Thematische Bibliographien / Planetary bodies

Auswahl der wissenschaftlichen Literatur zum Thema „Planetary bodies“

Autor: Grafiati
Veröffentlicht am 8. Juni 2024

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Zeitschriftenartikel zum Thema "Planetary bodies"

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Hu, H., und B. Wu. „PLANETARY3D: A PHOTOGRAMMETRIC TOOL FOR 3D TOPOGRAPHIC MAPPING OF PLANETARY BODIES“. ISPRS Annals of Photogrammetry, Remote Sensing and Spatial Information Sciences IV-2/W5 (29.05.2019): 519–26. http://dx.doi.org/10.5194/isprs-annals-iv-2-w5-519-2019.

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<p><strong>Abstract.</strong> Planetary remote sensing images are the primary datasets for high-resolution topographic mapping and modeling of the planetary surfaces. However, unlike the mapping satellites for Earth observations, cameras onboard the planetary satellites generally present special imaging geometries and configurations, which makes the stereo photogrammetric process difficult and requires a large number of manual interactions. At the Hong Kong Polytechnic University, we developed a unified photogrammetric software system, namely Planetary3D, for 3D topographic mapping modeling of various planetary bodies using images collected by various sensors. Planetary3D consists of three modules, including: (1) the pre-processing module to deliver standardized image products, (2) the bundle adjustment module to alleviate the inconsistencies between the images and possibly the reference frame, and (3) the dense image matching module to create pixel-wise image matches and produce high quality topographic models. Examples of using three changeling datasets, including the MRO CTX, MRO HiRISE and Chang’E-2 images, have revealed that the automatic pipeline of Planetary3D can produce high-quality digital elevation models (DEMs) with favorable performances. Notably, the notorious jitter effects visible on HiRISE images can be effectively removed and good consistencies with the reference DEMs are found for the test datasets by the Planetary3D pipeline.</p>
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Kadish, Jon, J. R. Barber, P. D. Washabaugh und D. J. Scheeres. „Stresses in accreted planetary bodies“. International Journal of Solids and Structures 45, Nr. 2 (Januar 2008): 540–50. http://dx.doi.org/10.1016/j.ijsolstr.2007.08.008.

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Connolly, William E. „Bodies, Microbes and the Planetary“. Theory & Event 21, Nr. 4 (Oktober 2018): 962–67. http://dx.doi.org/10.1353/tae.2018.0058.

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Cockell, Charles S., und Gerda Horneck. „Planetary parks—formulating a wilderness policy for planetary bodies“. Space Policy 22, Nr. 4 (November 2006): 256–61. http://dx.doi.org/10.1016/j.spacepol.2006.08.006.

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Kotliarov, I. D. „Classification of celestial bodies within planetary systems“. Moscow University Physics Bulletin 63, Nr. 6 (Dezember 2008): 416–19. http://dx.doi.org/10.3103/s0027134908060118.

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Melosh, H. J. „Ejection of rock fragments from planetary bodies“. Geology 13, Nr. 2 (1985): 144. http://dx.doi.org/10.1130/0091-7613(1985)13<144:eorffp>2.0.co;2.

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Lin, Yucong, Melissa Bunte, Srikanth Saripalli, James Bell und Ronald Greeley. „Autonomous volcanic plume detection on planetary bodies“. Acta Astronautica 97 (April 2014): 151–63. http://dx.doi.org/10.1016/j.actaastro.2013.11.029.

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Binzel, Richard P. „Small bodies looming large in planetary science“. Nature Astronomy 3, Nr. 4 (April 2019): 282–83. http://dx.doi.org/10.1038/s41550-019-0747-6.

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Skripka, V. L., und L. H. Minyazeva. „Planetary rock-breaking bodies and horizontal drilling“. Proceedings of higher educational establishments. Geology and Exploration, Nr. 5 (05.02.2023): 86–93. http://dx.doi.org/10.32454/0016-7762-2022-64-5-86-93.

