Dissertations / Theses on the topic 'Planetary bodies'
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Romeo, Michael Joseph. "Routing Among Planetary Bodies." Kent State University / OhioLINK, 2018. http://rave.ohiolink.edu/etdc/view?acc_num=kent1528470515838277.
Chabot, Nancy Lynne. "Geochemical studies of the cores of terrestrial planetary bodies." Diss., The University of Arizona, 1999. http://hdl.handle.net/10150/289052.
Harri, Ari-Matti. "In situ obreviations of the atmospheres of terrestrial planetary bodies /." Helsinki : Finn. Meteorological Inst, 2005. http://www.gbv.de/dms/goettingen/509702546.pdf.
Hilbert, Bryan (Bryan Nathaniel) 1977. "Stellar occultation lightcurve modeling for elliptical occulting bodies." Thesis, Massachusetts Institute of Technology, 2001. http://hdl.handle.net/1721.1/54444.
Includes bibliographical references (leaf 41).
We present a new method of calculating model lightcurves for stellar occultations by the Jovian planets. We model the occulting planet as a three-dimensional body of non-zero ellipticity, and define two ellipses of intersection with the body which dictate the appearance of the lightcurve. These include the visible-limb plane ellipse, which is the observed figure of the body as seen in the sky, and the line-of-sight ellipse, which contains the line of sight to the occulted star, and is the plane in which the starlight is refracted. The observed stellar flux during the occultation is primarily dictated by the ellipticity and subsequent radius of curvature of the instantaneous ellipse in the line-of-sight plane. This new method is applied to several test cases, as well as to the Jovian occultation of HIP9369 on 10 October 1999. Lightcurves generated by this model are compared to identical situations using the method published in Hubbard et al. (1997), showing that the Hubbard model works well for low-latitude occultations, but fails at higher latitudes. In the case of the high-latitude Jovian occultation, the best-fit lightcurve, produced from this new method, yielded a half-light equatorial radius of 71,343±1.2 km with a scale height of 19.25±0.5km, and an isothermal temperature of 139K. The same data, fit using a lightcurve generated by the method described in Hubbard et al. (1997), resulted in a half-light equatorial radius of 71,819km with a scale height of 17.9km with errors comparable to the previous fit, resulting in an isothermal temperature of 129K. Lightcurves are numerically generated for an ellipsoidal planet and, for comparison, an approximation to the ellipsoidal case consisting of a sphere with radius equal to the radius of curvature of the ellipsoid at the half-light point. We find that in the case of an occultation where the line-of-sight ellipticity does not vary, that the radius of curvature approximation matches the ellipsoidal planet lightcurve to within 0.007%. For an oblique occultation however, the line-of-sight ellipticity varies, and the approximation, using only a single radius of curvature sphere, is only good to about 1%. As a result, we find that using a model such as that presented in Baum and Code (1953) to fit the lightcurve of an ellipsoidal planet can return values for half-light radius (after accounting for the distance between the center of curvature and the center of the body) which may match the local distance to the center of the ellipsoid to a fraction of a percent, while returning values of scale height which may be in error by several percent. Test cases are also then put through numerical inversions, to obtain temperature versus pressure profiles. Test cases with spherical planets return temperature profiles that match those used to create the lightcurves, while test cases with ellipsoidal planets return temperature profiles which can differ from the input temperatures by tens of degrees, assuming a constant local gravity over the course of the occultation.
by Bryan Hilbert.
S.M.
Theis, Karen Julia. "Iron isotope fractionation of planetary bodies during early solar system formation processes." Thesis, University of Manchester, 2008. http://www.manchester.ac.uk/escholar/uk-ac-man-scw:163898.
Kanata, Sayaka. "Research on Localization and Guidance for Space Rovers on Small Planetary Bodies." 京都大学 (Kyoto University), 2010. http://hdl.handle.net/2433/123338.
Ruprecht, Jessica Dawn. "Astronomical studies of solar system bodies 2060 Chiron and 1 Ceres." Thesis, Massachusetts Institute of Technology, 2013. http://hdl.handle.net/1721.1/82301.
Cataloged from PDF version of thesis.
Includes bibliographical references (p. 43-45).
