The instantaneous normal mode (INM) approach, which extends the normal mode description of collective excitations in solids to liquids, is applied to strongly coupled, three-dimensional Yukawa liquids. Based on data from Langevin dynamics simulations, we compute the instantaneous normal modes across a wide range of coupling and screening parameters. Yukawa liquids at weak to moderate screening exhibit a pronounced maximum in the INM density of states, which disappears as the coupling decreases or screening becomes stronger. The fraction of unstable modes displays a quasi-universal behavior, which can be described to a large extent by an effective coupling strength. The relation of the INM approach to the quasi-localized charge approximation (QLCA) is explored in some detail. In particular, the QLCA dispersion relation can be recovered explicitly from an appropriately weighted mode spectrum.
{"title":"Instantaneous Normal Modes of Yukawa Liquids","authors":"Tillman Keller, Hanno Kählert","doi":"10.1002/ctpp.70012","DOIUrl":"https://doi.org/10.1002/ctpp.70012","url":null,"abstract":"<p>The instantaneous normal mode (INM) approach, which extends the normal mode description of collective excitations in solids to liquids, is applied to strongly coupled, three-dimensional Yukawa liquids. Based on data from Langevin dynamics simulations, we compute the instantaneous normal modes across a wide range of coupling and screening parameters. Yukawa liquids at weak to moderate screening exhibit a pronounced maximum in the INM density of states, which disappears as the coupling decreases or screening becomes stronger. The fraction of unstable modes displays a quasi-universal behavior, which can be described to a large extent by an effective coupling strength. The relation of the INM approach to the quasi-localized charge approximation (QLCA) is explored in some detail. In particular, the QLCA dispersion relation can be recovered explicitly from an appropriately weighted mode spectrum.</p>","PeriodicalId":10700,"journal":{"name":"Contributions to Plasma Physics","volume":"65 8-9","pages":""},"PeriodicalIF":1.5,"publicationDate":"2025-04-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/ctpp.70012","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145426041","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}
Simulated trajectories of electrons bombarding the mask line, as well as incoming electrons from the surface above at different temperatures in the front view. The number of incident electrons in each panel is 25. The red dash indicates the profile of the mask line. Fig. 2 of the paper by Peng Zhang et al. https://doi.org/10.1002/ctpp.202400118
{"title":"Cover Picture: Contrib. Plasma Phys. 04/2025","authors":"","doi":"10.1002/ctpp.202590007","DOIUrl":"https://doi.org/10.1002/ctpp.202590007","url":null,"abstract":"<p>Simulated trajectories of electrons bombarding the mask line, as well as incoming electrons from the surface above at different temperatures in the front view. The number of incident electrons in each panel is 25. The red dash indicates the profile of the mask line. Fig. 2 of the paper by Peng Zhang et al. https://doi.org/10.1002/ctpp.202400118\u0000 \u0000 <figure>\u0000 <div><picture>\u0000 <source></source></picture><p></p>\u0000 </div>\u0000 </figure></p>","PeriodicalId":10700,"journal":{"name":"Contributions to Plasma Physics","volume":"65 4","pages":""},"PeriodicalIF":1.3,"publicationDate":"2025-04-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/ctpp.202590007","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143871618","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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 Cairns–Tsallis (CT) distribution function is employed to model the quasi-neutral region of a basic bounded-plasma system, such as the one described by Tonks and Langmuir (TL). Electrons are assumed to follow the CT distribution, while ions are generated through electron-impact ionization of cold neutral atoms. Under the plasma approximation, the ion velocity distribution function is derived, and fluid moments are taken to evaluate the ion density, temperature, and polytropic coefficient. The results indicate that the ion polytropic coefficient is strongly dependent on the electron nonextensivity () and nonthermality () parameters inherent to the CT distribution. Specifically, an increase in electron nonextensivity leads to a significant deviation in the polytropic index, emphasizing the role of nonthermal effects in plasma behavior. These findings reduce to the Maxwellian case under specific limits, thus, validating the model. The study highlights the relevance of the CT distribution in capturing a broader range of physical phenomena in bounded plasmas, potentially applicable to space and astrophysical plasma environments.