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Background. The article considers one of the variants of the original planetary drilling organ, in which used multiple impacts on the mass to be destroyed. This makes it possible to improve the methods of sinking inclined and horizontal wells by significantly reducing the required feed force and reducing the energy intensity of bottom hole destructionAim. To investigate drilling methods and tools, which can be used to significantly reduce the radius of changes in drilling direction when creating inclined and horizontal wellbores.Materials and methods. An analysis of patent information and its experimental verification under laboratory conditions.Results. The main advantage of the analyzed drilling bodies is associated with their rock-breaking ability due to multiple shock pulses directed at an angle to the face surface. This allows the energy intensity of fracture and the required feed force in the axial direction to be significantly reduced, thus providing for larger wellbore diameters. A reduction in the axial length of the drilling body leads to a decrease in the radius of changes in drilling direction, thereby contributing to improved technologies of wellbore drilling, in particular, when creating horizontal wellbores.Conclusion. Planetary rock-breaking bodies implement quasi-dynamic rock destruction by multiple shock pulses and spalling off rock pieces from an automatically formed wavy face surface. On this basis, modern technologies of drilling inclined and horizontal wellbores can be improved.
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Visser, R. G., C. W. Ormel, C. Dominik und S. Ida. „Spinning up planetary bodies by pebble accretion“. Icarus 335 (Januar 2020): 113380. http://dx.doi.org/10.1016/j.icarus.2019.07.014.

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Dissertationen zum Thema "Planetary bodies"

1

Romeo, Michael Joseph. „Routing Among Planetary Bodies“. Kent State University / OhioLINK, 2018. http://rave.ohiolink.edu/etdc/view?acc_num=kent1528470515838277.

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Chabot, Nancy Lynne. „Geochemical studies of the cores of terrestrial planetary bodies“. Diss., The University of Arizona, 1999. http://hdl.handle.net/10150/289052.

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From the Earth to asteroids, numerous rocky bodies in our solar system are believed to have a metallic core at their center. However, due to the inaccessibility of these cores, fundamental issues, such as the composition of the cores or the processes of core formation and core evolution, are not well known. I have conducted both theoretical and experimental geochemical studies which have improved our understanding of the cores of terrestrial planetary bodies. The radioactive decay of K is an important planetary heat source, but the distribution of K in terrestrial planetary bodies has been debated. My experimental work, which examined the solubility of K in metal, shows no evidence for K to be an important heat source in metallic cores. The element pairs of Ag, Pd and Re, Os have been used to date core formation and core evolution events in our solar system. My experimental determination of the partitioning behavior of these important elements can be used to better understand their distribution in iron meteorites, our only samples of planetary cores. Simple fractional crystallization of a metallic core cannot explain the elemental trends observed within iron meteorite groups. I have developed a crystallization model which suggests slight inhomogeneities and mixing in the molten core were important during core evolution. As a metallic core crystallizes, liquid immiscibility may be encountered, which could significantly affect the subsequent evolution of the core. My experimental work suggests the role of liquid immiscibility during the crystallization of a metallic core is significantly smaller than the published phase diagram implies. These four topics, though each an independent project, together provide insight into the nature of the cores of terrestrial planetary bodies and the processes which affect those cores.
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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.

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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.

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Thesis (S.M.)--Massachusetts Institute of Technology, Dept. of Earth, Atmospheric, and Planetary Sciences, 2001.
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.
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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.