In this thesis two separate projects are investigated, a stellar occultation by 2060 Chiron and rotationally resolved spectra of 1 Ceres. On 29 November 2011 UT, 2060 Chiron occulted a 14-mag star; data were successfully obtained at the 3-m IRTF on Mauna Kea and 2-m Faulkes North Telescope at Haleakala. The IRTF lightcurve shows a solid-body detection of Chiron's nucleus with a chord lasting 16.04 seconds, corresponding to a chord length of 158±14 km. Symmetric, dual extinction features in the Faulkes light curve indicate the presence of optically thick material roughly 300 km from the body midpoint. The duration of the features indicates a ~ 3 km feature separated by 10-14 km from a second - 7 km feature. The symmetry, optical thickness, and narrow size of these features allows for the intriguing possibility of a near-circular arc or shell of material. Rotationally resolved spectra of Ceres in the 0.43-0.85 micron range were observed using the DeVeny spectrograph on the Perkins 72-inch telescope at Lowell Observatory. Spectral differences as a function of phase were investigated. It is concluded that Ceres' surface is uniform at the 1% level at visible wavelengths. Additionally, the 0.6 and 0.67 pm features reported by Vilas and McFadden [1992] and Fornasier et al. [1999] are not seen at any phase at the 1% level.
by Jessica Dawn Ruprecht.
S.M.
Bryson, James Francis Joseph. "The origin of ancient magnetic activity on small planetary bodies : a nanopaleomagnetic study." Thesis, University of Cambridge, 2015. https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.708801.
Bettella, Alberto. "Generation and propagation of vibrations on satellite structures and planetary bodies after hypervelocity impacts." Doctoral thesis, Università degli studi di Padova, 2008. http://hdl.handle.net/11577/3425965.
Alibay, Farah. "Evaluation of multi-vehicle architectures for the exploration of planetary bodies in the Solar System." Thesis, Massachusetts Institute of Technology, 2014. http://hdl.handle.net/1721.1/87476.
Cataloged from PDF version of thesis.
Includes bibliographical references (pages 193-210).
Planetary exploration missions are becoming increasingly complex and expensive due to ever more ambitious scientific and technical goals. On the other hand, budgets in planetary science have suffered from dramatic cuts over the past decade and projections estimate a flat budget of approximately $1.2B/year for the upcoming years. This has led to a desire for a reduction in the risk and complexity, as well as an increase in the robustness and reliability, of planetary exploration vehicles. One of the methods proposed to deal with this issue is the use of distributed, multi-vehicle architectures as a replacement for the traditional large, monolithic systems used in flagship missions. However, mission concept formulation engineers do not possess the tools to include multi-vehicle architectures in their early trade space exploration process. This is mostly due to the fact that these types of architectures cannot be readily evaluated against monolithic systems through the use of traditional mass-based metrics. Furthermore, in multi-vehicle system, architectural decisions about one vehicle, such as instrument or capability selection, quickly propagate through the entire system and impose requirements on the other vehicles. This can be difficult to model without going through detailed point designs. The objective of this thesis is to explore the potential benefits of both spatially and temporally distributed multi-vehicle systems, where the vehicles are heterogeneous, as compared to monolithic systems. Specifically, a set of metrics mapping the effects of using multi-vehicle systems on science benefit, complexity, mass, cost, coverage, productivity and risk are developed. Furthermore, a software tool to simulate the performance of teams of planetary surface vehicles in their operational environment has been built and its use demonstrated. Finally, the framework put forward in this thesis is used to perform several case studies, including a case study on the exploration of the Jovian moon Europa and another on the ascent and return components of a Mars Sample Return mission. From these, distributed systems are shown to provide increased science return and robustness as well as lower development and manufacturing costs as compared to their monolithic equivalents.
by Farah Alibay.
Ph. D.
Schmedemann, Nico [Verfasser]. "On the Chronostratigraphy of Planetary Satellites and Asteroids : Absolute Surface Age Determination of Small Planetary Bodies: Scaling the Lunar Crater Chronology System / Nico Schmedemann." Berlin : Freie Universität Berlin, 2016. http://d-nb.info/108166021X/34.
Grimm, Robert E. (Robert Earl). "I. Aspects of lithospheric evolution on Venus. ; II. Thermal and collisional histories of chondrite parent bodies." Thesis, Massachusetts Institute of Technology, 1988. http://hdl.handle.net/1721.1/52901.
