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Heliopause Stability
IF 1 4区 工程技术
Fluid Dynamics Pub Date : 2025-03-09 DOI: 10.1134/S0015462824605114
M. S. Ruderman
{"title":"Heliopause Stability","authors":"M. S. Ruderman","doi":"10.1134/S0015462824605114","DOIUrl":"10.1134/S0015462824605114","url":null,"abstract":"<p>Interaction of the supersonic wind with the supersonic flow of the interstellar medium results in the development of interaction region called the heliospheric interphase. It is bounded by two shocks, termination and bow. The solar wind flow compressed at the termination shock and the interstellar medium flow compressed at the bow shock are separated by a tangential discontinuity called the heliopause. An important problem related to the physical processes in the heliosphere is the heliopause stability. We present a brief review of studies of two types of instabilities that can operate at the heliopause: the Kelvin–Helmholtz (KH) instability of the heliopause flanks and the Rayleigh–Taylor instability of the part of heliopause close to the apex point. Using the local analysis the stability of the magnetic-free heliopause flanks was considered, and then the effect of the magnetic field in the interstellar medium and solar wind was discussed. The RT instability in the vicinity of the apex point can be driven by the accelerated motion of the heliospheric interface toward the interstellar medium. It was studied both in the case of constant acceleration as well as acceleration oscillating with the period of the solar cycle. Another mechanism of driving the RT instability is the charge exchange between the hydrogen atoms and ions. This kind of instability was studied for the magnetic-free heliopause.</p>","PeriodicalId":560,"journal":{"name":"Fluid Dynamics","volume":"59 8","pages":"2339 - 2352"},"PeriodicalIF":1.0,"publicationDate":"2025-03-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143581082","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"工程技术","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Application of the Thin Shock Layer Model to the Determination of the Parameters of the Envelopes of Young Stellar Objects
IF 1 4区 工程技术
Fluid Dynamics Pub Date : 2025-03-09 DOI: 10.1134/S0015462824605096
K. V. Krasnobaev
{"title":"Application of the Thin Shock Layer Model to the Determination of the Parameters of the Envelopes of Young Stellar Objects","authors":"K. V. Krasnobaev","doi":"10.1134/S0015462824605096","DOIUrl":"10.1134/S0015462824605096","url":null,"abstract":"<p>Classical problems of unsteady one-dimensional and two-dimensional explosive motions are generalized to the case of gas expansion by ionizing ultraviolet radiation in regions of active star formation. An essential feature of the developed model is the use of the ionization balance condition instead of the adiabaticity condition, which is invalid due to the interaction of gas with radiation. The model allows one to study gas dynamic phenomena in an inhomogeneous medium and in a non-stationary radiation field. The results of the calculations are compared with those obtained within the framework of the Cherny and Kompaneets approximations, and a physical interpretation of the differences that arise is given. It is analytically shown that for one-dimensional motions it is impossible to move a finite mass of gas to infinity in a finite time interval. A criterion is derived for such a two-dimensional density distribution in the gas envelope, at which a “break” of the envelope occurs in a finite time. An analysis of theoretically predicted properties of motions at different stages of the evolution of HII regions with observations is carried out. The analysis made it possible to establish new dependencies of the measured fluxes of ultraviolet, infrared and radio radiation on the parameters of the ionized and neutral gas involved in the motion.</p>","PeriodicalId":560,"journal":{"name":"Fluid Dynamics","volume":"59 8","pages":"2353 - 2361"},"PeriodicalIF":1.0,"publicationDate":"2025-03-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143581129","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"工程技术","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Asymmetric Magnetorotational Supernovae for Various Stellar Masses
IF 1 4区 工程技术
Fluid Dynamics Pub Date : 2025-03-09 DOI: 10.1134/S0015462824605060
I. A. Kondratyev, S. G. Moiseenko, G. S. Bisnovatyi-Kogan
{"title":"Asymmetric Magnetorotational Supernovae for Various Stellar Masses","authors":"I. A. Kondratyev,&nbsp;S. G. Moiseenko,&nbsp;G. S. Bisnovatyi-Kogan","doi":"10.1134/S0015462824605060","DOIUrl":"10.1134/S0015462824605060","url":null,"abstract":"<p>Asymmetry of a core-collapse supernova explosion is an effective mechanism for a large kick velocity generation of neutron stars and black holes, formed during such violent and bright events. In this work, we conduct MHD simulations of a magnetorotational supernova explosion with an offset dipole field for two progenitor models of massive stars with zero-age main sequence masses of 20 and 35 <span>({{M}_{ odot }})</span>. The offset position of the dipole field results in a development of equatorially asymmetric outflows, leading to a formation of kick velocity of the protoneturon star. The results show, that the initial mass of the massive star could strongly affect the acquired protoneutron star kicks, while their estimated values are in order of several hundreds of kilometers per second at <span>( sim 1)</span> s after the core bounce.</p>","PeriodicalId":560,"journal":{"name":"Fluid Dynamics","volume":"59 8","pages":"2458 - 2467"},"PeriodicalIF":1.0,"publicationDate":"2025-03-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143581087","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"工程技术","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Calculation of Transport Coefficients for Low-Temperature Plasma, and the Role of V. B. Baranov