{"title":"Ion Polytropic Coefficient in Bounded Plasmas With Cairns–Tsallis Distributed Electrons","authors":"Majid Khan, Sobia Shabbir, M. Kamran","doi":"10.1002/ctpp.70010","DOIUrl":"https://doi.org/10.1002/ctpp.70010","url":null,"abstract":"<div>\u0000 \u0000 <p>The Cairns–Tsallis (CT) distribution function is employed to model the quasi-neutral region of a basic bounded-plasma system, such as the one described by Tonks and Langmuir (TL). Electrons are assumed to follow the CT distribution, while ions are generated through electron-impact ionization of cold neutral atoms. Under the plasma approximation, the ion velocity distribution function is derived, and fluid moments are taken to evaluate the ion density, temperature, and polytropic coefficient. The results indicate that the ion polytropic coefficient is strongly dependent on the electron nonextensivity (<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>q</mi>\u0000 </mrow>\u0000 <annotation>$$ q $$</annotation>\u0000 </semantics></math>) and nonthermality (<span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>α</mi>\u0000 </mrow>\u0000 <annotation>$$ alpha $$</annotation>\u0000 </semantics></math>) parameters inherent to the CT distribution. Specifically, an increase in electron nonextensivity leads to a significant deviation in the polytropic index, emphasizing the role of nonthermal effects in plasma behavior. These findings reduce to the Maxwellian case under specific limits, thus, validating the model. The study highlights the relevance of the CT distribution in capturing a broader range of physical phenomena in bounded plasmas, potentially applicable to space and astrophysical plasma environments.</p>\u0000 </div>","PeriodicalId":10700,"journal":{"name":"Contributions to Plasma Physics","volume":"65 6","pages":""},"PeriodicalIF":1.3,"publicationDate":"2025-04-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144574303","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}
This study delves into the effects of dust size distribution on the properties of shock waves in a dusty plasma, where electrons follow a nonextensive distribution. Employing the reductive perturbation method, the research explores the influence of dust size distribution, modeled by polynomial and power law distributions, on shock wave characteristics such as amplitude, width, and phase velocity. The results reveal that the phase velocity and width of a shock wave considering the dust size distribution are larger than those of the dusty plasma with the averaged dust size. However, the amplitude of a shock wave considering the dust size distribution is smaller than that of the dusty plasma with the averaged dust size. These findings are pivotal for grasping the behavior of shock waves in diverse astrophysical and space plasma contexts where dust particles present a multitude of sizes.
{"title":"Effects of Dust Size Distribution on Shock Waves in Dusty Plasma With Nonextensive Electron","authors":"Bo Liu, Heng Zhang, Wenshan Duan","doi":"10.1002/ctpp.70008","DOIUrl":"https://doi.org/10.1002/ctpp.70008","url":null,"abstract":"<div>\u0000 \u0000 <p>This study delves into the effects of dust size distribution on the properties of shock waves in a dusty plasma, where electrons follow a nonextensive distribution. Employing the reductive perturbation method, the research explores the influence of dust size distribution, modeled by polynomial and power law distributions, on shock wave characteristics such as amplitude, width, and phase velocity. The results reveal that the phase velocity and width of a shock wave considering the dust size distribution are larger than those of the dusty plasma with the averaged dust size. However, the amplitude of a shock wave considering the dust size distribution is smaller than that of the dusty plasma with the averaged dust size. These findings are pivotal for grasping the behavior of shock waves in diverse astrophysical and space plasma contexts where dust particles present a multitude of sizes.</p>\u0000 </div>","PeriodicalId":10700,"journal":{"name":"Contributions to Plasma Physics","volume":"65 6","pages":""},"PeriodicalIF":1.3,"publicationDate":"2025-04-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144574064","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}
Linear properties of acoustic modes associated with dust-acoustic waves (DAWs) has been examined in a dusty plasma medium containing inertial negatively charged dust species, non-inertial ions following Maxwellian distribution and non-inertial electrons following non-extensive q-distribution. The dust kinematic viscosity and also the dissipation due to the dust-neutral collision have been taken into consideration. The thermal effect of dust species is also taken into account. The linear dispersion relation (LDR) is derived by adopting the normal mode analysis and the linear properties of DAWs is studied for different plasma contexts. It is shown that the propagation zone for DAWs is significantly influenced by the dust-neutral collision and also by the viscosity of dust species. The implications of our results are discussed elaborately in connection with Saturn's rings, Earth's noctilucent clouds (NLC) and DC discharge plasmas.
