Development of the Full Lagrangian Approach for Modeling Dilute Dispersed Media Flows (a Review)

Osiptsov, A. N.

doi:10.1134/s0015462823602425

Fluid Dyn

2024

DOI: 10.1134/s0015462823602425

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Development of the Full Lagrangian Approach for Modeling Dilute Dispersed Media Flows (a Review)

A. N. Osiptsov

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2024

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Cited by 5 publications

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The unexpected role of heliospheric boundaries in facilitating interstellar dust penetration at 1–5 AU

Godenko,

Izmodenov

2024

A&A

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Aims. Interstellar dust (ISD) particles penetrate the heliosphere because of the relative motion of the local interstellar cloud and the Sun. The penetrated particles pass through the heliospheric interface, that is, the region in which solar wind and interstellar plasma interact. As a result, the ISD flow is modified after the passage through this region under the influence of electromagnetic force. The main goal of this work is to show how the heliospheric interface affects the distribution of ISD particles near the Sun. Methods. We have developed a Monte Carlo model of the ISD distribution in the heliosphere. It first takes the effects of the heliospheric interface and the rotating heliospheric current sheet into account. The effects of the heliospheric interface were probed using a global heliospheric model. Results. The computation results show that the heliospheric interface strongly influences the distribution of relatively small (radius a = 150 − 250 nm) astronomical silicates. The unexpected finding is that the heliospheric interface facilitates the penetration of a = 150 nm particles at small heliocentric distances and, particularly, to the Ulysses orbit (1 − 5 AU). We demonstrate that the deflection of ISD particles in the outer heliosheath is the principal mechanism that causes the effects of the heliospheric interface on the distribution near the Sun. The computations with different heliospheric models show that the distribution near the Sun is sensitive to the plasma parameters in the pristine local interstellar medium. Thus, we demonstrated that being measured near the Sun, the ISD may serve as a new independent diagnostics of the local interstellar medium and the heliospheric boundaries.

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The unexpected role of heliospheric boundaries in facilitating interstellar dust penetration at 1–5 AU

Godenko,

Izmodenov

2024

A&A

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Concentration and cavitation phenomena of Riemann solutions for the isothermal three-component model

Jiang,

Shen

2024

Physics of Fluids

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Riemann solutions with four different structures are explicitly derived for the one-dimensional one-velocity and one-pressure compressible three-component model under the isothermal equation of state. The vacuum and delta shock formation in the Riemann solutions for the pressureless three-component model can be specifically deduced from the corresponding ones for the above-mentioned isothermal three-component model by letting the perturbation parameter drop to zero. Additionally, the associated phenomena of cavitation and concentration are observed and explored in detail during the entire process of taking the limit.

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Peculiarities of the Interstellar Dust Distribution in the Heliosphere Induced by the Time-Dependent Magnetic Field

Godenko,

Izmodenov

2024

Fluid Dyn

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Interstellar dust enters the heliosphere due to the relative motion of the Sun and the Local Interstellar Cloud, which contains the Sun. The dynamics of interstellar dust particles is governed mainly by the electromagnetic force. The direction of this force depends on the polarity of the heliospheric magnetic field. In turn, polarity is a function of position and time and depends on the orientation of the solar magnetic dipole axis relative to the solar rotation axis. Previously it was shown that for the case when the magnetic dipole axis coincides with the solar rotation axis, the electromagnetic force acting on dust particles is directed towards the solar equatorial plane in both the northern and southern solar hemispheres. As a result, under the influence of such a force, the distribution of interstellar dust becomes highly inhomogeneous and, in particular, thin regions of increased number density (caustics) are formed. The goal of this work is to study the nature of caustics for a more realistic time-dependent model, when it is assumed that the magnetic dipole axis rotates relative to the solar rotation axis with a period of 22 years in accordance with the 22-year solar cycle. In addition, the magnetic dipole axis rotates due to the rotation of the Sun with a period of 25 days. To calculate the dust number density, the Lagrangian Osiptsov method is used. The shape and evolution of the resulting caustics are examined and the physical mechanisms of their origin are discussed. It is shown that, when taking into account time-dependent effects, caustics appear only in certain phases of the 22-year solar cycle, and then disappear.

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Development of the Full Lagrangian Approach for Modeling Dilute Dispersed Media Flows (a Review)

Cited by 5 publications

References 99 publications

The unexpected role of heliospheric boundaries in facilitating interstellar dust penetration at 1–5 AU

The unexpected role of heliospheric boundaries in facilitating interstellar dust penetration at 1–5 AU

Concentration and cavitation phenomena of Riemann solutions for the isothermal three-component model

Peculiarities of the Interstellar Dust Distribution in the Heliosphere Induced by the Time-Dependent Magnetic Field

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