Pub Date : 2026-01-27DOI: 10.1016/j.hedp.2026.101267
M. Sharif , Tayyab Naseer , Hira Shadab
Our investigation develops two new singularity-free interior solutions, describing spherical anisotropic configurations within the framework of gravity. The modified Einstein field equations are established along with the expression of anisotropic pressure for a static geometry. Two independent constraints are imposed to solve the resulting field equations. In each case, we solve differential equations for temporal metric function under the assumption of radial potential and the anisotropic factor. Such an integration results in multiple integration constants that are fixed by matching the interior line element with the Schwarzschild exterior solution at the stellar surface. The vanishing radial condition at the surface also serves as an additional constraint. Afterwards, we investigate particular requirements whose fulfillment produce physically feasible compact star models. For graphical evaluation, we utilize observational data from two compact objects, namely SMC X-4 and 4U 1820-30, and vary the model parameter. Our analysis demonstrates that both stellar models satisfy all necessary physical acceptability conditions for specific parametric choices.
{"title":"Modeling compact stellar objects admitting anisotropic fluid in f(R,T) gravity: Viability and stability analysis","authors":"M. Sharif , Tayyab Naseer , Hira Shadab","doi":"10.1016/j.hedp.2026.101267","DOIUrl":"10.1016/j.hedp.2026.101267","url":null,"abstract":"<div><div>Our investigation develops two new singularity-free interior solutions, describing spherical anisotropic configurations within the framework of <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></mrow></math></span> gravity. The modified Einstein field equations are established along with the expression of anisotropic pressure for a static geometry. Two independent constraints are imposed to solve the resulting field equations. In each case, we solve differential equations for temporal metric function under the assumption of radial potential and the anisotropic factor. Such an integration results in multiple integration constants that are fixed by matching the interior line element with the Schwarzschild exterior solution at the stellar surface. The vanishing radial condition at the surface also serves as an additional constraint. Afterwards, we investigate particular requirements whose fulfillment produce physically feasible compact star models. For graphical evaluation, we utilize observational data from two compact objects, namely SMC X-4 and 4U 1820-30, and vary the model parameter. Our analysis demonstrates that both stellar models satisfy all necessary physical acceptability conditions for specific parametric choices.</div></div>","PeriodicalId":49267,"journal":{"name":"High Energy Density Physics","volume":"58 ","pages":"Article 101267"},"PeriodicalIF":0.9,"publicationDate":"2026-01-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146090383","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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 : 2026-01-17DOI: 10.1016/j.hedp.2026.101265
M. Lashgari , M. Asghari , D. Komaizi , A.R. Niknam , H. Moghadasin
The amplification of ultrashort laser pulses has attracted significant attention in recent years. An advanced approach involves utilizing plasma as a medium for the amplification process. In this research, we conduct particle-in-cell (PIC) simulations to study the interaction between two counter-propagating seed and pump pulses in a plasma with sub-quarter-critical density. To reduce noise in the simulations, we initially optimized the number of particles per cell. Various plasma conditions affecting the amplification process are considered. The findings reveal that among the studied cases, density ramps and plasma lengths significantly influence energy transfer efficiency. The seed pulse reaches maximum amplification at a plasma density of , where the largest Brillouin peak is observed. For the three ramp shapes – linear, quadratic, and exponential – the results show that quadratic ramps achieve the highest amplification levels due to the enhanced phase matching condition. It was also found that seed amplification is more effective with asymmetric density ramps. These insights contribute to the optimization of plasma-based stimulated Brillouin scattering for achieving ultrahigh-intensity laser pulses in applications ranging from inertial confinement fusion to high-energy particle acceleration.
