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Journal articles on the topic 'Planetary bodies'

Author: Grafiati

Published: 8 June 2024

Last updated: 31 July 2025

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1

Hu, H., and 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 (May 29, 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 m

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2

Kadish, Jon, J. R. Barber, P. D. Washabaugh, and D. J. Scheeres. "Stresses in accreted planetary bodies." International Journal of Solids and Structures 45, no. 2 (2008): 540–50. http://dx.doi.org/10.1016/j.ijsolstr.2007.08.008.

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3

Connolly, William E. "Bodies, Microbes and the Planetary." Theory & Event 21, no. 4 (2018): 962–67. http://dx.doi.org/10.1353/tae.2018.0058.

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4

Cockell, Charles S., and Gerda Horneck. "Planetary parks—formulating a wilderness policy for planetary bodies." Space Policy 22, no. 4 (2006): 256–61. http://dx.doi.org/10.1016/j.spacepol.2006.08.006.

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5

Kotliarov, I. D. "Classification of celestial bodies within planetary systems." Moscow University Physics Bulletin 63, no. 6 (2008): 416–19. http://dx.doi.org/10.3103/s0027134908060118.

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6

Melosh, H. J. "Ejection of rock fragments from planetary bodies." Geology 13, no. 2 (1985): 144. http://dx.doi.org/10.1130/0091-7613(1985)13<144:eorffp>2.0.co;2.

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7

Lin, Yucong, Melissa Bunte, Srikanth Saripalli, James Bell, and 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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8

Binzel, Richard P. "Small bodies looming large in planetary science." Nature Astronomy 3, no. 4 (2019): 282–83. http://dx.doi.org/10.1038/s41550-019-0747-6.

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9

Skripka, V. L., and L. H. Minyazeva. "Planetary rock-breaking bodies and horizontal drilling." Proceedings of higher educational establishments. Geology and Exploration, no. 5 (February 5, 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

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10

Visser, R. G., C. W. Ormel, C. Dominik, and S. Ida. "Spinning up planetary bodies by pebble accretion." Icarus 335 (January 2020): 113380. http://dx.doi.org/10.1016/j.icarus.2019.07.014.

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11

Minglibayev, M. Zh, and A. B. Kosherbayeva. "EQUATIONS OF PLANETARY SYSTEMS MOTION." SERIES PHYSICO-MATHEMATICAL 6, no. 334 (2020): 53–60. http://dx.doi.org/10.32014/2020.2518-1726.97.

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The study of the dynamically evolution of planetary systems is very actually in relation with findings of exoplanet systems. free spherical bodies problem is considered in this paper, mutually gravitating according to Newton's law, with isotropically variable masses as a celestial-mechanical model of non-stationary exoplanetary systems. The dynamic evolution of planetary systems is learned, when evolution's leading factor is the masses' variability of gravitating bodies themselves. The laws of the bodies' masses varying are assumed to be known arbitrary functions of time. When doing so the rat

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12

ten Kate, I. L., and M. Reuver. "PALLAS: Planetary Analogues Laboratory for Light, Atmosphere, and Surface Simulations." Netherlands Journal of Geosciences - Geologie en Mijnbouw 95, no. 2 (2015): 183–89. http://dx.doi.org/10.1017/njg.2015.19.

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AbstractHumankind has been interested in space throughout the ages and studies of the universe and our own solar system have been ongoing since the first observations of celestial bodies. In the current era space exploration has provided in situ data for the different bodies in our solar system. To fully comprehend the underlying processes occurring in these bodies, missions and telescope observations are, however, not sufficient and additional modelling studies, both numerical and analogue, are necessary. In this paper we present a new facility specifically designed to experimentally study or

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13

Wang, Y., R. B. Dong, D. N. C. Lin, and X. W. Liu. "Origin of debris disks and the supply of metals in DZ white dwarfs." Proceedings of the International Astronomical Union 3, S249 (2007): 389–92. http://dx.doi.org/10.1017/s1743921308016876.

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AbstractWe discuss the dynamical evolution of minor planetary bodies in the outer regions of planetary systems around the progenitors of DZ white dwarfs. We show that during the planetary-nebula phase of these stars, mass loss can lead to the expansion of all planetary bodies. The orbital eccentricity of the minor bodies, as relics of planetesimals, may be largely excited by the perturbation due to both gas drag effects and nearby gas giant planets. Some of these bodies migrate toward the host star, while others are scattered out of the planetary system. The former have modest probability of b

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14

Rietmeijer, Frans J. M. "A model for diagenesis in proto-planetary bodies." Nature 313, no. 6000 (1985): 293–94. http://dx.doi.org/10.1038/313293a0.