{"title":"Linear Properties of Dust-Acoustic Waves in Viscous and Collisional Dusty Plasmas","authors":"Md. Mehedi Hasan, Sharmin Sultana, A. A. Mamun","doi":"10.1002/ctpp.70007","DOIUrl":"https://doi.org/10.1002/ctpp.70007","url":null,"abstract":"<div>\u0000 \u0000 <p>Linear properties of acoustic modes associated with dust-acoustic waves (DAWs) has been examined in a dusty plasma medium containing inertial negatively charged dust species, non-inertial ions following Maxwellian distribution and non-inertial electrons following non-extensive <i>q</i>-distribution. The dust kinematic viscosity and also the dissipation due to the dust-neutral collision have been taken into consideration. The thermal effect of dust species is also taken into account. The linear dispersion relation (LDR) is derived by adopting the normal mode analysis and the linear properties of DAWs is studied for different plasma contexts. It is shown that the propagation zone for DAWs is significantly influenced by the dust-neutral collision and also by the viscosity of dust species. The implications of our results are discussed elaborately in connection with Saturn's rings, Earth's noctilucent clouds (NLC) and DC discharge plasmas.</p>\u0000 </div>","PeriodicalId":10700,"journal":{"name":"Contributions to Plasma Physics","volume":"65 6","pages":""},"PeriodicalIF":1.3,"publicationDate":"2025-04-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144574009","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}
<div> <p>This manuscript provides the theoretical explanation of the nonlinear scattering of an EMIC into an IAW <span></span><math> <semantics> <mrow> <mtext>and</mtext> </mrow> <annotation>$$ mathrm{and} $$</annotation> </semantics></math> a scattered ion-cyclotron wave (SICW) in a dusty plasma using fluid theory. The low-frequency nonlinearity arises through the parallel ponderomotive force on ions and the high-frequency nonlinearity arises through <span></span><math> <semantics> <mrow> <mtext>the</mtext> </mrow> <annotation>$$ mathrm{the} $$</annotation> </semantics></math> nonlinear current density of ions. For the linked modes, a nonlinear dispersion relation is obtained. A formula for the SICW growth rate has been derived. The estimation of the turbulence growth rate takes into account for the typical parameters of dusty plasma. It is detected that an increased growth rate can be seen with a rise in the pump wave amplitude and the number density <span></span><math> <semantics> <mrow> <msup> <mi>n</mi> <mrow> <mn>0</mn> <mi>d</mi> </mrow> </msup> <mfenced> <msup> <mi>cm</mi> <mrow> <mo>−</mo> <mn>3</mn> </mrow> </msup> </mfenced> </mrow> <annotation>$$ {n}^{0d}left({mathrm{cm}}^{-3}right) $$</annotation> </semantics></math> of dust grains. However, a decline in the growth rate has been reported with growing relative density <span></span><math> <semantics> <mrow> <mi>d</mi> <mo>=</mo> <mfrac> <msup> <mi>n</mi> <mrow> <mn>0</mn> <mi>i</mi> </mrow> </msup> <msup> <mi>n</mi> <mrow> <mn>0</mn> <mi>e</mi> </mrow> </msup> </mfrac> </mrow> <annotation>$$ d=frac{n^{0i}}{n^{0e}} $$</annotation> </semantics></math> <span></span><math> <semantics> <mrow> <mtext>of</mtext> </mrow> <annotation>$$ mathrm{of} $$</annotation> </semantics></math> dust grains, magnetic field, and the dust grain's size. Th
{"title":"Generation of Scattered Ion-Cyclotron Wave and Ion Acoustic Wave by Parametric Instability of Electromagnetic Ion-Cyclotron Wave in a Dusty Plasma","authors":"Twinkle Pahuja, Supreet, Jyotsna Sharma","doi":"10.1002/ctpp.70005","DOIUrl":"https://doi.org/10.1002/ctpp.70005","url":null,"abstract":"<div>\u0000 \u0000 <p>This manuscript provides the theoretical explanation of the nonlinear scattering of an EMIC into an IAW <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mtext>and</mtext>\u0000 </mrow>\u0000 <annotation>$$ mathrm{and} $$</annotation>\u0000 </semantics></math> a