{"title":"Effect of shape and asymmetry of density ramp on laser pulse amplification via stimulated Brillouin scattering","authors":"M. Lashgari , M. Asghari , D. Komaizi , A.R. Niknam , H. Moghadasin","doi":"10.1016/j.hedp.2026.101265","DOIUrl":"10.1016/j.hedp.2026.101265","url":null,"abstract":"<div><div>The amplification of ultrashort laser pulses has attracted significant attention in recent years. An advanced approach involves utilizing plasma as a medium for the amplification process. In this research, we conduct particle-in-cell (PIC) simulations to study the interaction between two counter-propagating seed and pump pulses in a plasma with sub-quarter-critical density. To reduce noise in the simulations, we initially optimized the number of particles per cell. Various plasma conditions affecting the amplification process are considered. The findings reveal that among the studied cases, density ramps and plasma lengths significantly influence energy transfer efficiency. The seed pulse reaches maximum amplification at a plasma density of <span><math><mrow><mn>0</mn><mo>.</mo><mn>0104</mn><mspace></mspace><msub><mrow><mi>n</mi></mrow><mrow><mi>c</mi><mi>r</mi></mrow></msub></mrow></math></span>, where the largest Brillouin peak is observed. For the three ramp shapes – linear, quadratic, and exponential – the results show that quadratic ramps achieve the highest amplification levels due to the enhanced phase matching condition. It was also found that seed amplification is more effective with asymmetric density ramps. These insights contribute to the optimization of plasma-based stimulated Brillouin scattering for achieving ultrahigh-intensity laser pulses in applications ranging from inertial confinement fusion to high-energy particle acceleration.</div></div>","PeriodicalId":49267,"journal":{"name":"High Energy Density Physics","volume":"58 ","pages":"Article 101265"},"PeriodicalIF":0.9,"publicationDate":"2026-01-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146090382","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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 : 2026-01-17DOI: 10.1016/j.hedp.2026.101266
Elangbam Chingkheinganba Meetei, S. Surendra Singh
<div><div>The Friedmann–Robertson–Walker (FRW) cosmological model is analysed within the framework of <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>,</mo><mi>G</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></mrow></math></span> gravity, where <span><math><mi>T</mi></math></span> denotes the trace of the energy–momentum tensor, <span><math><mi>G</mi></math></span> is the Gauss–Bonnet invariant, and <span><math><mi>R</mi></math></span> is the Ricci scalar. We consider the functional form <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>,</mo><mi>G</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow><mo>=</mo><mi>R</mi><mo>+</mo><msup><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>+</mo><mi>λ</mi><mspace></mspace><mi>G</mi><mspace></mspace><msup><mrow><mrow><mo>(</mo><mo>−</mo><mi>T</mi><mo>)</mo></mrow></mrow><mrow><mi>m</mi></mrow></msup></mrow></math></span>, where <span><math><mi>λ</mi></math></span> and <span><math><mi>m</mi></math></span> are model parameters. Adopting a newly proposed deceleration parameter, <span><math><mrow><mi>q</mi><mrow><mo>(</mo><mi>z</mi><mo>)</mo></mrow><mo>=</mo><msub><mrow><mi>q</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>+</mo><mfrac><mrow><mi>a</mi><mi>z</mi><mo>+</mo><mi>b</mi><mrow><mo>(</mo><msup><mrow><mi>z</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>+</mo><msup><mrow><mi>z</mi></mrow><mrow><mn>3</mn></mrow></msup><mo>)</mo></mrow></mrow><mrow><mn>1</mn><mo>+</mo><msup><mrow><mi>z</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></mfrac></mrow></math></span>, we employ the Markov Chain Monte Carlo (MCMC) method to find the constrained values of the cosmological parameters using Hubble, BAO, and Pantheon+ datasets. Our analysis shows that the pressure becomes negative for <span><math><mrow><mi>z</mi><mo>→</mo><mo>−</mo><mn>1</mn></mrow></math></span> after <span><math><mrow><mi>z</mi><mo>≈</mo><mn>0</mn><mo>.</mo><mn>42</mn></mrow></math></span>, while the energy density remains positive for all <span><math><mi>z</mi></math></span>. The deceleration parameter converges to <span><math><mrow><mo>−</mo><mn>1</mn></mrow></math></span>, with a present value <span><math><mrow><msub><mrow><mi>q</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mo>−</mo><mn>0</mn><mo>.</mo><mn>54</mn></mrow></math></span> which implies that the present stage of accelerated expansion. The equation-of-state parameter <span><math><mi>ω</mi></math></span> also approaches to <span><math><mrow><mo>−</mo><mn>1</mn></mrow></math></span> at late times which is consistent with a dark energy dominated era. Examination of the energy conditions reveals that the Strong Energy Condition (SEC) fails for <span><math><mrow><mi>z</mi><mo>→</mo><mo>−</mo><mn>1</mn></mrow></math></span> supporting the interpretation of ongoing late-time cosmic acceleration. State finder diagnostics indicate a transition from a Quintessence regime to a <span><math><mi>Λ</mi></math></span>CDM-like behaviour which is in agreement with current observational d