Person, Michael James. "The use of stellar occultations to study the figures and atmospheres of small bodies in the outer solar system." Thesis, Massachusetts Institute of Technology, 2006. http://hdl.handle.net/1721.1/37278.
Includes bibliographical references (p. 111-117).
The methods of analyzing stellar occultations by small bodies in the outer solar system are discussed with examples from Triton, Pluto, and Charon. Simulations were performed characterizing the analysis of multi-chord occultations including: the effects of the direction of residual minimization in figure fits, the complications in measuring the reliability of fitted figure parameters when there are few degrees of freedom, and the proper treatment of grazing chords in model fitting. The 2005 July 11 C313.2 stellar occultation by Charon was analyzed. Occultation timings from the three published data sets were combined to accurately determine the mean radius of Charon: 606.0 ± 1.5 km. The analysis indicates that a slight oblateness in the body (0.006 ± 0.003) best matches the data, with a confidence level of 86%. Charon's mean radius corresponds to a bulk density of 1.63 0.07 g/cm3, which is significantly less than Pluto's (1.92 ± 0.12 g/cm3), consistent with an impact formation scenario in which at least one of the impactors was differentiated. The 2002 August 21 P131.1 and the 1988 June 9 P8 stellar occultations by Pluto were analyzed.
(cont.) The ellipticity of Pluto's atmosphere as measured by the P131.1 event is 0.066 ± 0.040, with a Gaussian confidence level of 63%, and the ellipticity as measured by the P8 occultations is 0.091 ± 0.041, with a Gaussian confidence level of 70%. If this non-sphericity is confirmed, its size and variation could possibly be attributed to super-rotating winds driven by sources such as surface frost migration due to changing insolation patterns or albedo properties, gravity waves, and an asymmetric mass distribution in Pluto itself. The 2001 August 23 Tr231 stellar occultation by Triton was analyzed. The half-light radius of Triton's atmosphere was calculated from astrometrically calibrated model fits to the occultation light curve. The resulting half-light radius of 1479.01 km is larger than the value of 1456.3 km derived from the 1997 Trl80 occultation, with a confidence of 77% derived from the uncertainty in the astrometric calibration. If this increase were confirmed, it would indicate that the expansion of Triton's atmosphere detected between the 1989 Voyager 2 observations the 1995 and 1997 stellar occultations by Triton has continued through 2001.
by Michael James Person.
Ph.D.
Lomax, Jamie R., John P. Wisniewski, Carol A. Grady, Michael W. McElwain, Jun Hashimoto, Tomoyuki Kudo, Nobuhiko Kusakabe, et al. "CONSTRAINING THE MOVEMENT OF THE SPIRAL FEATURES AND THE LOCATIONS OF PLANETARY BODIES WITHIN THE AB AUR SYSTEM." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622048.
Molaro, Jamie. "Stress, on the Rocks: Thermally Induced Stresses in Rocks and Microstructures on Airless Bodies, Implications for Breakdown." Diss., The University of Arizona, 2015. http://hdl.handle.net/10150/593618.
Vernisse, Yoann Edwin Verfasser], and Karl-Heinz [Akademischer Betreuer] [Glassmeier. "Classification of the interactions of planetary bodies with stellar winds by hybrid simulation / Yoann Edwin Vernisse ; Betreuer: Karl-Heinz Glassmeier." Braunschweig : Technische Universität Braunschweig, 2014. http://d-nb.info/1175820679/34.
Burmeister, Steffi [Verfasser], Jürgen [Akademischer Betreuer] Oberst, Jürgen [Gutachter] Oberst, and Jürgen [Gutachter] Kusche. "Determining rotational elements of planetary bodies : method and implementation of an inertial frame bundle block adjustment / Steffi Burmeister ; Gutachter: Jürgen Oberst, Jürgen Kusche ; Betreuer: Jürgen Oberst." Berlin : Technische Universität Berlin, 2017. http://d-nb.info/1156271487/34.
Ennis, Courtney. "Spectroscopic identification of complex species containing water and ammonia and their importance to icy outer solar system bodies." University of Western Australia. Chemistry Discipline Group, 2009. http://theses.library.uwa.edu.au/adt-WU2009.0110.