scattered ion-cyclotron wave (SICW) in a dusty plasma using fluid theory. The low-frequency nonlinearity arises through the parallel ponderomotive force on ions and the high-frequency nonlinearity arises through <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mtext>the</mtext>\u0000 </mrow>\u0000 <annotation>$$ mathrm{the} $$</annotation>\u0000 </semantics></math> nonlinear current density of ions. For the linked modes, a nonlinear dispersion relation is obtained. A formula for the SICW growth rate has been derived. The estimation of the turbulence growth rate takes into account for the typical parameters of dusty plasma. It is detected that an increased growth rate can be seen with a rise in the pump wave amplitude and the number density <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <msup>\u0000 <mi>n</mi>\u0000 <mrow>\u0000 <mn>0</mn>\u0000 <mi>d</mi>\u0000 </mrow>\u0000 </msup>\u0000 <mfenced>\u0000 <msup>\u0000 <mi>cm</mi>\u0000 <mrow>\u0000 <mo>−</mo>\u0000 <mn>3</mn>\u0000 </mrow>\u0000 </msup>\u0000 </mfenced>\u0000 </mrow>\u0000 <annotation>$$ {n}^{0d}left({mathrm{cm}}^{-3}right) $$</annotation>\u0000 </semantics></math> of dust grains. However, a decline in the growth rate has been reported with growing relative density <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>d</mi>\u0000 <mo>=</mo>\u0000 <mfrac>\u0000 <msup>\u0000 <mi>n</mi>\u0000 <mrow>\u0000 <mn>0</mn>\u0000 <mi>i</mi>\u0000 </mrow>\u0000 </msup>\u0000 <msup>\u0000 <mi>n</mi>\u0000 <mrow>\u0000 <mn>0</mn>\u0000 <mi>e</mi>\u0000 </mrow>\u0000 </msup>\u0000 </mfrac>\u0000 </mrow>\u0000 <annotation>$$ d=frac{n^{0i}}{n^{0e}} $$</annotation>\u0000 </semantics></math> <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mtext>of</mtext>\u0000 </mrow>\u0000 <annotation>$$ mathrm{of} $$</annotation>\u0000 </semantics></math> dust grains, magnetic field, and the dust grain's size. Th","PeriodicalId":10700,"journal":{"name":"Contributions to Plasma Physics","volume":"65 6","pages":""},"PeriodicalIF":1.3,"publicationDate":"2025-04-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144573721","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}
Mikael Tacu, Jean-Christophe Pain, Matthias Pautard, Christophe Blancard
In this article, we examine different approaches for calculating low frequency opacities in the warm dense matter regime. The relevance of the average-atom approximation and of different models for calculating opacities, such as the Ziman or Ziman–Evans models is discussed and the results compared to ab initio simulations. We begin by recalling the derivation of the Ziman–Evans resistivity from Kubo's linear response theory, using the local approximation to the solutions of the Lippmann–Schwinger equation. With the help of this approximation, we explicitly introduce an ionic structure factor into the Ziman formula, without resorting to the Born approximation. Both approaches involve the calculation of scattering phase shifts, which we integrate from Calogero equation with an adaptive step numerical scheme based on a Runge–Kutta–Merson solver. We show that if the atomic number is not too large, integrating the phase shifts in this way is more time-efficient than using a classical Numerov-type scheme to solve the radial Schrödinger equation. Various approximations are explored for phase shifts to further improve computation time. For the Born approximation, we show that using Born phase shifts directly in the scattering cross-section gives more accurate results than with the integral formula based on the Fourier transform of the electron-ion potential. We also compare an analytical formula based on a Yukawa fit of the electron-ion potential to a numerical integration. The average-atom results are compared with DFT-based molecular dynamics simulations for aluminum in the dilute regime and for copper, aluminum and gold at solid density and different temperatures.