在f（R，G，T）引力框架下分析了FRW宇宙学模型，其中T表示能量动量张量的轨迹，G表示高斯-博内不变量，R表示里奇标量。我们考虑函数形式f(R，G，T)=R+R2+λG(- T)m，其中λ和m是模型参数。采用新提出的减速参数q(z)=q0+az+b(z2+z3)1+z2，利用Markov Chain Monte Carlo （MCMC）方法，利用Hubble、BAO和Pantheon+数据集求出宇宙学参数的约束值。我们的分析表明，在z≈0.42之后，压力在z→−1处变为负值，而能量密度在所有z处都保持正值。减速参数收敛于−1，其现值q0=−0.54，这意味着当前阶段的加速膨胀。状态方程参数ω在较晚时间也接近于−1，这与暗能量占主导的时代相一致。对能量条件的检验表明，对于z→−1，强能量条件（SEC）不成立，支持对正在进行的晚时间宇宙加速的解释。状态查找器诊断表明从Quintessence状态过渡到ΛCDM-like行为，这与当前的观测数据一致。此外，宇宙的总熵随着z→−1单调增加，从而满足热力学第二定律。在整个演化过程中，声速平方的正性进一步确保了梯度不稳定性的存在，从而证实了所提出的f（R，G，T）宇宙学模型的微扰稳定性。
{"title":"Observational compliance of cosmic parameters in modified f(R,G,T) gravity","authors":"Elangbam Chingkheinganba Meetei, S. Surendra Singh","doi":"10.1016/j.hedp.2026.101266","DOIUrl":"10.1016/j.hedp.2026.101266","url":null,"abstract":"<div><div>The Friedmann–Robertson–Walker (FRW) cosmological model is analysed within the framework of <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>,</mo><mi>G</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></mrow></math></span> gravity, where <span><math><mi>T</mi></math></span> denotes the trace of the energy–momentum tensor, <span><math><mi>G</mi></math></span> is the Gauss–Bonnet invariant, and <span><math><mi>R</mi></math></span> is the Ricci scalar. We consider the functional form <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>,</mo><mi>G</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow><mo>=</mo><mi>R</mi><mo>+</mo><msup><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>+</mo><mi>λ</mi><mspace></mspace><mi>G</mi><mspace></mspace><msup><mrow><mrow><mo>(</mo><mo>−</mo><mi>T</mi><mo>)</mo></mrow></mrow><mrow><mi>m</mi></mrow></msup></mrow></math></span>, where <span><math><mi>λ</mi></math></span> and <span><math><mi>m</mi></math></span> are model parameters. Adopting a newly proposed deceleration parameter, <span><math><mrow><mi>q</mi><mrow><mo>(</mo><mi>z</mi><mo>)</mo></mrow><mo>=</mo><msub><mrow><mi>q</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>+</mo><mfrac><mrow><mi>a</mi><mi>z</mi><mo>+</mo><mi>b</mi><mrow><mo>(</mo><msup><mrow><mi>z</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>+</mo><msup><mrow><mi>z</mi></mrow><mrow><mn>3</mn></mrow></msup><mo>)</mo></mrow></mrow><mrow><mn>1</mn><mo>+</mo><msup><mrow><mi>z</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></mfrac></mrow></math></span>, we employ the Markov Chain Monte Carlo (MCMC) method to find the constrained values of the cosmological parameters using Hubble, BAO, and Pantheon+ datasets. Our analysis shows that the pressure becomes negative for <span><math><mrow><mi>z</mi><mo>→</mo><mo>−</mo><mn>1</mn></mrow></math></span> after <span><math><mrow><mi>z</mi><mo>≈</mo><mn>0</mn><mo>.</mo><mn>42</mn></mrow></math></span>, while the energy density remains positive for all <span><math><mi>z</mi></math></span>. The deceleration parameter converges to <span><math><mrow><mo>−</mo><mn>1</mn></mrow></math></span>, with a present value <span><math><mrow><msub><mrow><mi>q</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mo>−</mo><mn>0</mn><mo>.</mo><mn>54</mn></mrow></math></span> which implies that the present stage of accelerated expansion. The equation-of-state parameter <span><math><mi>ω</mi></math></span> also approaches to <span><math><mrow><mo>−</mo><mn>1</mn></mrow></math></span> at late times which is consistent with a dark energy dominated era. Examination of the energy conditions reveals that the Strong Energy Condition (SEC) fails for <span><math><mrow><mi>z</mi><mo>→</mo><mo>−</mo><mn>1</mn></mrow></math></span> supporting the interpretation of ongoing late-time cosmic acceleration. State finder diagnostics indicate a transition from a Quintessence regime to a <span><math><mi>Λ</mi></math></span>CDM-like behaviour which is in agreement with current observational d","PeriodicalId":49267,"journal":{"name":"High Energy Density Physics","volume":"58 ","pages":"Article 101266"},"PeriodicalIF":0.9,"publicationDate":"2026-01-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146037529","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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 : 2026-01-12DOI: 10.1016/j.hedp.2025.101264
Mehnaz Shakeel , Shahida Parveen , Mustafa Inc , Hina Zahir , Hina Bibi
In this article, the Korteweg–de Vries–Burgers equation (KdVBE) is derived for ion-acoustic shocks in a dusty plasma considering warm ions, electrons and dust. The set of equations is normalized using different schemes, and the reductive perturbation technique (RPT) is applied to derive the model. The KdVBE is converted to time fractional KdVBE and then numerical scheme is formulated for the solution of time fractional KdVBE. A radial basis function collocation scheme and the Crank–Nicolson scheme are applied on time fractional KdVBE. The time-fractional derivative is discretized using the Caputo–Fabrizio fractional derivative. Moreover, a -weighted scheme is implemented for the spatial derivatives, in which radial basis functions are used for space derivatives in which radial basis function is used to approximate the derivatives. The behaviour of the method is assessed with the help of graphs and tables, and also shows the effect of the Caputo–Fabrizio fractional derivative. Numerical simulations indicate that the proposed scheme is highly efficient to find more accurate results. The solution is obtained for a variety of parameters to describe their behaviour of parameters like temperature ratio, fractional parameter and non-extensive distribution. The accuracy of the proposed method is verified by comparing the results with other methods in the literature.