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The aims of this research programme were twofold: to analyse the iron isotope compositions of metal grains from ordinary chondrite meteorites over a range of class and petrographic type to investigate redox reactions and thermal metamorphism during primitive planetesimal formation; and to analyse the iron isotope composition of secondary carbonate minerals in Martian meteorite ALH84001 to determine the formation temperature and thus constrain near surface conditions on early Mars. To analyse the iron isotope compositions of these materials it was necessary to develop a methodology using a Nu Plasma multi collector inductively coupled plasma mass spectrometer and a new technique for analysing natural iron-bearing samples without first purifying them by anion exchange chromatography. The purification process can cause fractionation within the sample which may mask small natural fractionation variations. The new methodology developed here yielded reproducible iron isotope ratios to within o.osroo (20) ensuring that small isotopic variations of (i56Fe -0.06roo to 0.3sroo were resolved during the analysis of the ordinary chondrite metal grains. The method for analysing samples containing matrix elements was successful and achieved an accuracy and precision comparable to pure analyte solutions for the analysis of the Martian carbonates. The analysis of the metal grains revealed a correlation between their iron isotope compositions and the redox and thermal metamorphism that these materials have experienced. The results indicate that the degree of iron isotope fractionation can be related to thermal metamorphism temperatures, except for metal grains from type 3 chondrites. This was interpreted as resulting from the type 3 chondrites not getting hot enough during thermal metamorphism to overprint the original igneous isotopic signatures. The a-rich carbonates in ALH84001 were petrographically characterised to place them within the known carbonate assemblage sequence which implied that the zoned carbonate deposition occurred during multiple phases. The zoned carbonates were then analysed for iron isotope composition and an isotopic fractionation variation for (i56Fe of -0.6%0 was determined relative to bulk Martian silicates. This indicated a formation temperature of approximately ±800( (20) and implied that liquid water was stable on or near the surface during this time.
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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.

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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.

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Thesis (S.M.)--Massachusetts Institute of Technology, Dept. of Earth, Atmospheric, and Planetary Sciences, 2013.
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.
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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.

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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.

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Hyper-Velocity-Impacts (HVI) are a common problem in the space environment. They especially concern space missions, in terms of: Potential damage to spacecrafts and satellites Collisional evolution of small and large bodies of the Solar System. This thesis focuses on the effect of such impacts, through the analysis of the vibration field generated by HVI on both of the aforementioned cases. Referring to the first point, i.e. the HVI-induced disturbances on spacecraft internal components, a wide experimental campaign has been performed on targets representative of S/C structures, making it possible to measuring and reproducing the HVI-induced vibration field on the selected targets. The aim of this activity was to acquire data on transient waves generated after an HVI and propagating from the impact point. Such disturbances have been evaluated in from of acceleration signals. The invaluable information achievable from such an activity is related to the HVI ability of loading structures up to frequencies that are normally not explored in the standard practice for mechanical dynamic testing. These loads can damage electronic components and sensors mounted on S/C. An experimental campaign on structural components represents a unique mean of collecting data about the transient behaviour of spacecraft components subjected to HVI threat. The Study is relevant to both "simplified" (i.e. simple plates and sandwich panels made by Aluminium alloy and composite materials) and "complex" (i.e. structural assemblies including joints) targets, hit by projectiles in the range 0.6 - 2.3 mm at velocity from 2 to 5 km/s. The test-case selected for the experimental activity is the GOCE satellite, whose mission main objective is to measure the Earth's gravity field modelling the geoid with extremely high accuracy and spatial resolution. To do this, it will carry a gradiometer that is sensitive to disturbances, like the one generated by HVI. For this reason, the assessment of the vibration field that propagates after an HVI is fundamental. As a conclusion, the activity on spacecraft structures resulted in the creation of an extensive database of the disturbance field generated and propagated by HVI on simple and complex assemblies, even highlighting the dependence of the structural response from the mass and velocity of the impacting debris. The disturbance was quantified computing SRS spectra of the measured acceleration signals. This activity made also possible to evaluate the momentum transferred by the projectiles to the impacted targets. This measurement was necessary to validate the numerical technique used to extrapolate the experimental results to structures and impact conditions different from those achievable at laboratory scale with the existing hypervelocity facilities [28]. Moreover, to investigate in detail the typical features of transient disturbances, a dedicated study was implemented on the application of Wavelet Transform (WT) to the sampled acceleration signal on aluminium simple plates and honeycomb sandwich panels. WT was used to explore the complex wave generation and propagation behaviour inside these targets, thanks to its ability of identifying the following wave features: speed of propagation, type, dispersion properties and frequency content. This work led to a better understanding of the origin of disturbance field due to HVI, demonstrating that WT technique may be used to analyse the elementary constituents of transitory signals. Referring to the second point, i.e. the study of the collisional evolution of minor bodies of the Solar System, several numerical simulations were carried out to study the wave propagation on planetary-like objects. HVI characterize the evolutional story of all the small and large bodies of the Solar System. For this reason, the goal of simulations on porous materials (concrete was used as test-case in this thesis) was to obtain a better comprehension of the impact processes and to provide a tool to validate the results of numerical models, through the analysis of wave generation and propagation on different materials. The results of this activity aimed also to contribute to the data interpretation of the ground and space based observations, in particular in view of space missions such as Smart1, MarsExpress, VenusExpress, BepiColombo, Cassini-Huygens, Rosetta, Dawn. Impact experiments to investigate craterization and catastrophic disruption on planetary objects are limited due to scale effect (i.e. size of the targets, Earth gravity environment, actual performance of the modern hypervelocity facilities). Therefore, a possible method used to study the impact processes is to perform numerical simulations with hydrocodes. The main issue with these tools is the unknown response of materials to high velocity impacts, pressures of several MPa and shock wave propagation. The validation of such models implies to test with the available impact facilities small-scale targets representative of real asteroids and to match experiments and numerical simulations. Waves propagating within the impacted target can be used in the assessment of such numerical models, through the comparison of waves features like: speed, frequency and reflections. In this thesis the possibility to use an accelerometer to measure waves propagation in concrete spheres (representative of porous targets) and to identify wave features with WT is explored. For this reason, SPH (smooth particles hydrocode) simulations have been carried out on a small-scale concrete sphere to better understand the propagation of shock waves and to evaluate the load effects due to the accelerometer mass. Results show that this measurement is possible, even if it is necessary to perform it with a highly sensitive measurement chain.
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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.

