Numerical simulations of mass loading in the solar wind interaction with Venus

Cover of: Numerical simulations of mass loading in the solar wind interaction with Venus |

Published by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va .

Written in English

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Subjects:

  • Numerical analysis.,
  • Venus (Planet),
  • Solar wind.,
  • Plasma interactions.,
  • Magnetohydrodynamics.,
  • Magnetic flux.

Edition Notes

Book details

StatementK. Murawski and R.S. Steinolfson.
Series[NASA contractor report] -- NASA-CR-205115., NASA contractor report -- NASA CR-205115.
ContributionsSteinolfson, R. S., United States. National Aeronautics and Space Administration.
The Physical Object
FormatMicroform
Pagination1 v.
ID Numbers
Open LibraryOL15494973M

Download Numerical simulations of mass loading in the solar wind interaction with Venus

Abstract. Numerical simulations are performed in the framework of nonlinear two - dimensional magnetohydrodynamics to investigate the influence of mass loading on the solar wind interaction with Venus.

The principal physical features of the interaction of the solar wind with the atmosphere of Venus are presented. The formation of the bow shock, the magnetic barrier, and the magnetotail are.

Numerical simulations are performed in the framework of nonlinear two-dimensional magnetohydrodynamics to investigate the influence of mass loading on the solar wind interaction with Venus.

The. The solar wind interaction with Venus is characterized by the mass loading of the solar wind with heavy oxygen ions which are produced by the photoionization of neutrals in the extensive ionosphere. This mass loading slows down the solar wind and ultimately leads to the formation of a magnetic barrier and a by: Get this from a library.

Numerical simulations of mass loading in the solar wind interaction with Venus. [K Murawski; R S Steinolfson; United States.

National Aeronautics and Space Administration.]. Numerical simulations are performed in the framework of nonlinear two-dimensional magnetohydrodynamics to investigate the influence of mass loading on the solar wind interaction with Venus.

The principal physical features of the interaction of the solar wind with the atmosphere of Venus are : K. Murawski and R. Steinolfson. The results of the numerical simulations gave a general.

TANAKA AND MURAWSKI: SOLAR WIND INTERACTION WITH VE gen atoms and showed that the solar wind is decelerated by the mass loading and that the bow shock is pushed farther from the planet. This model, however. A 2-D gasdynamic simulation of the massloaded solar wind flow around the dayside of Venus is presented.

For average ionopause conditions near km, the simulations show that mass loading from the pickup of oxygen ions produces a boundary layer of finite thickness along the ionopause.

Within this layer and toward the ionopause, the temperature decreases and the total mass density increases. A three‐dimensional MHD study of solar wind mass loading processes at Venus: Effects of photoionization, electron impact ionization, and charge exchange.

Rainer Bauske. K.G. Powell, 3D multiscale mass loaded MHD simulations of the solar wind interaction with Mars, Advances in Space Research, /S(00), 26, 10, ( Numerical simulations suggest that the conductivity of the ionosphere controls the rate of reconnection, but this has not been verified observationally.

Although solar wind properties ultimately control the interaction, the properties of the plasma that make direct contact with the magnetosphere are different than those of the solar wind. Numerical simulation of coupled equations of kinetic Alfvén wave (KAW) and ion acoustic wave is presented in the solar wind.

The nonlinear dynamical equations satisfy the modified Zakharov system of equations by taking the nonadiabatic response of the background density. The ponderomotive nonlinearity is incorporated in the wave dynamics.

The effect of Landau damping of KAW is taken into. The authors thank very much Drs S. Brecht T K. Breus ct al.: Comparative study of numerical simulations and K.

Moore for the discussion of the hybrid simulation results, and Dr S. Stahara and Professor J. Spreiter who kindly presented high resolution numerical data and figures on the GD simulation of the solar wind interaction with Venus.

We present a 3-dimensional global hybrid simulation of the interaction of the solar wind with the entire dayside of Venus. The model obstacle is half the size of Venus, and planetary Numerical simulations of mass loading in the solar wind interaction with Venus book mass loading is included self-consistently.

Results are compared to observations as well as to results from gasdynamic convected field modeling. Abstract: Our research activity in computer simulations of the solar wind interaction with the magnetosphere is reviewed.