{"title":"Numerical solution of time fractional Korteweg–de Vries–Burgers equation in a dusty plasma with non-extensive distributed electrons","authors":"Mehnaz Shakeel , Shahida Parveen , Mustafa Inc , Hina Zahir , Hina Bibi","doi":"10.1016/j.hedp.2025.101264","DOIUrl":"10.1016/j.hedp.2025.101264","url":null,"abstract":"<div><div>In this article, the Korteweg–de Vries–Burgers equation (KdVBE) is derived for ion-acoustic shocks in a dusty plasma considering warm ions, electrons and dust. The set of equations is normalized using different schemes, and the reductive perturbation technique (RPT) is applied to derive the model. The KdVBE is converted to time fractional KdVBE and then numerical scheme is formulated for the solution of time fractional KdVBE. A radial basis function collocation scheme and the Crank–Nicolson scheme are applied on time fractional KdVBE. The time-fractional derivative is discretized using the Caputo–Fabrizio fractional derivative. Moreover, a <span><math><mi>θ</mi></math></span>-weighted scheme is implemented for the spatial derivatives, in which radial basis functions are used for space derivatives in which radial basis function is used to approximate the derivatives. The behaviour of the method is assessed with the help of graphs and tables, and also shows the effect of the Caputo–Fabrizio fractional derivative. Numerical simulations indicate that the proposed scheme is highly efficient to find more accurate results. The solution is obtained for a variety of parameters to describe their behaviour of parameters like temperature ratio, fractional parameter and non-extensive distribution. The accuracy of the proposed method is verified by comparing the results with other methods in the literature.</div></div>","PeriodicalId":49267,"journal":{"name":"High Energy Density Physics","volume":"58 ","pages":"Article 101264"},"PeriodicalIF":0.9,"publicationDate":"2026-01-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145976617","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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 : 2026-01-06DOI: 10.1016/j.hedp.2025.101261
Adnan Malik , Jamshed Khan , Fatemah Mofarreh
We present the first exact analytical solution for a Locally Rotationally Symmetric (LRS) Bianchi type I universe in quadratic gravity filled with a generalized Chaplygin gas. The critical constraint emerges as a necessary condition for integrability, leading to a novel cosmological phase: a non-expanding universe where anisotropic shear completely dominates volumetric expansion. This solution reveals a precise equilibrium between geometric curvature corrections and exotic matter pressure, maintaining finite shear despite a vanishing expansion scalar. The existence of this stationary anisotropic configuration challenges conventional isotropization paradigms and provides a new benchmark for understanding early-universe dynamics in modified gravity. Comprehensive numerical verification confirms the solution’s accuracy and linear stability.
