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Dissertations / Theses on the topic 'Planetary magnetic fields'

Author: Grafiati

Published: 4 June 2021

Last updated: 25 July 2025

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1

Fu, Roger R. (Roger Rennan). "Magnetic fields in the early solar system." Thesis, Massachusetts Institute of Technology, 2015. http://hdl.handle.net/1721.1/101348.

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Thesis: Ph. D., Massachusetts Institute of Technology, Department of Earth, Atmospheric, and Planetary Sciences, 2015.<br>Cataloged from PDF version of thesis.<br>Includes bibliographical references (pages 251-283).<br>The first magnetic fields in the solar system were embedded in the ionized gas of the protoplanetary disk itself. Soon after, newly formed protoplanets may have harbored magnetic core dynamos. Paleomagnetic analysis of ancient samples permits direct constraints on these early solar system magnetic fields. Here I present paleomagnetic studies of several classes of meteorites. Exp

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2

Sun, Peng, and Peng Sun. "Charged-Particle Transport in Turbulent Magnetic Fields." Diss., The University of Arizona, 2016. http://hdl.handle.net/10150/621573.

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Collisionless turbulence is common in astrophysical magnetic fields and plasmas. The determination of the transport of high-energy charged particles both parallel and perpendicular to the average magnetic field in such a system is of considerable interest. It is recognized that the turbulent magnetic field has important effects on the transport of charged particles and that the properties of different turbulence models may significantly affect the resulting transport properties. A number of different magnetic turbulence models have been proposed in the last several decades. We present here the

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3

Knapp, Mary (Mary E. ). "Toward detection and characterization of exoplanetary magnetic fields via low frequency radio observation." Thesis, Massachusetts Institute of Technology, 2018. http://hdl.handle.net/1721.1/115642.

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Thesis: Ph. D. in Planetary Sciences, Massachusetts Institute of Technology, Department of Earth, Atmospheric, and Planetary Sciences, 2018.<br>This electronic version was submitted by the student author. The certified thesis is available in the Institute Archives and Special Collections.<br>Cataloged from student-submitted PDF version of thesis.<br>Includes bibliographical references (pages 225-256).<br>Low frequency radio emission from planets is produced by the interaction of energetic charged particles from the planet's ionosphere and/or the solar wind with the planet's magnetic field. Th

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4

de, Lima Leal Ferreira Marcelo [Verfasser]. "Magnetic Fields and the Formation of Aspherical Planetary Nebulae / Marcelo de Lima Leal Ferreira." Bonn : Universitäts- und Landesbibliothek Bonn, 2015. http://d-nb.info/1077289383/34.

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5

Rees, Bryan. "A study of planetary nebulae in and towards the Galactic Bulge." Thesis, University of Manchester, 2011. https://www.research.manchester.ac.uk/portal/en/theses/a-study-of-planetary-nebulae-in-and-towards-the-galactic-bulge(ff6c0373-e5a5-491f-b5fb-bda36acac8ba).html.

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A planetary nebula (PN) consists of material, mainly gas, that has been ejected from a star on the asymptotic giant branch of its life cycle. This material emits electromagnetic radiation due to photoionization and recombination, collisional and radiative excitation or free-free radiation. The envelope of material moves outwards from the central star and may take one of a variety of shapes. These shapes are believed to be sculpted by the stellar wind, magnetic fields and interactions with a binary companion. However, within a time scale of as little as 10 000 years the nebula fades from view a

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6

Schad, Thomas Anthony. "Spectropolarimetry of Fine Magnetized Structures in the Upper Solar Atmosphere." Diss., The University of Arizona, 2013. http://hdl.handle.net/10150/301683.

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One of the earliest indications of magnetic fields acting in the solar atmosphere came at the beginning of the 20th century when George Hale noted a "decided definiteness of structure" in photographs within the Hydrogen Balmer-alpha line core. Fine structure both in the chromosphere and in the corona result from processes that are not well understood but accepted as a consequence of the solar magnetic field. Our knowledge of this field is lacking, and until recently, the assumed relationship between fine thermal structure and the magnetic field remained untested. Here, spectropolarimetric dia

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7

Guo, Fan. "Effects of Turbulent Magnetic Fields on the Transport and Acceleration of Energetic Charged Particles: Numerical Simulations with Application to Heliospheric Physics." Diss., The University of Arizona, 2012. http://hdl.handle.net/10150/255156.

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Turbulent magnetic fields are ubiquitous in space physics and astrophysics. The influence of magnetic turbulence on the motions of charged particles contains the essential physics of the transport and acceleration of energetic charged particles in the heliosphere, which is to be explored in this thesis. After a brief introduction on the energetic charged particles and magnetic fields in the heliosphere, the rest of this dissertation focuses on three specific topics: 1. the transport of energetic charged particles in the inner heliosphere, 2. the acceleration of ions at collisionless shocks, an

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8

Yu, Louise. "Recherche de Jupiters chauds autour d'étoiles jeunes." Thesis, Toulouse 3, 2019. http://www.theses.fr/2019TOU30240.