First, results of global MHD simulation of the Earth's magnetosphere are shown. They provided us a new insight into the field-aligned current system, the structure of the magnetospheric convention, and the substorm mechanism. mass-loading conditions of the solar wind is derived making use of the 3D LMD-GCM [Gonz alez-Galindo et al., ; Chaufray et al.,] and the 3D EGM [Leblanc et al., a, b].

In this work we perform three stationary numerical simulation runs with 80 km spatial resolution and a time step equal to 1 ciwhere.

tance of au from the Sun. Closer to the Sun, a larger mass-loading of the solar wind results in a di erent dynamical regime v SW B E conv v cometary ions SOLAR WIND Fig.

A simplistic view of light mass-loading: energy and momentum are transferred from the solar wind (red streamlines) to the cometary ions (blue dots) in a pick up process. Venus has intrigued planetary scientists for decades because of its huge contrasts to Earth, in spite of its nickname of “Earth’s Twin”.

Its invisible upper atmosphere and space environment are also part of the larger story of Venus and its evolution. In 60s to 70s, several missions (Venera and Mariner series) explored Venus-solar wind interaction regions.

model the interaction of the solar wind with the plasma tail of a comet by means of numerical simulations, taking into account the effects of viscous-like forces. Methods.A 2D hydrodynamical, two species, finite di fference code has been developed for the. These results were published in the article entitled "Numerical simulations of mass loading in the solar wind interaction with Venus" in Journal of Geophysical Research, Vol., 5.

3-D Numerical modeling of the solar wind interaction with Venus The large scale (global) interaction of atmosphere of Venus with the. Energy spectra in the solar wind and in numerical simulations 32 Numerical simulations: spectral indices in 80 independent snapshots, separated by a turnover time.

Solar wind observations: spectral indices in 15, independent measurements. (From tofit from £ to £ Hz) S.B., J. Perez, J Borovsky &. Numerical simulation of wind loading on ground-mounted solar panels at different flow configurations.

Shademan, a R.M. Barron, a b R. Balachandar, a c H. Hangan d. a Department of Mechanical, Automotive and Materials Engineering, University of. We simulate the solar wind interaction with Mars with the help of a three-dimensional MHD model, which includes mass loading by photoionization, electron impact ionization and charge exchange.

His research focuses on comparative magnetospheric physics with an emphasis on the numerical simulation of space plasmas using hybrid (kinetic ion, fluid electron) and multi-fluid techniques. Delamere has studied the solar wind interaction with the giant magnetospheres of Jupiter and Saturn, comets, Pluto and the plasma interaction at Io.

Figure 3 was chosen to illustrate an example when the mass loading strongly deflects the solar wind flow. The mass of new ions, X+, added into the solar wind was assumed to be artificially high, times the mass of O+ ions, and Fig.

3 gives a snapshot of the simulation at s after the solar wind enters in the simulation box. The solar wind.

determine the loads produced by wind action on a solar panels array, for different angles of attack and the simulation consisted in wind acting upon a group of 12 solar panels placed in perpendicular rows of 4x3 array, placed at the ground level.

CFD Simulation Cases The numerical simulation was developed using ANSYS 12 CFX code. In general, these unusual conditions help to highlight the role(s) numerical simulations can play in exploring the wide parameter space of the Venus-solar wind interaction, present and past.

11 Modeling Work Numerical Simulations of the Global Solar Wind Interaction By the time the Venus Express mission arrived at Venus, the ability to. Jubayer, Chowdhury, and Hangan, Horia. "Numerical Simulations of Wind Effects on an Array of Ground Mounted Solar Panels." Proceedings of the ASME 4th Joint US-European Fluids Engineering Division Summer Meeting collocated with the ASME 12th International Conference on Nanochannels, Microchannels, and Minichannels.

This volume is a collection of recent advancements in the study of Earth-affecting solar transients, including major solar flares, coronal mass ejections (CMEs), interplanetary CMEs (ICMEs), solar energetic particle (SEP) events, and corotating interaction regions (CIRs).

