physical properties, to assess the wormhole's stability.</div></div>","PeriodicalId":54712,"journal":{"name":"Nuclear Physics B","volume":"1011 ","pages":"Article 116794"},"PeriodicalIF":2.5,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143176962","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-02-01DOI: 10.1016/j.nuclphysb.2025.116798
Ya-Hui Liu, Rui Guo, Jian-Wen Zhang
In this paper, we develop the inverse scattering transform for an inhomogeneous time shifted nonlocal lattice equation, also known as the inhomogeneous discrete time shifted nonlocal nonlinear Schrödinger equation, and obtain the multi-type soliton solutions under zero boundary condition. According to the analyticity, asymptotic behavior and symmetries of eigenfunctions and scattering coefficients as well as the distribution of discrete eigenvalues, the Riemann-Hilbert problem is constructed and solved and the reconstruction formula of potential used to construct soliton solutions under the reflectionless condition is derived. Specially, according to the time shifted nonlocal condition, we deduce the specific constraint on the real function in the equation, which is a constraint on the time evolution of the scattering coefficients and eigenfunctions.
{"title":"Inverse scattering transform for an integrable inhomogeneous time shifted nonlocal lattice","authors":"Ya-Hui Liu, Rui Guo, Jian-Wen Zhang","doi":"10.1016/j.nuclphysb.2025.116798","DOIUrl":"10.1016/j.nuclphysb.2025.116798","url":null,"abstract":"<div><div>In this paper, we develop the inverse scattering transform for an inhomogeneous time shifted nonlocal lattice equation, also known as the inhomogeneous discrete time shifted nonlocal nonlinear Schrödinger equation, and obtain the multi-type soliton solutions under zero boundary condition. According to the analyticity, asymptotic behavior and symmetries of eigenfunctions and scattering coefficients as well as the distribution of discrete eigenvalues, the Riemann-Hilbert problem is constructed and solved and the reconstruction formula of potential used to construct soliton solutions under the reflectionless condition is derived. Specially, according to the time shifted nonlocal condition, we deduce the specific constraint on the real function <span><math><mi>γ</mi><mo>(</mo><mi>t</mi><mo>)</mo></math></span> in the equation, which is a constraint on the time evolution of the scattering coefficients and eigenfunctions.</div></div>","PeriodicalId":54712,"journal":{"name":"Nuclear Physics B","volume":"1011 ","pages":"Article 116798"},"PeriodicalIF":2.5,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143176937","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-02-01DOI: 10.1016/j.nuclphysb.2025.116797
S. Rastgoo, F. Parsaei
In this work, we introduce a novel set of asymptotically flat wormhole solutions within the framework of theory of gravity. Considering a linear form, we show that a wide variety of wormhole solutions with asymptotically linear equation of state exist. Our solutions satisfy all the energy conditions, namely the null, weak, strong and dominant energy conditions. The relationship between free parameters in the shape function and boundary conditions is analyzed.
{"title":"Wormholes in f(R,T) gravity with variable equation of state","authors":"S. Rastgoo, F. Parsaei","doi":"10.1016/j.nuclphysb.2025.116797","DOIUrl":"10.1016/j.nuclphysb.2025.116797","url":null,"abstract":"<div><div>In this work, we introduce a novel set of asymptotically flat wormhole solutions within the framework of <span><math><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><mi>T</mi><mo>)</mo></math></span> theory of gravity. Considering a linear <span><math><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><mi>T</mi><mo>)</mo><mo>=</mo><mi>R</mi><mo>+</mo><mn>2</mn><mi>λ</mi><mi>T</mi></math></span> form, we show that a wide variety of wormhole solutions with asymptotically linear equation of state exist. Our solutions satisfy all the energy conditions, namely the null, weak, strong and dominant energy conditions. The relationship between free parameters in the shape function and boundary conditions is analyzed.</div></div>","PeriodicalId":54712,"journal":{"name":"Nuclear Physics B","volume":"1011 ","pages":"Article 116797"},"PeriodicalIF":2.5,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143176939","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-02-01DOI: 10.1016/j.nuclphysb.2024.116790
Feri Apryandi , M. Lawrence Pattersons
The mass of galaxy clusters (GCs) can be determined by calculating the hydrostatic equilibrium equation. In this work, we derive the hydrostatic mass of GCs within Eddington-inspired Born-Infeld (EiBI) theory, beyond Horndeski gravity (BHG), and modified emergent Newtonian gravity (MENG) with generalized uncertainty principle (GUP) correction. We apply the formulations on the masses of 10 GCs. We compare our results with the Newtonian mass of GCs. Within a regime, we get an insight that all formulations could match the Newtonian mass. Thus, the impact of the modified theories of gravity used in this work can be neglected in this regime. The noteworthy impact starts if we set m2 for EiBI theory, for BHG, and for MENG. We also compare our results from EiBI theory and BHG with the baryonic masses of the GCs. A better linear fit is achieved by EiBI theory with m2, which gives the slope of . This value is closer to unity than the one of BHG. This leads us to the fact that EiBI theory is more effective than BHG in alleviating the mass discrepancy between hydrostatic mass and baryonic mass in GCs. Nevertheless, neither EiBI theory nor BHG completely addresses the mass discrepancy problem.