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15

Haghighipour, Nader. "Super-Earths: a new class of planetary bodies." Contemporary Physics 52, no. 5 (2011): 403–38. http://dx.doi.org/10.1080/00107514.2011.598370.

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16

Ibadov, Subhon, and Firuz S. Ibodov. "Explosive evolution of small bodies in planetary atmospheres." Proceedings of the International Astronomical Union 9, S310 (2014): 162–63. http://dx.doi.org/10.1017/s1743921314008126.

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AbstractThe entry of small celestial bodies such as cometary nuclei, asteroids and their large fragments, into a planetary atmosphere is accompanied by an “explosion”, i.e., sudden rise in brightness and the generation of a “blast” shock wave, like the 2013 Chelyabinsk event. Fully analytic approach to the phenomenon is developed taking into account aerodynamic crushing of the body and transversal expansion of the crushed mass, that leads to impulse generation of hot plasma and a “blast” shock wave in the thin “exploding” layer.

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17

GIRISH, T. "Nighttime operation of photovoltaic systems in planetary bodies." Solar Energy Materials and Solar Cells 90, no. 6 (2006): 825–31. http://dx.doi.org/10.1016/j.solmat.2005.04.018.

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18

WETHERILL, G. W. "Occurrence of Earth-Like Bodies in Planetary Systems." Science 253, no. 5019 (1991): 535–38. http://dx.doi.org/10.1126/science.253.5019.535.

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19

Wang, X., J. Schwan, H. W. Hsu, E. Grün, and M. Horányi. "Dust charging and transport on airless planetary bodies." Geophysical Research Letters 43, no. 12 (2016): 6103–10. http://dx.doi.org/10.1002/2016gl069491.

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20

Matsuyama, Isamu, and Francis Nimmo. "Tectonic patterns on reoriented and despun planetary bodies." Icarus 195, no. 1 (2008): 459–73. http://dx.doi.org/10.1016/j.icarus.2007.12.003.

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21

Saurety, Adrien, Razvan Caracas, and Sean N. Raymond. "Impact-induced Vaporization during Accretion of Planetary Bodies." Astrophysical Journal Letters 981, no. 1 (2025): L13. https://doi.org/10.3847/2041-8213/adb30e.

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Abstract Giant impacts dominate the late stages of accretion of rocky planets. They contribute to the heating, melting, and sometimes vaporizing of the bodies involved in the impacts. Due to fractionation during melting and vaporization, planet-building impacts can significantly change the composition and geochemical signatures of rocky objects. Using first-principles molecular dynamics simulations, we analyze the shock behavior of complex realistic silicate systems, representative of both rocky bodies. We introduce a novel criterion for vapor formation that uses entropy calculations to determ

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22

Jewitt, David. "Nongravitational Forces in Planetary Systems." Planetary Science Journal 6, no. 1 (2025): 12. https://doi.org/10.3847/psj/ad9824.

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Abstract Nongravitational forces play surprising and, sometimes, centrally important roles in shaping the motions and properties of small planetary bodies. In the solar system, the morphologies of comets, the delivery of meteorites, and the shapes and dynamics of asteroids and binaries are all affected by nongravitational forces. In exoplanetary systems and debris disks, nongravitational forces affect the lifetimes of circumstellar particles and feed refractory debris to the photospheres of the central stars. Unlike the gravitational force, which is a simple function of the well-known separati

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23

Brigham, Jonee Kulman. "Integrated Bodies: Language, Art, and Infrastructure in Planetary Health Education." Creative Nursing 27, no. 4 (2021): 269–72. http://dx.doi.org/10.1891/cn-2021-0036.

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The Planetary Health Education Framework recognizes the interdependence of human health and the health of planetary ecosystems, and centers its guidance on the paradigm of human interconnection within nature. Through the author's scholarship and art, she addresses this “paradigm work” to heal the human-nature divide. This essay explores ideas for the role of language, art, and infrastructure in supporting Planetary Health Education using the example of Earth Systems Journey, which is both an art form and a curriculum model for experiential, art-led environmental education about human integrati

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24

Melita, M. D., and A. Brunini. "The evolution of the Kuiper belt during the formation of the outer planets." International Astronomical Union Colloquium 173 (1999): 37–44. http://dx.doi.org/10.1017/s0252921100031213.

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AbstractA self-consistent study of the formation of planetary bodies beyond the orbit of Saturn and the evolution of Kuiper disks is carried out by means of an N-body code where accretion and gravitational encounters are considered. This investigation is focused on the aggregation of massive bodies in the outer planetary region and on the consequences of such process in the corresponding cometary belt. We study the link between the bombardment of massive bodies and mass depletion and eccentricity excitation.