IF 1 4区 工程技术
Fluid Dynamics Pub Date : 2025-03-09 DOI: 10.1134/S0015462824605205
G. S. Bisnovatyi-Kogan
{"title":"Calculation of Transport Coefficients for Low-Temperature Plasma, and the Role of V. B. Baranov","authors":"G. S. Bisnovatyi-Kogan","doi":"10.1134/S0015462824605205","DOIUrl":"10.1134/S0015462824605205","url":null,"abstract":"<p>The influence of  V.B. Baranov on the author’s work on the calculations of transport coefficients in partially ionized two-temperature plasma in magnetic field is considered, and the results of this work are presented briefly.</p>","PeriodicalId":560,"journal":{"name":"Fluid Dynamics","volume":"59 8","pages":"2333 - 2338"},"PeriodicalIF":1.0,"publicationDate":"2025-03-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143581022","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"工程技术","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Plasma-Dust Processes in Physics of Comets
IF 1 4区 工程技术
Fluid Dynamics Pub Date : 2025-03-09 DOI: 10.1134/S0015462824605126
S. I. Popel, A. P. Golub’, L. M. Zelenyi
{"title":"Plasma-Dust Processes in Physics of Comets","authors":"S. I. Popel,&nbsp;A. P. Golub’,&nbsp;L. M. Zelenyi","doi":"10.1134/S0015462824605126","DOIUrl":"10.1134/S0015462824605126","url":null,"abstract":"<p>Since cometary dust interacts with electrons and ions of the surrounding plasma, as well as with solar radiation, the dust becomes charged. As a result, it is possible to treat the medium surrounding the comet nucleus as a dusty plasma. The purpose of the present paper is to discuss plasma-dust processes in comet physics. It is shown that plasma-dust processes can have significant manifestations in the formation of the bow shock formed due to the interaction of the comet’s coma with the solar wind, as well as in situations when the comet is far from the Sun.</p>","PeriodicalId":560,"journal":{"name":"Fluid Dynamics","volume":"59 8","pages":"2392 - 2400"},"PeriodicalIF":1.0,"publicationDate":"2025-03-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143581089","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"工程技术","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Erratum to: Axisymmetric Poiseuille Flow with Temperature-Dependent Viscosity under Pressure and Temperature Gradients
IF 1 4区 工程技术
Fluid Dynamics Pub Date : 2025-03-09 DOI: 10.1134/S0015462824080019
D. V. Knyazev
{"title":"Erratum to: Axisymmetric Poiseuille Flow with Temperature-Dependent Viscosity under Pressure and Temperature Gradients","authors":"D. V. Knyazev","doi":"10.1134/S0015462824080019","DOIUrl":"10.1134/S0015462824080019","url":null,"abstract":"","PeriodicalId":560,"journal":{"name":"Fluid Dynamics","volume":"59 8","pages":"2504 - 2504"},"PeriodicalIF":1.0,"publicationDate":"2025-03-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1134/S0015462824080019.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143581268","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"工程技术","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Caustics of Interstellar Dust Particles in the Heliosphere
IF 1 4区 工程技术
Fluid Dynamics Pub Date : 2025-03-09 DOI: 10.1134/S0015462824605047
E. A. Godenko, V. V. Izmodenov
{"title":"Caustics of Interstellar Dust Particles in the Heliosphere","authors":"E. A. Godenko,&nbsp;V. V. Izmodenov","doi":"10.1134/S0015462824605047","DOIUrl":"10.1134/S0015462824605047","url":null,"abstract":"<p>Interstellar dust particles penetrate the heliosphere because of the relative motion of the Sun and the local interstellar medium. Inside the heliosphere, trajectories of dust grains deflect from the initial direction due to the action of three forces: gravitational attraction to the Sun, solar radiation pressure, and electromagnetic force. As a result, the distribution of dust grains becomes highly inhomogeneous. In our previous works, we demonstrated that under the influence of electromagnetic force, the envelopes of trajectories, or <i>caustics</i>, appear. We also studied the effects of velocity dispersion and the time-dependent magnetic field on the formation of caustics. The main goal of this work is to expand our knowledge about caustics. For this purpose, we apply two models of dust distribution in the heliosphere: 1) a kinetic model based on the solving of the kinetic equation for the velocity distribution function, and 2) a fluid cold gas model based on the solving of the continuity equation in the lagrangian form. For the first time, we perform simulations for particles of different sizes and discuss the physical reasons why the density singularities appear at the caustics. We also study the effects of combined gravity and solar radiation pressure on the dust distribution near the caustics.</p>","PeriodicalId":560,"journal":{"name":"Fluid Dynamics","volume":"59 8","pages":"2412 - 2425"},"PeriodicalIF":1.0,"publicationDate":"2025-03-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143581273","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"工程技术","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