{"title":"Hydrostatic mass of galaxy clusters within some theories of gravity","authors":"Feri Apryandi , M. Lawrence Pattersons","doi":"10.1016/j.nuclphysb.2024.116790","DOIUrl":"10.1016/j.nuclphysb.2024.116790","url":null,"abstract":"<div><div>The mass of galaxy clusters (GCs) can be determined by calculating the hydrostatic equilibrium equation. In this work, we derive the hydrostatic mass of GCs within Eddington-inspired Born-Infeld (EiBI) theory, beyond Horndeski gravity (BHG), and modified emergent Newtonian gravity (MENG) with generalized uncertainty principle (GUP) correction. We apply the formulations on the masses of 10 GCs. We compare our results with the Newtonian mass of GCs. Within a regime, we get an insight that all formulations could match the Newtonian mass. Thus, the impact of the modified theories of gravity used in this work can be neglected in this regime. The noteworthy impact starts if we set <span><math><mi>κ</mi><mo>=</mo><mn>5</mn><mo>×</mo><msup><mrow><mn>10</mn></mrow><mrow><mn>40</mn></mrow></msup></math></span> m<sup>2</sup> for EiBI theory, <span><math><mi>ϒ</mi><mo>=</mo><mo>−</mo><mn>0.1655</mn><mo>×</mo><msup><mrow><mn>10</mn></mrow><mrow><mn>69</mn></mrow></msup></math></span> for BHG, and <span><math><msub><mrow><mi>β</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mo>−</mo><mn>1.656</mn><mo>×</mo><msup><mrow><mn>10</mn></mrow><mrow><mn>110</mn></mrow></msup></math></span> for MENG. We also compare our results from EiBI theory and BHG with the baryonic masses <span><math><msub><mrow><mi>M</mi></mrow><mrow><mi>b</mi><mi>a</mi><mi>r</mi></mrow></msub></math></span> of the GCs. A better linear fit is achieved by EiBI theory with <span><math><mi>κ</mi><mo>=</mo><mn>5.80</mn><mo>×</mo><msup><mrow><mn>10</mn></mrow><mrow><mn>40</mn></mrow></msup></math></span> m<sup>2</sup>, which gives the slope <span><math><mi>M</mi></math></span> of <span><math><mn>0.126</mn><mo>±</mo><mn>0.086</mn></math></span>. This value is closer to unity than the one of BHG. This leads us to the fact that EiBI theory is more effective than BHG in alleviating the mass discrepancy between hydrostatic mass and baryonic mass in GCs. Nevertheless, neither EiBI theory nor BHG completely addresses the mass discrepancy problem.</div></div>","PeriodicalId":54712,"journal":{"name":"Nuclear Physics B","volume":"1011 ","pages":"Article 116790"},"PeriodicalIF":2.5,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143177374","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The nonextensive nature of black holes is one of the most intriguing discoveries. In fact, the black hole entropy is a nonextensive quantity that scales by its surface area at the event horizon. In our work, we extend the thermodynamic phase space of black holes by treating the nonextensive parameter analyzed via the Rényi entropy as the thermodynamic variable. Using Euler's theorem for a homogeneous function of the black holes' mass, the compatible Smarr formula and the first law of black hole thermodynamics can be obtained. It is also demonstrated that, by keeping the same form of the black hole mass, the Rényi temperature is straightforwardly defined as proposed in the literature. Since many different types of black holes can indeed be successfully treated with such a procedure, our consideration is fairly general. It is worthwhile to argue that the black hole thermodynamics in Rényi statistics is rooted from the relation among geometric quantities in the same way as the standard approach corresponding to the Gibbs–Boltzmann statistics. Even though our results are based on classical gravity, they may pave the way to derive the Rényi temperature using the notion of quantum field in curved spacetime.