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Les 25 dernières années ont vu la détection d'environ 400 Jupiters chauds (hJs), exoplanètes géantes semblables à Jupiter mais sur des orbites cent fois plus resserrées. Ces planètes étonnantes se seraient formées loin de leur étoile avant de migrer vers elle, cependant les processus physiques à l'origine de ce transfert orbital sont encore peu contraints par les observations. Cette question, essentielle à notre compréhension de la formation des systèmes planétaires, a de profondes répercussions sur l'architecture de ces systèmes, et en particulier sur la probabilité de former des planètes tel

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9

Dimmock, Andrew. "The study of magnetic and electric field structures at planetary magnetospheres." Thesis, University of Sheffield, 2012. http://etheses.whiterose.ac.uk/2679/.

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10

Aveiro, Henrique Carlotto. "Electric and magnetic field signatures of gravity waves and 2-day planetary waves in the equatorial E-region." Instituto Nacional de Pesquisas Espaciais, 2009. http://urlib.net/sid.inpe.br/mtc-m18@80/2008/12.16.11.31.

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Observações do eletrojato equatorial (EEJ) utilizando radares VHF mostram ecos retro-espalhados em dois tipos de irregularidades de densidade eletrônica, explicadas pelas instabilidades de dois-feixes modificada (ecos Tipo I) e deriva de gradiente (ecos Tipo II). Das velocidades das irregularidades Tipo II obtidas de dados de radar, inferimos os campos elétricos verticais (E_z). A análise harmônica de tais campos mostra a presença de campos elétricos induzidos por ondas de gravidade (GW) no EEJ. Calculamos a razão entre os campos elétricos relacionados a GW e o campo elétrico vertical total. E

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11

Vidotto, Aline de Almeida. "Simulações Numéricas Tri-dimensionais de Ventos Magnetizados de Estrelas de Baixa Massa." Universidade de São Paulo, 2009. http://www.teses.usp.br/teses/disponiveis/14/14131/tde-05082010-071118/.

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O tópico abordado nesta tese é a perda de massa através de ventos coronais magnetizados em estrelas de baixa massa. Ventos estelares têm sido estudados extensivamente há vários anos, tendo inicialmente como foco o vento solar. Atualmente, sabe-se que o campo magnético é essencial na aceleração e aquecimento dos ventos coronais. Apesar do conhecimento detalhado que temos da estrutura magnética do Sol, pouco se sabe sobre a configuração do campo magnético em outras estrelas. Nesta tese, é investigada a estrutura do campo magnético nas coroas de estrelas do tipo solar na Seqüência Principal e de

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12

Yadav, Rakesh Kumar. "Effect of density stratification on dynamos in gas planets and low-mass stars." Doctoral thesis, 2015. http://hdl.handle.net/11858/00-1735-0000-0022-5FFF-D.

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13

Oliveira, Joana. "Modeling the magnetic field of mercury." Master's thesis, 2011. http://hdl.handle.net/10316/15860.

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In this thesis work I have been concerned with modeling the magnetic eld of planet Mercury. With this goal in mind, I tested a new method for modeling the time dependent magnetic eld of a planet, the Time Variable Equivalent Source Dipole method. I showed that in the case that applies to Mercury, namely a concentration of observations over the northern hemisphere, this method gives better results than the standard Spherical Harmonic method. The main conclusion of this thesis is that, assuming that the secular variation of Mercury is around one tenth of its main eld, in amplitude, the

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14

JordanVannitsen and 方喬丹. "Propagation of Solar Energetic Particles in inter-planetary space by study of the particles spreading across the Interplanetary Magnetic Field." Thesis, 2019. http://ndltd.ncl.edu.tw/handle/27x95z.

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博士<br>國立成功大學<br>航空太空工程學系<br>107<br>This thesis presents a Multi-satellite Data Analysis and Simulator Tool (MDAST), developed with the original goal to support the science requirements of a Martian 3-Unit CubeSat mission profile named Bleeping Interplanetary Radiation Determination Yo-yo (BIRDY). MDAST was firstly designed and tested by taking into account the positions, attitudes, instruments field of view and energetic particles flux measurements from four spacecraft (ACE, MSL, STEREO A, and STEREO B). The focus of this thesis will be in the period 6 December 2011 - 14 July 2012, period duri

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15

Gutynska, Olga. "Korelační vlastností fluktuací v přechodové oblasti." Doctoral thesis, 2011. http://www.nusl.cz/ntk/nusl-311483.

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Title: Correlation properties of magnetosheath fluctuations Author: Olga Gutynska Department: Department of Surface and Plasma Science Supervisor: Prof. RNDr. Jana Šafránková, DrSc. e-mail address: Jana.Safrankova@mff.cuni.cz Abstract: This thesis deals with fluctuations of the magnetic field (MF) and plasma density in different magnetosheath locations. The statistical study of the correlation length of these quantities has shown that these lengths are surprisingly low for both the ion flux and MF (approx. 1 RE). However, the correlation length increases with an increasing correlation between

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