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Thesis: Ph. D., Massachusetts Institute of Technology, Department of Aeronautics and Astronautics, 2014.
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.
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Bücher zum Thema "Planetary bodies"

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Mann, Ingrid, Akiko Nakamura und Tadashi Mukai, Hrsg. Small Bodies in Planetary Systems. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-76935-4.

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Nakamura, A. M., T. Mukai und Ingrid Mann. Small bodies in planetary systems. Berlin: Springer, 2009.

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Hanslmeier, Arnold, Stephan Kempe und Joseph Seckbach, Hrsg. Life on Earth and other Planetary Bodies. Dordrecht: Springer Netherlands, 2012. http://dx.doi.org/10.1007/978-94-007-4966-5.

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1929-, Teisseyre R., Leliwa-Kopystyński J. 1937-, Lang B und Bakun-Czubarow N, Hrsg. Evolution of the Earth and other planetary bodies. Amsterdam: Elsevier, 1992.

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United States. National Aeronautics and Space Administration., Hrsg. Solar wind effects on atmospheres of the weakly magnetized bodies--Mars, Titan, and the moon: Final technical report. [Washington, DC: National Aeronautics and Space Administration, 1996.

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Luhmann, Janet G. Solar wind effects on atmospheres of the weakly magnetized bodies--Mars, Titan, and the moon: Final technical report. [Washington, DC: National Aeronautics and Space Administration, 1996.

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Digitalis, Raven. Planetary spells & rituals: Practicing dark & light magick aligned with the cosmic bodies. Woodbury, Minn: Llewellyn Publications, 2010.

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Digitalis, Raven. Planetary spells & rituals: Practicing dark & light magick aligned with the cosmic bodies. Woodbury, Minn: Llewellyn Publications, 2010.

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National Research Council (U.S.). Task Group on Sample Return from Small Solar System Bodies. Evaluating the biological potential in samples returned from planetary satellites and small solar system bodies: Framework for decision making. Washington, D.C: National Academy Press, 1998.

