The Interaction of Fast Flowing Plasma with Non-Magnetized Solar System Bodies: A New 3D Multi-fluid MHD Model of Mars and its Applications.
dc.contributor.author | Najib, Dalal | en_US |
dc.date.accessioned | 2011-06-10T18:18:03Z | |
dc.date.available | NO_RESTRICTION | en_US |
dc.date.available | 2011-06-10T18:18:03Z | |
dc.date.issued | 2011 | en_US |
dc.date.submitted | en_US | |
dc.identifier.uri | https://hdl.handle.net/2027.42/84512 | |
dc.description.abstract | This dissertation presents numerical simulation results of the interaction of Mars ionosphere with the solar wind plasma using our new multi-fluid model, and the application of the model to Venus. Our study starts with a multispecies Magnetohydrodynamics (MHD) single- fluid model. It contains four ion species, H+, O+2 , O+ and CO+2 and includes an extensive chemistry model. We modify our existing single fluid model and solve the multi-fluid equations. This results in the ion species being decoupled, that is each one has its own density, velocity and pressure. We use a spherical adaptive grid system to obtain a very good altitude resolution (10km) and set the lower boundary at 100 km altitude in order to include the ionospheric region in our simulation. Our results show clear asymmetries in the X-Z plane due to the effect of the electric field on the decoupled ions. These asymmetries, similar to the ones observed by kinetic models, could not be observed by the single fluid MHD model and show us a new distribution of the ions around the planet, a distinct magnetic field configuration and different escape fluxes. The model results agree well with Mars Global Surveyor (MGS) and Viking observations. We use our Mars model to study the effect of different upstream conditions, the hot ionospheric oxygen corona and the crustal magnetic field. These applications show a clear change in the bow shock location and the ion distribution. Finally, we successfully apply our multi-fluid model to Venus thus illustrating the versatility of our model. We reproduce the physical processes (asymmetries) calculated in Mars' case and observe, as expected, that kinetic effects are less pronounced in Venus' case. We use our model to study the effects of different solar wind conditions and we compare our results to observations by Pioneer Venus Orbiter (PVO) and Venus Express (VEX). Our results reproduce observed bow shock positions and show a reasonable fit to the data. | en_US |
dc.language.iso | en_US | en_US |
dc.subject | The Interaction of Fast Flowing Plasma With Non-Magnetized Solar System Bodies: a New 3D Multi-fluid MHD Model of Mars and Its Applications | en_US |
dc.title | The Interaction of Fast Flowing Plasma with Non-Magnetized Solar System Bodies: A New 3D Multi-fluid MHD Model of Mars and its Applications. | en_US |
dc.type | Thesis | en_US |
dc.description.thesisdegreename | PhD | en_US |
dc.description.thesisdegreediscipline | Atmospheric and Space Sciences | en_US |
dc.description.thesisdegreegrantor | University of Michigan, Horace H. Rackham School of Graduate Studies | en_US |
dc.contributor.committeemember | Nagy, Andrew F. | en_US |
dc.contributor.committeemember | Toth, Gabor | en_US |
dc.contributor.committeemember | Bougher, Stephen | en_US |
dc.contributor.committeemember | Liemohn, Michael Warren | en_US |
dc.contributor.committeemember | Ma, Yingjuan | en_US |
dc.contributor.committeemember | Powell, Kenneth G. | en_US |
dc.subject.hlbsecondlevel | Atmospheric, Oceanic and Space Sciences | en_US |
dc.subject.hlbtoplevel | Science | en_US |
dc.description.bitstreamurl | http://deepblue.lib.umich.edu/bitstream/2027.42/84512/1/dnajib_1.pdf | |
dc.owningcollname | Dissertations and Theses (Ph.D. and Master's) |
Files in this item
Remediation of Harmful Language
The University of Michigan Library aims to describe library materials in a way that respects the people and communities who create, use, and are represented in our collections. Report harmful or offensive language in catalog records, finding aids, or elsewhere in our collections anonymously through our metadata feedback form. More information at Remediation of Harmful Language.
Accessibility
If you are unable to use this file in its current format, please select the Contact Us link and we can modify it to make it more accessible to you.