The interaction of the solar wind electrons in the optical umbra of Venus with the planetary atmosphere - the origin of the nighttime ionosphere, J. Geophys. Res., 84,Gombosi, et al., Anisotropy of cosmic radiation in the Galaxy, Nature, @article{osti_, title = {Numerical modeling of the interaction of the solar wind with cometary plasma}, author = {Lipatov, A.S.}, abstractNote = {Using the collisionless particle-in-a-cell method, the author investigates the magnetic field dynamics and the processes of interaction of the solar wind with heavy cometary ions.

He discusses the results of the calculation of the parameters. Numerical simulation of solar magneto-convection Manfred Schussler¨ Max-Planck-Institut fur¨ Aeronomie, Max-Planck-Str. 2, Katlenburg-Lindau, Germany ([email protected]) Abstract.

Numerical simulations of the interaction of magnetic field and solar surface convection are reviewed. Emphasis is laid upon the. Simulations of the flow past solar panels in an arrayed configuration are also conducted to investigate the effect of longitudinal spacing between the panels on the wind loading.

Results from the flow past the stand-alone panel reveal that the structure experiences maximum values of wind loading at two azimuthal wind directions of θ = 0° and. The interaction of the solar wind with the Martian (Sauer et al., ).

Mass loading of the solar wind by plan-etary ions can partly be taken into account by gas dynamics ertial length in the solar wind. The size of the simulation domain is defined by −≤X≤+Martian radii. A kinetic study of solar wind mass loading and cometary bow shocks, (). Numerical simulation of fluid flow with strong shocks, ().

The solar wind interaction with Venus. Numerical simulations suggest that the conductivity of the ionosphere controls the rate of reconnection but this has not been verified observationally.

While solar wind properties ultimately control the interaction, the properties of the plasma that makes direct contact with the magnetosphere are different than those of the solar wind, having. The draping of tubes of solar magnetic flux around a conducting ionosphere such as that of Venus.

The flux tubes are slowed down and sink into the wake to form a tail (after Saunders and Russell ). (Click image for full size) Interaction of the solar wind with the.

(discontinuities; numerical simulation studies) 1 Introduction Unlike the Earth, Mars does not have an intrinsic mag-netic field, neglecting the recently measured crustal magnetic fields.

Therefore, the solar wind interacts directly with the ionosphere of the planet. The solar wind interaction with Mars is similar in many ways to that of. Yet, solar wind electrons and protons show different temperatures, e.g. electrons are typically cooler than protons in the fast wind while hotter in the slow wind (Marsch ) suggesting that different heating mechanisms are at work for electrons and ions.

Close Drawer Menu Close Drawer Menu Menu. Home; Journals. AIAA Journal; Journal of Aerospace Information Systems; Journal of Air Transportation; Journal of Aircraft; Journal of. SOLAR WIND AND SUPRATHERMAL ION COMPOSITION 81 energy measurement to determine both the mass/charge and mass of ions from to 30 keV/e.

Post-acceleration is required in order to measure the mass of ions of solar wind energies, which otherwise would fall below the threshold of the solid-state detector. Wind Loads on Single-Family Dwellings in Suburban Terrain: Comparing Field Data and Wind Tunnel Simulation Structures Congress Structural Engineering and Public Safety June Impact of Empirical Models for Approach Wind Exposures on Wind Loading.

The primary science objective of the Planet-B mission to Mars is to study the Martian upper atmosphere-ionosphere system and its interaction with the solar wind. An improved knowledge of the Martian magnetic field (whether it is induced or intrinsic) is needed, and will be provided by Planet-B.

In addition, a proper characterization of the neutral thermosphere structure is essential to place.MHD Simulations of Mass Loaded Boundary Layers Along the Venus Ionopause Quantitative DeteImination of Mass Loading Effects in the Solar Wind/Venusian Ionosphere Interaction: Application of a Global 3-D MHD Model MHD Modeling of the Interaction of the Solar Wind with Venus R.

.In many respects, the complex coupling between the solar wind and the interstellar medium is the quintessential example of multiscale, regional, and disparate populations (solar wind plasma, pickup ions, anomalous and galactic cosmic rays, neutral atoms) coupling across complex boundaries.

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