{"title":"Shear-dominated LRS Bianchi type I cosmology in quadratic f(R) gravity with Chaplygin gas: A novel exact solution","authors":"Adnan Malik , Jamshed Khan , Fatemah Mofarreh","doi":"10.1016/j.hedp.2025.101261","DOIUrl":"10.1016/j.hedp.2025.101261","url":null,"abstract":"<div><div>We present the first exact analytical solution for a Locally Rotationally Symmetric (LRS) Bianchi type I universe in quadratic <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>)</mo></mrow><mo>=</mo><mi>R</mi><mo>+</mo><mi>α</mi><msup><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></math></span> gravity filled with a generalized Chaplygin gas. The critical constraint <span><math><mrow><mi>n</mi><mo>=</mo><mo>−</mo><mn>2</mn></mrow></math></span> emerges as a necessary condition for integrability, leading to a novel cosmological phase: a non-expanding universe where anisotropic shear completely dominates volumetric expansion. This solution reveals a precise equilibrium between geometric curvature corrections and exotic matter pressure, maintaining finite shear <span><math><mrow><msup><mrow><mi>σ</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>∝</mo><msup><mrow><mi>t</mi></mrow><mrow><mo>−</mo><mn>2</mn></mrow></msup></mrow></math></span> despite a vanishing expansion scalar. The existence of this stationary anisotropic configuration challenges conventional isotropization paradigms and provides a new benchmark for understanding early-universe dynamics in modified gravity. Comprehensive numerical verification confirms the solution’s accuracy and linear stability.</div></div>","PeriodicalId":49267,"journal":{"name":"High Energy Density Physics","volume":"58 ","pages":"Article 101261"},"PeriodicalIF":0.9,"publicationDate":"2026-01-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145938399","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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 : 2025-12-30DOI: 10.1016/j.hedp.2025.101259
M. Ilyas , Fawad Khan , Arooba Gul , Javeria Mehtab
In the framework of gravity with the exponential correction model , we explore the possibility of obtaining traversable wormhole geometries supported by galactic dark matter distributions. To this end, we investigate three distinct dark matter halo density profiles-namely the Universal Rotation Curve (URC), the Navarro–Frenk–White (NFW) model-I, and the NFW model-II-within the chosen modified gravity scenario. By analyzing the corresponding field equations, we show that these halo profiles can generate viable wormhole shape functions that satisfy the required flare-out conditions at the throat for suitable choices of the free parameters. Furthermore, the energy conditions are examined, and we find that the solutions inevitably lead to the violation of the null energy condition (NEC), a feature commonly associated with wormhole physics. This indicates that dark matter, within the modified gravity background considered here, may act as an effective source to sustain wormhole geometries in galactic halo regions. Our results therefore provide an intriguing connection between dark matter phenomenology, galactic halo structures, and non-linear corrections in gravity.
在f(R)引力框架下，采用指数修正模型f(R)=R+αRe−R/α1−1，探讨了在星系暗物质分布支持下获得可穿越虫洞几何形状的可能性。为此，我们研究了三种不同的暗物质晕密度分布-即通用旋转曲线（URC），纳瓦罗-弗兰克-怀特（NFW）模型- i和NFW模型- ii -在选定的修正重力情景下。通过分析相应的场方程，我们表明，这些光晕剖面可以产生可行的虫洞形状函数，并且在合适的自由参数选择下，这些虫洞形状函数可以满足喉部所需的爆发条件。此外，我们检查了能量条件，我们发现解不可避免地导致违反零能量条件（NEC），这是一个通常与虫洞物理相关的特征。这表明暗物质，在这里考虑的修正重力背景中，可能作为维持星系晕区域虫洞几何形状的有效来源。因此，我们的结果提供了暗物质现象学、星系晕结构和f(R)引力非线性修正之间的有趣联系。
{"title":"Exploring wormhole solutions with dark matter distributions in f(R) gravity","authors":"M. Ilyas , Fawad Khan , Arooba Gul , Javeria Mehtab","doi":"10.1016/j.hedp.2025.101259","DOIUrl":"10.1016/j.hedp.2025.101259","url":null,"abstract":"<div><div>In the framework of <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>)</mo></mrow></mrow></math></span> gravity with the exponential correction model <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>)</mo></mrow><mo>=</mo><mi>R</mi><mo>+</mo><mi>α</mi><mi>R</mi><mfenced><mrow><msup><mrow><mi>e</mi></mrow><mrow><mo>−</mo><mi>R</mi><mo>/</mo><msub><mrow><mi>α</mi></mrow><mrow><mn>1</mn></mrow></msub></mrow></msup><mo>−</mo><mn>1</mn></mrow></mfenced></mrow></math></span>, we explore the possibility of obtaining traversable wormhole geometries supported by galactic dark matter distributions. To this end, we investigate three distinct dark matter halo density profiles-namely the Universal Rotation Curve (URC), the Navarro–Frenk–White (NFW) model-I, and the NFW model-II-within the chosen modified gravity scenario. By analyzing the corresponding field equations, we show that these halo profiles can generate viable wormhole shape functions that satisfy the required flare-out conditions at the throat for suitable choices of the free parameters. Furthermore, the energy conditions are examined, and we find that the solutions inevitably lead to the violation of the null energy condition (NEC), a feature commonly associated with wormhole physics. This indicates that dark matter, within the modified gravity background considered here, may act as an effective source to sustain wormhole geometries in galactic halo regions. Our results therefore provide an intriguing connection between dark matter phenomenology, galactic halo structures, and non-linear corrections in <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>)</mo></mrow></mrow></math></span> gravity.</div></div>","PeriodicalId":49267,"journal":{"name":"High Energy Density Physics","volume":"58 ","pages":"Article 101259"},"PeriodicalIF":0.9,"publicationDate":"2025-12-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145884464","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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 : 2025-12-29DOI: 10.1016/j.hedp.2025.101260