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MEVTV, Workshop on the Evolution of Magma Bodies on Mars (1990 San Diego Calif ). MEVTV Workshop on the Evolution of Magma Bodies on Mars: Held at San Diego, California, January 15-17, 1990. Houston, Tex: The Institute, 1990.

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Buchteile zum Thema "Planetary bodies"

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Hare, Trent Michael. „Mapping planetary bodies“. In The Routledge Handbook of Geospatial Technologies and Society, 562–76. London: Routledge, 2023. http://dx.doi.org/10.4324/9780367855765-46.

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Schmedemann, Nico, Matteo Massironi, Roland Wagner und Katrin Stephan. „Small Bodies and Dwarf Planets“. In Planetary Geology, 311–43. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-65179-8_13.

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Jiwani, Yasmin. „Contagious Bodies“. In Planetary Health Humanities and Pandemics, 179–98. New York: Routledge, 2024. http://dx.doi.org/10.4324/9781003367581-12.

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Saur, Joachim, Fritz M. Neubauer und Karl-Heinz Glassmeier. „Induced Magnetic Fields in Solar System Bodies“. In Planetary Magnetism, 391–421. New York, NY: Springer New York, 2009. http://dx.doi.org/10.1007/978-1-4419-5901-0_12.

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Mittlefehldt, David W., Timothy J. McCoy, Cyrena A. Goodrich und Alfred Kracher. „Chapter 4. NON-CHONDRITIC METEORITES FROM ASTEROIDAL BODIES“. In Planetary Materials, herausgegeben von James J. Papike, 523–718. Berlin, Boston: De Gruyter, 1998. http://dx.doi.org/10.1515/9781501508806-019.

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Baur, Oliver. „Gravity Field of Planetary Bodies“. In Encyclopedia of Geodesy, 1–6. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-02370-0_46-1.

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Dwivedi, Om Prakash. „Ecoprogramming the Vulnerable Bodies“. In Eco-Anxiety and Planetary Hope, 111–18. Cham: Springer International Publishing, 2022. http://dx.doi.org/10.1007/978-3-031-08431-7_11.

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Christou, A. A. „Future Planetary Missions“. In The Dynamics of Small Bodies in the Solar System, 587–93. Dordrecht: Springer Netherlands, 1999. http://dx.doi.org/10.1007/978-94-015-9221-5_56.

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Jewitt, D. „Six Hot Topics in Planetary Astronomy“. In Small Bodies in Planetary Systems, 1–37. Berlin, Heidelberg: Springer Berlin Heidelberg, 2008. http://dx.doi.org/10.1007/978-3-540-76935-4_9.

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Hussmann, H., F. Sohl und J. Oberst. „4.2.2 Basic data of planetary bodies“. In Solar System, 208–29. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-88055-4_15.

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Konferenzberichte zum Thema "Planetary bodies"

1

Remo, John L. „Classifying Solid Planetary Bodies“. In NEW TRENDS IN ASTRODYNAMICS AND APPLICATIONS III. AIP, 2007. http://dx.doi.org/10.1063/1.2710063.

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Schulte, Mitch. „Remote sensing of planetary bodies“. In Autonomous Systems: Sensors, Processing, and Security for Ground, Air, Sea, and Space Vehicles and Infrastructure 2024, herausgegeben von Michael C. Dudzik, Theresa J. Axenson und Stephen M. Jameson. SPIE, 2024. http://dx.doi.org/10.1117/12.3023813.

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White, Robert A. „Generating Artificial Gravity on Planetary Bodies“. In 55th AIAA Aerospace Sciences Meeting. Reston, Virginia: American Institute of Aeronautics and Astronautics, 2017. http://dx.doi.org/10.2514/6.2017-1447.

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Dollfus, Audouin. „Telescopic polarimetry of planetary bodies: an overview“. In San Diego '92, herausgegeben von Walter G. Egan. SPIE, 1992. http://dx.doi.org/10.1117/12.138829.