{"title":"Thermodynamics of black holes with Rényi entropy from classical gravity","authors":"Ratchaphat Nakarachinda , Chatchai Promsiri , Lunchakorn Tannukij , Pitayuth Wongjun","doi":"10.1016/j.nuclphysb.2025.116796","DOIUrl":"10.1016/j.nuclphysb.2025.116796","url":null,"abstract":"<div><div>The nonextensive nature of black holes is one of the most intriguing discoveries. In fact, the black hole entropy is a nonextensive quantity that scales by its surface area at the event horizon. In our work, we extend the thermodynamic phase space of black holes by treating the nonextensive parameter analyzed via the Rényi entropy as the thermodynamic variable. Using Euler's theorem for a homogeneous function of the black holes' mass, the compatible Smarr formula and the first law of black hole thermodynamics can be obtained. It is also demonstrated that, by keeping the same form of the black hole mass, the Rényi temperature is straightforwardly defined as proposed in the literature. Since many different types of black holes can indeed be successfully treated with such a procedure, our consideration is fairly general. It is worthwhile to argue that the black hole thermodynamics in Rényi statistics is rooted from the relation among geometric quantities in the same way as the standard approach corresponding to the Gibbs–Boltzmann statistics. Even though our results are based on classical gravity, they may pave the way to derive the Rényi temperature using the notion of quantum field in curved spacetime.</div></div>","PeriodicalId":54712,"journal":{"name":"Nuclear Physics B","volume":"1011 ","pages":"Article 116796"},"PeriodicalIF":2.5,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143176916","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-02-01DOI: 10.1016/j.nuclphysb.2025.116803
Abdullah Guvendi , Omar Mustafa
In this research, we study fermion-antifermion pairs in a magnetized spacetime induced by a point-like source and characterized by an angular deficit parameter, α. In the rest frame, the relative motion (∝r) of these pairs is analyzed using exact solutions of a two-body Dirac equation with a position-dependent mass expressed as . We select the Lorentz scalar potential , which modifies the rest mass in a manner analogous to an attractive Coulomb potential, and derive analytical solutions to the resulting radial wave equation. Our findings are applicable to pairs in flat spacetime when without loss of generality. We elucidate how the spectra of such pairs are influenced by the spacetime background. Additionally, we observe that even the well-known non-relativistic energy () reflects the influence of the parameter α in positronium-like fermion-antifermion systems. We propose that our results can also be extended to study charge carriers in magnetized monolayer materials. Furthermore, we demonstrate that the metric for a 2+1-dimensional spinning point source background can be transformed into the metric describing the near-horizon region of a rotating BTZ black hole, a result not previously reported in the literature. This metric holds potential for providing meaningful insights into topics such as holographic superconductivity and quantum critical phenomena in future research.
{"title":"Fermion-antifermion pairs in magnetized spacetime generated by a point source","authors":"Abdullah Guvendi , Omar Mustafa","doi":"10.1016/j.nuclphysb.2025.116803","DOIUrl":"10.1016/j.nuclphysb.2025.116803","url":null,"abstract":"<div><div>In this research, we study fermion-antifermion pairs in a magnetized spacetime induced by a point-like source and characterized by an angular deficit parameter, <em>α</em>. In the rest frame, the relative motion (∝<em>r</em>) of these pairs is analyzed using exact solutions of a two-body Dirac equation with a position-dependent mass expressed as <span><math><mi>m</mi><mo>(</mo><mi>r</mi><mo>)</mo><mo>=</mo><msub><mrow><mi>m</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>+</mo><mi>S</mi><mo>(</mo><mi>r</mi><mo>)</mo></math></span>. We select the Lorentz scalar potential <span><math><mi>S</mi><mo>(</mo><mi>r</mi><mo>)</mo><mo>=</mo><mo>−</mo><msub><mrow><mi>α</mi></mrow><mrow><mi>c</mi></mrow></msub><mo>/</mo><mi>r</mi></math></span>, which modifies the rest mass in a manner analogous to an attractive Coulomb potential, and derive analytical solutions to the resulting radial wave equation. Our findings are applicable to pairs in flat spacetime when <span><math><mi>α</mi><mo>=</mo><mn>1</mn></math></span> without loss of generality. We elucidate how the spectra of such pairs are influenced by the spacetime background. Additionally, we observe that even the well-known non-relativistic energy (<span><math><mo>∝</mo><msubsup><mrow><mi>α</mi></mrow><mrow><mi>c</mi></mrow><mrow><mn>2</mn></mrow></msubsup></math></span>) reflects the influence of the parameter <em>α</em> in positronium-like fermion-antifermion systems. We propose that our results can also be extended to study charge carriers in magnetized monolayer materials. Furthermore, we demonstrate that the metric for a 2+1-dimensional spinning point source background can be transformed into the metric describing the near-horizon region of a rotating BTZ black hole, a result not previously reported in the literature. This metric holds potential for providing meaningful insights into topics such as holographic superconductivity and quantum critical phenomena in future research.</div></div>","PeriodicalId":54712,"journal":{"name":"Nuclear Physics B","volume":"1011 ","pages":"Article 116803"},"PeriodicalIF":2.5,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143176940","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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