C.H. Allen , A.M. Rasmus , J.M. Levesque , E.C. Merritt , S. Pellone , K.A. Flippo , N. Christiansen , C.A. Di Stefano , P. Donovan , J. Lavelle , K. Love , J.I. Martinez , D.W. Schmidt , S.J. Stringfield , C. Wilson , F. Doss
High-energy-density (HED) systems, such as inertial confinement fusion (ICF), are susceptible to hydrodynamic instabilities that can significantly affect both experimental results and modeling predictions. Isolated features, such as fill tubes or divots in the capsule, can cause material to jet as a result of the compressive shock exciting the Richtmyer–Meshkov instability, and serve as one of the primary degradation mechanisms in ICF yield. Simulations of feature-driven jets and how they mix require extensive experimental validation, particularly for understanding to what degree the initial size and shape of a feature influence jet dynamics, and how much instability feeds through downstream layers. A better understanding of feature-driven jetting can improve our mix modeling capabilities and increase hydrodynamic simulation accuracy.
This manuscript describes a series of experimental platforms fielded by Los Alamos National Laboratory as a part of the Mshock Omega 60 and ModCons Omega EP campaigns to explore feature-driven jetting. These platforms are designed to benchmark jet evolution and growth as a function of initial feature size and shape, investigate jet-layer interactions leading to instability feedthrough, and will be used to characterize jet-jet interactions resulting from clusters of features. Preliminary results for both platforms are shown. The ModCons experiments are on-going, and a discussion of future work directions is included.
{"title":"Experimental platforms for investigating feature-driven jets for HED mix model validation","authors":"C.H. Allen , A.M. Rasmus , J.M. Levesque , E.C. Merritt , S. Pellone , K.A. Flippo , N. Christiansen , C.A. Di Stefano , P. Donovan , J. Lavelle , K. Love , J.I. Martinez , D.W. Schmidt , S.J. Stringfield , C. Wilson , F. Doss","doi":"10.1016/j.hedp.2025.101260","DOIUrl":"10.1016/j.hedp.2025.101260","url":null,"abstract":"<div><div>High-energy-density (HED) systems, such as inertial confinement fusion (ICF), are susceptible to hydrodynamic instabilities that can significantly affect both experimental results and modeling predictions. Isolated features, such as fill tubes or divots in the capsule, can cause material to jet as a result of the compressive shock exciting the Richtmyer–Meshkov instability, and serve as one of the primary degradation mechanisms in ICF yield. Simulations of feature-driven jets and how they mix require extensive experimental validation, particularly for understanding to what degree the initial size and shape of a feature influence jet dynamics, and how much instability feeds through downstream layers. A better understanding of feature-driven jetting can improve our mix modeling capabilities and increase hydrodynamic simulation accuracy.</div><div>This manuscript describes a series of experimental platforms fielded by Los Alamos National Laboratory as a part of the <em>Mshock</em> Omega 60 and <em>ModCons</em> Omega EP campaigns to explore feature-driven jetting. These platforms are designed to benchmark jet evolution and growth as a function of initial feature size and shape, investigate jet-layer interactions leading to instability feedthrough, and will be used to characterize jet-jet interactions resulting from clusters of features. Preliminary results for both platforms are shown. The <em>ModCons</em> experiments are on-going, and a discussion of future work directions is included.</div></div>","PeriodicalId":49267,"journal":{"name":"High Energy Density Physics","volume":"58 ","pages":"Article 101260"},"PeriodicalIF":0.9,"publicationDate":"2025-12-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145884466","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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 : 2025-12-29DOI: 10.1016/j.hedp.2025.101262
Ghazala Akram, Maasoomah Sadaf, Saima Arshed, Muhammad Sheraz
A significant problem in mathematics and physics is the extraction of exact solutions for nonlinear partial differential equations. In this research paper, exact solutions of the (2+1)-dimensional Sakovich problem are obtained using three widely recognized techniques: the new Kudryashov method, the modified Kudryashov method, and the unified method. The results are visualized using Maple software, which illustrates the dynamics of the solutions.