Nascimento, Sanzia Alves do. "Intera??o estrela planeta: sobre o magnetismo de planetas gigantes gasosos." Universidade Federal do Rio Grande do Norte, 2012. http://repositorio.ufrn.br:8080/jspui/handle/123456789/16620.
Coordena??o de Aperfei?oamento de Pessoal de N?vel Superior
In this thesis we analyze the effects that the presence of a near gas giant planet can cause in its host star. It has been argued that the star planet interaction can cause changes in the coronal and chromospheric stellar activity. With this in mind, we analyze a sample of 53 extrasolar planets orbiting F, G and K main sequence stars, among them three super-Earths. In this analysis, we look for evidence of changes in the chromospheric activity due to the proximity of the giant planet. We show that, so far, there is not enough evidence to support such a hypothesis. Making use of the same sample and also taking in account available data for the Solar System, we revisit the so-called magnetic Bode s law. This law proposes the existence of a direct relationship between magnetism and rotation. By using estimations for the stellar and planetary magnetic momentM and the angular momentumL, we construct a Blackett s diagram (logL logM). In this diagram is evident that the magnetic Bode s law is valid for both the Solar System and the new planetary systems
Nesta tese s?o analisados os efeitos que a presen?a de um planeta gigante gasoso pr?ximo causa em sua estrela hospedeira. Tem se discutido que a intera??o estrela - planeta possa provocar mudan?as na atividade cromosf?rica e coronal estelar. Tendo isto em mente, analisamos uma amostra composta por 53 planetas extrassolares orbitando estrelas F, G e K da sequ?ncia principal, dentre os quais tr?s superterras. Nesta an?lise, buscamos ind?cios de mudan?as na atividade cromosf?rica estelar devido ? proximidade do planeta gigante. Mostramos que n?o existem evid?ncias suficientes que corroborem tal hip?tese. Fazendo uso desta mesma amostra e de dados dispon?veis na literatura para o Sistema Solar, revisitamos a chamada lei magn?tica de Bode. Esta lei prop?e a exist?ncia de uma rela??o direta entre magnetismo e rota??o. Atrav?s de estimativas para o momento magn?tico M e para o momentum angular L destes objetos, constru?mos e analisamos detalhadamente o diagrama de Blackett (logL logM). Neste diagrama ficou evidente que a lei magn?tica de Bode ? v?lida tanto para o Sistema Solar quanto para os novos sistemas planet?rios
Deligny, Cécile. "Origine des éléments volatils et chronologie de leur accrétion au sein du Système Solaire interne : Apport de l'analyse in-situ des achondrites." Electronic Thesis or Diss., Université de Lorraine, 2021. http://www.theses.fr/2021LORR0329.
Volatile elements such as hydrogen and nitrogen control the evolution of planetary bodies and their atmospheres, and are essential elements for the development of life on Earth. Nevertheless, the origin of volatile elements and the timing of their accretion by terrestrial planets formed in the inner solar system remains a subject of debate and controversy in planetary science. To answer these questions, the isotopic ratios of hydrogen (D/H) and nitrogen (15N/14N) are powerful tools to trace the origin (solar, chondritic or cometary) of volatile elements trapped in planetary bodies. Therefore, to constrain the source(s) of volatile elements trapped in rocky planets, we analyzed hydrogen and nitrogen contents and isotopic compositions by ion microprobe (LGSIMS) in achondrites that originate from asteroids or from planets that are assumed to have formed in the inner solar system. These meteorites preserve a record of the initial stages of the formation of their parent bodies and can constrain the early evolution of planetary volatile elements. In-situ analysis by SIMS is a quasi-non-destructive technique, which permits to measure the abundance and the isotopic composition of volatile elements of different phases in terrestrial, extraterrestrial and synthetic samples. The recent development of the protocol of nitrogen analysis in silicate samples by ion probe allows us to target tens of micron- sized objects (i.e., glassy melt inclusions). Volatile elements were measured in melt inclusions trapped in minerals and in interstitial glasses. Although the analysis of nitrogen in aubrites was unsuccessful, the analysis performed on Martian meteorites and angrites revealed the presence of a large amount of water and nitrogen within these meteorites. In particular, the study of angrites and more precisely the meteorite D'Orbigny allowed us to highlight the presence of water and nitrogen having isotopic composition similar to those of the primitive meteorites formed in the outer solar system (i.e., CM-like carbonaceous chondrites). These results imply that these volatile elements must have been present in the inner solar system within the first ~4 Ma after CAI formation (i.e., the first solids to form in the solar system) and may have been trapped by the terrestrial planets during their formation. Furthermore, the analysis of Martian meteorites and more particularly of Chassigny revealed the presence of nitrogen with an isotopic composition enriched in 15N compared to enstatite chondrites and terrestrial diamonds which are believed to record the most primitive value of nitrogen on Earth
Iagnemma, Karl Dubowsky S. "Mobile robots in rough terrain : estimation, motion planning, and control with application to planetary rovers /." Berlin ; New York : Springer, 2004. http://www.loc.gov/catdir/toc/fy0606/2004106986.html.
