APPLICATIONS: Astronomy
Investigation of the interstellar neutrals in the heliosphere
Katushkina Olga
Space Research Institute of RAS
DRIVER: To develop a model of the interstellar hydrogen distribution in the heliosphere. To apply this model for the analysis of experimental data from different spacecraft.
STRATEGY: The main idea for the solving of this problem is to use the kinetic approach for the modelling of interstellar hydrogen distribution. To do this, we solve the 7-dimension kinetic equation in 3D time-dependent case.
OBJECTIVE: To develop the model of the interstellar hydrogen destribution inside the heliosphere. It is needed for explanation and interpretation of different experimental data. From this we can obtain additional restrictions for the parameters of the Local Interstellar Medium and properties of the heliospheric boundaries.
IMPACT: Scientific effect is the following: we are going to explain different experimental data and obtain additional information on physical properties of the heliospheric boundary.
USAGE: The field of view - the investigation of the solar wind and the heliosphere.
AREA: Astronomy
Investigation of the interstellar wind interaction with surrounding interstellar medium
Izmodenov Vladislav
Space Research Institute of RAS
DRIVER: To develop universal numerical model of th interaction between the stellar wind and interstellar matter. The model should take into account multi-component nature of plasma (neutral and charged particles) and magnetic fields.
STRATEGY: The main idea for the solving of this problem is to use the kinetic approach for the modelling of interstellar hydrogen distribution. To do this, we solve the 7-dimension kinetic equation in 3D time-dependent case.
OBJECTIVE: To analyze and interpret the new experimental data obtained by Voyager-1/2 and IBEX about heliospheric boundary. And to analyze new experimental data on astrospheres around other stars.
IMPACT: New knowledge on the Local Interstellar Medium parameters as well as on the physical processes at the heliospheric boundaries and in the astrospheres.
USAGE: The field of view - the investigation of the solar wind and the heliosphere
AREA: Astronomy
Turbulent astrophysical convection and magneto-convection in compressible fast rotating spherical shells
Kuzanian Kirill
Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation of RAS
DRIVER: Modeling turbulent convection and magneto-convection and structure formation in atmospheres of giant planets andconvective zones of the Sun and stars
STRATEGY: Numerical solution of MHD equations leading convection and magnetic field generation in fast rotating stratified media with scale separation, multi-scale approach
OBJECTIVE: Understanding condition of formation of coherent structures in fast rotating highly turbulent convective media
IMPACT: understanding of origin of helicity in solar magnetic fields
USAGE: Improving analysis of space weather
AREA: Astronomy
Numerical simulations of magnetohydrodynamic processes in the solar convection zone
Getling Alexander
Moscow State Uiversity
DRIVER: Studying situations in which multiscale convection can develop in a globally unstable layer of a compressible gas
STRATEGY: It is assumed that the thermal diffusivity makes a jump at a certain height, which results in much stronger convective instavility within the thin overlying sublayer, compared to the remaining portion of the layer (the lower sublayer). Therefore, a scale-splitting phenomenon becomes possible: convective motions of two widely different scales can coexist, with the large-scale flows filling the full layer thickness and the small-scale flows being concentrated near the upper boundary.
OBJECTIVE: Studying the flow structure in the solar convection zone, where the splitting of convection scales is observed; it can substantially affect the structure of magnetic fields.
IMPACT: scientific
USAGE: Solar physics, solar-activity mechanisms
AREA: Astronomy, Mechanics
Formation of the molecular clouds in the external galaxies
Khoperskov Sergey
Sternberg Astronomical Institute
DRIVER: The aim of the project is the simulations of the structure of the molecular clouds with taking into account multiphase interstellar medium (ISM), UV background, chemical reactions, self gravity of the gas and the large scale structure of the galactic discs. The most of the molecular gas forms on the dust grain surface then an important issue is the process of the clouds formation due to dynamical segregation of the ISM dust on sizes, charge and masses of grains.
STRATEGY: The evolution 3D the galactic discs will be simulated numerically. This models should be based on the observational data for sample of the THINGS (The HI Nearby Galaxy Survey) disc galaxies. Segregation of the ISM dust due to turbulent motions within magnetized ISM and galactic halo will be simulated using the hybrid N-body/MHD approach.
OBJECTIVE: Searching of the scenarios of formation and evolution of the molecular clouds in external galaxies. Particular interest is the determination of the dominant mechanism in the process of clouds birth in an inhomogeneous interstellar medium.
IMPACT: The expected results of numerical experiments will help to explain the observed statistical characteristics of molecular hydrogen clouds in external galaxies. Also, these calculations will predict the early stages of the current star formation in galaxies. Accounting segregation of dust may explain the observed heterogeneity of the infrared radiation in the maps of external galaxies obtained by Spizer and Herschel space telescopes.
USAGE: In addition to the direct results of analysis of the properties of molecular gas in galaxies, the calculations of interest may be applicable in a wide range of astrophysical problems. The results of the simulations of the formation and evolution of molecular clouds can be used as initial conditions for the current star formation in galaxies. At the same time, a large sample of clouds allows to test different models of accretion processes. Fundamental application of the results of the calculations is the determination the diffusion mode of charged dust particles in the interstellar medium gas which is partially magnetized.
AREA: Astronomy, Plasma Physics
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