The Influence of H–p, H–H Elastic Collisions, and Charge Transfer with Angular Scattering on the H Atom Velocity Distribution Function in a Plasma Layer 等离子体层中 H-p、H-H 弹性碰撞和角散射电荷转移对 H 原子速度分布函数的影响
IF 1 4区 工程技术
Fluid Dynamics Pub Date : 2025-03-09 DOI: 10.1134/S001546282460514X
A. V. Titova, V. V. Izmodenov
{"title":"The Influence of H–p, H–H Elastic Collisions, and Charge Transfer with Angular Scattering on the H Atom Velocity Distribution Function in a Plasma Layer","authors":"A. V. Titova,&nbsp;V. V. Izmodenov","doi":"10.1134/S001546282460514X","DOIUrl":"10.1134/S001546282460514X","url":null,"abstract":"<p>In this study, we examine the influence of hydrogen–proton (H–p) and hydrogen–hydrogen (H–H) elastic collisions, along with charge transfer with angular scattering, on the velocity redistribution of hydrogen atoms within a plasma layer. To achieve this, we developed a kinetic model to explore H atom behavior in a homogeneous plasma region, assessing how these effects influence the maxwellization of the H atom distribution function relative to the case where only charge exchange is considered. The homogeneous layer results provide a simplified but valuable demonstration of how elastic collisions impact H atom behavior, creating a foundation for future studies in more complex, spatially varying plasma environments. Calculations of the distribution functions at various distances reveal that combined H–p and H–H collisions lead to faster maxwellization and blur the distinction between hydrogen atoms that have undergone charge exchange and those that have not interacted with protons.</p>","PeriodicalId":560,"journal":{"name":"Fluid Dynamics","volume":"59 8","pages":"2435 - 2444"},"PeriodicalIF":1.0,"publicationDate":"2025-03-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143581271","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"工程技术","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Adaptive Mesh Refinement with a “Garden” Technique for Solving the Special Relativistic Hydrodynamics Equations 用 "花园 "技术自适应细化网格，求解特殊相对论流体力学方程
IF 1 4区 工程技术
Fluid Dynamics Pub Date : 2025-03-09 DOI: 10.1134/S0015462824605072
I. M. Kulikov
{"title":"Adaptive Mesh Refinement with a “Garden” Technique for Solving the Special Relativistic Hydrodynamics Equations","authors":"I. M. Kulikov","doi":"10.1134/S0015462824605072","DOIUrl":"10.1134/S0015462824605072","url":null,"abstract":"<p>When simulating relativistic gas flows, complex flows are often formed in zones that are much smaller than the entire calculation domain. The processes that take place outside such zones may greatly affect not only the behavior but also the formation of the complex flows. The use of adaptive grids is a universal method of calculation domain discretization in calculating such multi-scale flows. An approach describing adaptive grids with a “Garden” technique is proposed. As the name suggests, this approach is to divide the calculation domain into equal grid cells (an external grid), which are also divided (internal grids), and a microgrid is the atomic structure in each of the internal grids. The microgrids consist of cells whose numbers are fixed. All necessary operations are performed with the microgrids. In this paper, we use Adaptive Mesh Refinement (AMR) with the “Garden” technique for the simulation of relativistic gas flows.</p>","PeriodicalId":560,"journal":{"name":"Fluid Dynamics","volume":"59 8","pages":"2453 - 2457"},"PeriodicalIF":1.0,"publicationDate":"2025-03-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143581274","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"工程技术","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Vibrational Methods for the Symmetrization of Asymmetric Laminar Viscous Fluid Flow in a Plane Diffuser
IF 1 4区 工程技术
Fluid Dynamics Pub Date : 2025-03-09 DOI: 10.1134/S0015462824605229
A. I. Fedyushkin, A. A. Gnevushev, A. S. Zakharov
{"title":"Vibrational Methods for the Symmetrization of Asymmetric Laminar Viscous Fluid Flow in a Plane Diffuser","authors":"A. I. Fedyushkin,&nbsp;A. A. Gnevushev,&nbsp;A. S. Zakharov","doi":"10.1134/S0015462824605229","DOIUrl":"10.1134/S0015462824605229","url":null,"abstract":"<p>This paper presents the results of numerical modeling of laminar flows of a viscous incompressible fluid in a flat diffuser with and without vibration effects. Two methods of flow symmetrization in a flat diffuser are considered: by means of periodic vibration action at the inlet to the diffuser and on its walls. Modeling has shown that it is possible to symmetrize the flow of a viscous liquid in the diffuser by using a weak harmonic vibration action, the speed of which can be less than 0.01% of the speed of the main flow.</p>","PeriodicalId":560,"journal":{"name":"Fluid Dynamics","volume":"59 8","pages":"2475 - 2486"},"PeriodicalIF":1.0,"publicationDate":"2025-03-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143581088","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"工程技术","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
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