"Isotopic Investigations of Meteoritic Materials: From Earliest-Formed Solids to Planetary Bodies." Doctoral diss., 2016. http://hdl.handle.net/2286/R.I.41284.
Dissertation/Thesis
Doctoral Dissertation Geological Sciences 2016
Masoumzadeh, Jouzdani Nafiseh. "Surface reflectance analysis of small bodies on different scales." Doctoral thesis, 2015. http://hdl.handle.net/11858/00-1735-0000-0022-6075-E.
Liao, Chen-yuan, and 廖振淵. "A Study of Magnetic Polishing for SUS304 Curve Surface with Planetary Bodies Combined Two-Dimensional Vibration." Thesis, 2013. http://ndltd.ncl.edu.tw/handle/73817624674849029840.
國立中央大學
機械工程學系在職專班
101
Abstract The normal vibration directions of vibration-assisted magnetic abrasive finishing are all parallel or perpendicular to the surface of workpiece. It’s shortcomings are easily lead to more scratches on the surface, and difficult to obtain mirror effect. A study of magnetic polishing for SUS304 with planetary bodies combined two-dimensional vibration. The main purpose of the planetary bodies of rotation and revolution characteristics, excellent surface morphology, and saving energy and time can also be reached. Series of experiments by controlling the working gap, the amplitude of the vibration platform, steel particle size and so on. This mechanism can enhance the surface quality and efficiency. Taguchi experiment show that the combination of better parameters for the surface improvement : working gap 1 mm, the amplitude of the vibration platform 0.1mm, steel particle size of 0.125 mm , SiC weight of 3 g, steel weight of 0.5 g * 2, the weight of the slurry 5g, vibration platform frequency of 16.667Hz, magnet pole rotational speed 500 rpm (156). For the curve improvement : working gap 0.5 mm, the amplitude of the vibration platform 0.1mm, steel particle size of 0.125 mm , SiC weight of 3 g, steel weight of 0.5 g * 2, the weight of the slurry 5g, vibration platform frequency of 16.667Hz, magnet pole rotational speed 500 rpm (156). This mechanism can be effective in improving the stainless surface S.R. from Ra 0.23 μm to 0.058 μm, improvement rate was 74% and improving the stainless curve S.R. from Ra 0.23 μm to 0.058 μm, improvement rate was 74%. which can prove that planetary bodies combination of the two-dimensional vibration support mechanisms to improve quality. Keywords: planetary bodies, two-dimensional vibration, polished stainless steel, rotation and revolution.
"Planetary Geological Science and Aerospace Systems Engineering Applications of Thermal Infrared Remote Sensing for Earth, Mars, and the Outer Bodies." Doctoral diss., 2018. http://hdl.handle.net/2286/R.I.50586.
Dissertation/Thesis
Doctoral Dissertation Geological Sciences 2018
POGGIALI, VALERIO. "Observations of Titan liquid bodies by means of the Cassini RADAR altimeter." Doctoral thesis, 2017. http://hdl.handle.net/11573/938037.
Lantukh, Demyan Vasilyevich. "Preliminary design of spacecraft trajectories for missions to outer planets and small bodies." Thesis, 2015. http://hdl.handle.net/2152/31341.
Millar, Candida Sharon. "Wellness pastoral care and women with new babies." Thesis, 2003. http://hdl.handle.net/10500/1238.
Practical Theology
M.Th.
Pohl, Leoš. "Rovnice vedení tepla a termofyzikální modelování planetek." Master's thesis, 2014. http://www.nusl.cz/ntk/nusl-336583.