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MARTINO, MARIO DI, ALBINO CARBOGNANI und ALBERTO CELLINO. „DETECTION OF TRANSIENT PHENOMENA ON PLANETARY BODIES“. In The 32nd Session of International Seminars and International Collaboration. WORLD SCIENTIFIC, 2005. http://dx.doi.org/10.1142/9789812701787_0053.

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Foster, Cyrus, und Matthew Daniels. „Mission Opportunities for Human Exploration of Nearby Planetary Bodies“. In AIAA SPACE 2010 Conference & Exposition. Reston, Virigina: American Institute of Aeronautics and Astronautics, 2010. http://dx.doi.org/10.2514/6.2010-8609.

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Gold, Thomas. „Reasons for expecting subsurface life on many planetary bodies“. In Optical Science, Engineering and Instrumentation '97, herausgegeben von Richard B. Hoover. SPIE, 1997. http://dx.doi.org/10.1117/12.278775.

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Picardi, Giovanni, und Roberto Seu. „Radar Sounding of Planetary Bodies: An Instrument Design Approach“. In 20th European Microwave Conference, 1990. IEEE, 1990. http://dx.doi.org/10.1109/euma.1990.336266.

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Yucong Lin, Melissa Bunte, Srikanth Saripalli und Ronald Greeley. „Autonomous detection of volcanic plumes on outer planetary bodies“. In 2012 IEEE International Conference on Robotics and Automation (ICRA). IEEE, 2012. http://dx.doi.org/10.1109/icra.2012.6224796.

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Primeau, Gilles. „Magnetoaerodynamic (MAD) propulsion for exploration of atmosphere-bearing planetary bodies“. In 34th AIAA/ASME/SAE/ASEE Joint Propulsion Conference and Exhibit. Reston, Virigina: American Institute of Aeronautics and Astronautics, 1998. http://dx.doi.org/10.2514/6.1998-3408.

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Berichte der Organisationen zum Thema "Planetary bodies"

1

Shin, Tony. The Search for Water on Planetary Bodies using Neutron Science. Office of Scientific and Technical Information (OSTI), März 2022. http://dx.doi.org/10.2172/1853890.

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Gender justice and planetary health. Global Health 50/50, 2024. http://dx.doi.org/10.56649/tauj1442.

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Dive into the critical intersection of gender justice and planetary health with our latest report. As Earth’s natural systems deteriorate, marginalised communities bear the brunt, often excluded from solutions. Our report delves into how gender considerations shape global responses to planetary health crises. Daily, communities worldwide grapple with planetary health disasters—from East Africa’s famines to Europe's wildfires. Gender differences expose individuals to varying risks, from air pollution to violence. Marginalised groups, including LGBTQ+ communities, face compounded risks due to discrimination and socioeconomic factors, emphasising the need for an intersectional approach in addressing planetary health crises. Gender justice in planetary health means equal opportunities to shape policies and decisions affecting everyone's lives. Our analysis of 114 organisations reveals gaps in gender integration in planetary health efforts. While some recognise gender inequalities' structural roots, many overlook gender entirely. Transformative gender justice demands inclusive leadership. While progress has been made in gender parity, disparities persist—particularly in representation from low- and middle-income countries. This report complements our annual Global Health 50/50 Report, highlighting organisations’ commitments to gender equality in global health. Key findings: 24% of non-profit organisations recognised structural causes of gender inequalities in their planetary health activities 37% of organisations did not mention gender in their planetary health activities. 38% of organisations focused solely on addressing the needs of women and girls. None of the organisations specifically addressed the gender roles of men/boys. 38% of CEOs in non-profit organisations were women. 48% of board chairs and 50% of board members were women. Inequalities were most evident in the representation of individuals from low- and middle-income countries on governing bodies. Only 4.5% of board members were nationals of low-income countries, while high-income country nationals held 68% of board seats. There was a lack of representation from Small Island Developing States and the 10 countries most affected by extreme weather events.
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