{"title":"Novel soliton solutions for the (2+1)-dimensional Sakovich equation using analytical methods","authors":"Ghazala Akram, Maasoomah Sadaf, Saima Arshed, Muhammad Sheraz","doi":"10.1016/j.hedp.2025.101262","DOIUrl":"10.1016/j.hedp.2025.101262","url":null,"abstract":"<div><div>A significant problem in mathematics and physics is the extraction of exact solutions for nonlinear partial differential equations. In this research paper, exact solutions of the (2+1)-dimensional Sakovich problem are obtained using three widely recognized techniques: the new Kudryashov method, the modified Kudryashov method, and the unified method. The results are visualized using Maple software, which illustrates the dynamics of the solutions.</div></div>","PeriodicalId":49267,"journal":{"name":"High Energy Density Physics","volume":"58 ","pages":"Article 101262"},"PeriodicalIF":0.9,"publicationDate":"2025-12-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145884465","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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 : 2025-12-28DOI: 10.1016/j.hedp.2025.101263
Md. Mamunur Roshid , Mahtab Uddin , Mrityunjoy Kumar Pandit , Golam Mostafa , M S Osman
This manuscript studies the stochastic fractional Yajima-Oikawa model in short-wave and long-wave, focusing on the optical soliton solutions, the impact of multiplicative noise on the solitons, Quasi-periodic, super-periodic, and chaotic nature. A planar dynamic system is formed from the stochastic fractional Yajima-Oikawa model by using a transformation variable. Then, the chaotic nature, super-periodicity, and quasi-periodicity are analyzed by using a frequency and strength cosine perturbation term. The optical soliton solutions of the stochastic fractional Yajima-Oikawa model are constructed by using a functional transformation approach as well. The solutions take all trigonometric and hyperbolic functions from. Using suitable values for the free parameters, three-dimensional profiles were plotted to analyze the dynamic properties of the derived solutions, such as bright bell-shaped, dark bell-shaped, bright periodic, and cross double-periodic solitons. The noise causes changes in the soliton profiles, which makes the soliton amplitude peaks wider and less clear. White noise models mimic actual scenarios where random variations, including thermal or ambient noise, affect the stability of solitons as they propagate. In optical fiber communication, understanding how noise affects things helps engineers build systems that are better able to handle random problems. This method demonstrates how well graphical simulations work to show how these solutions behave and interact in practical settings. Finally, the result of the comparison demonstrates that the multiplicative noise intensity and the fractional parameter have a great influence on the obtained solutions. Moreover, this work contributes some new phenomena to advance the concept of nonlinear optical research and communication technology.
{"title":"Analysis of multiplicative noise intensity and nature for the stochastic Yajima-Oikawa in short-wave and long-wave","authors":"Md. Mamunur Roshid , Mahtab Uddin , Mrityunjoy Kumar Pandit , Golam Mostafa , M S Osman","doi":"10.1016/j.hedp.2025.101263","DOIUrl":"10.1016/j.hedp.2025.101263","url":null,"abstract":"<div><div>This manuscript studies the stochastic fractional Yajima-Oikawa model in short-wave and long-wave, focusing on the optical soliton solutions, the impact of multiplicative noise on the solitons, Quasi-periodic, super-periodic, and chaotic nature. A planar dynamic system is formed from the stochastic fractional Yajima-Oikawa model by using a transformation variable. Then, the chaotic nature, super-periodicity, and quasi-periodicity are analyzed by using a frequency and strength cosine perturbation term. The optical soliton solutions of the stochastic fractional Yajima-Oikawa model are constructed by using a functional transformation approach as well. The solutions take all trigonometric and hyperbolic functions from. Using suitable values for the free parameters, three-dimensional profiles were plotted to analyze the dynamic properties of the derived solutions, such as bright bell-shaped, dark bell-shaped, bright periodic, and cross double-periodic solitons. The noise causes changes in the soliton profiles, which makes the soliton amplitude peaks wider and less clear. White noise models mimic actual scenarios where random variations, including thermal or ambient noise, affect the stability of solitons as they propagate. In optical fiber communication, understanding how noise affects things helps engineers build systems that are better able to handle random problems. This method demonstrates how well graphical simulations work to show how these solutions behave and interact in practical settings. Finally, the result of the comparison demonstrates that the multiplicative noise intensity and the fractional parameter have a great influence on the obtained solutions. Moreover, this work contributes some new phenomena to advance the concept of nonlinear optical research and communication technology.</div></div>","PeriodicalId":49267,"journal":{"name":"High Energy Density Physics","volume":"58 ","pages":"Article 101263"},"PeriodicalIF":0.9,"publicationDate":"2025-12-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145976505","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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}