在这篇文章中，我们研究了计算热致密物质状态下低频不透明度的不同方法。讨论了平均原子近似和不同模型（如Ziman或Ziman - evans模型）计算不透明度的相关性，并将结果与从头计算模拟进行了比较。我们首先回顾从Kubo的线性响应理论推导齐曼-埃文斯电阻率，使用Lippmann-Schwinger方程解的局部近似。在这种近似的帮助下，我们明确地在齐曼公式中引入了离子结构因子，而无需诉诸玻恩近似。这两种方法都涉及到散射相移的计算，我们用基于Runge-Kutta-Merson解算器的自适应阶跃数值格式对Calogero方程进行积分。我们表明，如果原子序数Z $$ Z $$不是太大，以这种方式积分相移比使用经典的numerov型方案来求解径向Schrödinger方程更省时。为了进一步缩短计算时间，对相移进行了各种近似的探讨。对于玻恩近似，我们证明了在散射截面中直接使用玻恩相移比基于电子-离子势的傅里叶变换的积分公式给出更准确的结果。我们还比较了基于汤川拟合的电子-离子势的解析公式与数值积分。将平均原子结果与基于dft的分子动力学模拟结果进行了比较，分别模拟了铝在稀态下和铜、铝和金在固体密度和不同温度下的分子动力学模拟结果。
{"title":"Electrical Conductivities and Low Frequency Opacities in the Warm Dense Matter Regime","authors":"Mikael Tacu, Jean-Christophe Pain, Matthias Pautard, Christophe Blancard","doi":"10.1002/ctpp.70004","DOIUrl":"https://doi.org/10.1002/ctpp.70004","url":null,"abstract":"<p>In this article, we examine different approaches for calculating low frequency opacities in the warm dense matter regime. The relevance of the average-atom approximation and of different models for calculating opacities, such as the Ziman or Ziman–Evans models is discussed and the results compared to ab initio simulations. We begin by recalling the derivation of the Ziman–Evans resistivity from Kubo's linear response theory, using the local approximation to the solutions of the Lippmann–Schwinger equation. With the help of this approximation, we explicitly introduce an ionic structure factor into the Ziman formula, without resorting to the Born approximation. Both approaches involve the calculation of scattering phase shifts, which we integrate from Calogero equation with an adaptive step numerical scheme based on a Runge–Kutta–Merson solver. We show that if the atomic number <span></span><math>\u0000 <semantics>\u0000 <mrow>\u0000 <mi>Z</mi>\u0000 </mrow>\u0000 <annotation>$$ Z $$</annotation>\u0000 </semantics></math> is not too large, integrating the phase shifts in this way is more time-efficient than using a classical Numerov-type scheme to solve the radial Schrödinger equation. Various approximations are explored for phase shifts to further improve computation time. For the Born approximation, we show that using Born phase shifts directly in the scattering cross-section gives more accurate results than with the integral formula based on the Fourier transform of the electron-ion potential. We also compare an analytical formula based on a Yukawa fit of the electron-ion potential to a numerical integration. The average-atom results are compared with DFT-based molecular dynamics simulations for aluminum in the dilute regime and for copper, aluminum and gold at solid density and different temperatures.</p>","PeriodicalId":10700,"journal":{"name":"Contributions to Plasma Physics","volume":"65 6","pages":""},"PeriodicalIF":1.3,"publicationDate":"2025-04-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/ctpp.70004","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144573115","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}
Samuel Schumacher, Julian Lütgert, Dirk O. Gericke, Mandy Bethkenhagen, Tilo Döppner, Otto L. Landen, Nathaniel R. Shaffer, Charles E. Starrett, Dominik Kraus
Under the extreme conditions found in small stars, where electron degeneracy and Coulomb coupling are significant, accurate modeling of Thomson scattering is crucial for determining opacity, a primary quantity for stellar energy transport. We use hypernetted-chain calculations, incorporating quantum pseudopotentials and electron-exchange effects to obtain the electron–electron static structure factor to calculate the Thomson scattering transport cross-section for conditions prevailing in the interior of small stars. These results are compared to those from average-atom simulations and analytical calculations. Our findings support laboratory astrophysics experiments aimed at benchmarking opacity models for stellar interiors, particularly for red dwarf stars, and help to bridge theoretical models with observations.
{"title":"Modelling Thomson Scattering in a Hydrogen Plasma at Stellar Interior Conditions Using the Hypernetted-Chain Approach","authors":"Samuel Schumacher, Julian Lütgert, Dirk O. Gericke, Mandy Bethkenhagen, Tilo Döppner, Otto L. Landen, Nathaniel R. Shaffer, Charles E. Starrett, Dominik Kraus","doi":"10.1002/ctpp.70002","DOIUrl":"https://doi.org/10.1002/ctpp.70002","url":null,"abstract":"<p>Under the extreme conditions found in small stars, where electron degeneracy and Coulomb coupling are significant, accurate modeling of Thomson scattering is crucial for determining opacity, a primary quantity for stellar energy transport. We use hypernetted-chain calculations, incorporating quantum pseudopotentials and electron-exchange effects to obtain the electron–electron static structure factor to calculate the Thomson scattering transport cross-section for conditions prevailing in the interior of small stars. These results are compared to those from average-atom simulations and analytical calculations. Our findings support laboratory astrophysics experiments aimed at benchmarking opacity models for stellar interiors, particularly for red dwarf stars, and help to bridge theoretical models with observations.</p>","PeriodicalId":10700,"journal":{"name":"Contributions to Plasma Physics","volume":"65 8-9","pages":""},"PeriodicalIF":1.5,"publicationDate":"2025-03-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1002/ctpp.70002","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145426199","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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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