We investigated plasma-heating enhancement for the efficient production of high-energy-density plasma by irradiating a high-intensity, high-contrast short pulse from a kilojoule-class laser system onto a cone-attached target. Irradiating a cone-attached planar target with a high-contrast laser causes specular reflection of the laser pulse on the inner cone wall, aligning the laser pointing direction with the cone axis and focusing the laser near the tip. Using a simplified cone-attached target configuration, we directly demonstrate this guiding/focusing mechanism while isolating it from other complexities inherent to integrated fast-ignition experiments. The high contrast was achieved using a plasma mirror. Electron energy analyzer, X-ray spectrometer, and atomic kinetics modeling with a two-component electron distribution were applied to three cases: (i) flat target irradiated by low contrast pulse, (ii) flat target irradiated by high contrast pulse, and (iii) cone target irradiated by high contrast pulse. The cone irradiated by the high-contrast pulse case achieved an electron temperature of 9.9 keV, that is roughly 17.5 higher than in the low-contrast flat case. X-ray pinhole images show a multi-spot laser being guided to the cone tip, yielding localized X-ray emission. While a high-contrast laser reduced the fast-electron slope temperature for flat targets, adding the cone boosted the slope temperature by more than threefold, equivalent to a fourfold rise in local laser intensity. These results demonstrate that combining a high-contrast pulse with cone geometry markedly improves laser-to-plasma energy coupling for the fast-ignition inertial confinement fusion research.
{"title":"Enhanced plasma heating by interaction with high-contrast laser and cone-shaped target","authors":"Yuga Karaki , Yoshitaka Mori , Eigo Ebisawa , Yuichi Inubushi , Sadaoki Kojima , Kohei Yamanoi , Yuki Abe , Takumi Tsuido , Hiroki Matsubara , Rinya Akematsu , Ryo Omura , Ryunosuke Takizawa , King Fai Farley Law , Eisuke Miura , Yasunobu Arikawa , Keisuke Shigemori , Akifumi Iwamoto , Katsuhiro Ishii , Ryohei Hanayama , Yoneyoshi Kitagawa , Shinsuke Fujioka","doi":"10.1016/j.hedp.2025.101256","DOIUrl":"10.1016/j.hedp.2025.101256","url":null,"abstract":"<div><div>We investigated plasma-heating enhancement for the efficient production of high-energy-density plasma by irradiating a high-intensity, high-contrast short pulse from a kilojoule-class laser system onto a cone-attached target. Irradiating a cone-attached planar target with a high-contrast laser causes specular reflection of the laser pulse on the inner cone wall, aligning the laser pointing direction with the cone axis and focusing the laser near the tip. Using a simplified cone-attached target configuration, we directly demonstrate this guiding/focusing mechanism while isolating it from other complexities inherent to integrated fast-ignition experiments. The high contrast was achieved using a plasma mirror. Electron energy analyzer, X-ray spectrometer, and atomic kinetics modeling with a two-component electron distribution were applied to three cases: (i) flat target irradiated by low contrast pulse, (ii) flat target irradiated by high contrast pulse, and (iii) cone target irradiated by high contrast pulse. The cone irradiated by the high-contrast pulse case achieved an electron temperature of 9.9 <span><math><msubsup><mrow></mrow><mrow><mo>−</mo><mn>2</mn><mo>.</mo><mn>5</mn></mrow><mrow><mo>+</mo><mn>4</mn><mo>.</mo><mn>1</mn></mrow></msubsup></math></span> keV, that is roughly 17.5 <span><math><mo>×</mo></math></span> higher than in the low-contrast flat case. X-ray pinhole images show a multi-spot laser being guided to the cone tip, yielding localized X-ray emission. While a high-contrast laser reduced the fast-electron slope temperature for flat targets, adding the cone boosted the slope temperature by more than threefold, equivalent to a fourfold rise in local laser intensity. These results demonstrate that combining a high-contrast pulse with cone geometry markedly improves laser-to-plasma energy coupling for the fast-ignition inertial confinement fusion research.</div></div>","PeriodicalId":49267,"journal":{"name":"High Energy Density Physics","volume":"58 ","pages":"Article 101256"},"PeriodicalIF":0.9,"publicationDate":"2025-12-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145797534","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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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