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25

Williams, Iwan P., Edward L. G. Bowell, Mikhail Ya Marov, et al. "DIVISION III: PLANETARY SYSTEM SCIENCES." Proceedings of the International Astronomical Union 3, T26B (2007): 111–17. http://dx.doi.org/10.1017/s1743921308023764.

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Division III gathers astronomers engaged in the study of a comprehensive range of phenomena in the solar system and its bodies, from the major planets via comets to meteorites and interplanetary dust.

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26

Bowell, Edward L. G., Karen J. Meech, Iwan P. Williams, et al. "DIVISION III: PLANETARY SYSTEMS SCIENCES." Proceedings of the International Astronomical Union 4, T27A (2008): 149–53. http://dx.doi.org/10.1017/s1743921308025398.

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27

Tichá, Jana, Brian G. Marsden, Daniel Green, et al. "DIVISION III / WG: COMMITTEE SMALL BODIES NOMENCLATURE." Proceedings of the International Astronomical Union 3, T26B (2007): 118–19. http://dx.doi.org/10.1017/s1743921308023776.

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28

Singh, Surendra V., Haritha Dilip, Jaya K. Meka, et al. "New Signatures of Bio-Molecular Complexity in the Hypervelocity Impact Ejecta of Icy Moon Analogues." Life 12, no. 4 (2022): 508. http://dx.doi.org/10.3390/life12040508.

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Impact delivery of prebiotic compounds to the early Earth from an impacting comet is considered to be one of the possible ways by which prebiotic molecules arrived on the Earth. Given the ubiquity of impact features observed on all planetary bodies, bolide impacts may be a common source of organics on other planetary bodies both in our own and other solar systems. Biomolecules such as amino acids have been detected on comets and are known to be synthesized due to impact-induced shock processing. Here we report the results of a set of hypervelocity impact experiments where we shocked icy mixtur

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29

Minglibayev, M. Zh, and A. B. Kosherbayeva. "DIFFERENTIAL EQUATIONS OF PLANETARY SYSTEMS." REPORTS 2, no. 330 (2020): 14–20. http://dx.doi.org/10.32014/10.32014/2020.2518-1483.26.

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In this article will be considered many spherical bodies problem with variable masses, varying non-isotropic at different rates as celestial-mechanical model of non-stationary planetary systems. In this article were obtained differential equations of motions of spherical bodies with variable masses to reach purpose exploration of evolution planetary systems. The scientific importance of the work is exploration to the effects of masses’ variability of the dynamic evolution of the planetary system for a long period of time. According to equation of Mescherskiy, we obtained differential equations

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30

Sarid, Gal, Sarah T. Stewart, and Zoë M. Leinhardt. "Erosive Hit-and-Run Impact Events: Debris Unbound." Proceedings of the International Astronomical Union 10, S318 (2015): 9–15. http://dx.doi.org/10.1017/s1743921315009679.

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AbstractErosive collisions among planetary embryos in the inner solar system can lead to multiple remnant bodies, varied in mass, composition and residual velocity. Some of the smaller, unbound debris may become available to seed the main asteroid belt. The makeup of these collisionally produced bodies is different from the canonical chondritic composition, in terms of rock/iron ratio and may contain further shock-processed material. Having some of the material in the asteroid belt owe its origin from collisions of larger planetary bodies may help in explaining some of the diversity and odditi

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31

Bischoff, Adolf, and Dieter Stöffler. "Shock metamorphism as a fundamental process in the evolution of planetary bodies: Information from meteorites." European Journal of Mineralogy 4, no. 4 (1992): 707–56. http://dx.doi.org/10.1127/ejm/4/4/0707.

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32

Yeo, Li Hsia, Xu Wang, Jan Deca, Hsiang-Wen Hsu, and Mihály Horányi. "Dynamics of electrostatically lofted dust on airless planetary bodies." Icarus 366 (September 2021): 114519. http://dx.doi.org/10.1016/j.icarus.2021.114519.

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33

Dumoulin, C., O. Čadek, and G. Choblet. "Predicting surface dynamic topographies of stagnant lid planetary bodies." Geophysical Journal International 195, no. 3 (2013): 1494–508. http://dx.doi.org/10.1093/gji/ggt363.

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34

Neto-Lima, J., M. Fernández-Sampedro, and O. Prieto-Ballesteros. "High Pressure Serpentinization Catalysed by Awaruite in Planetary Bodies." Journal of Physics: Conference Series 950 (October 2017): 042041. http://dx.doi.org/10.1088/1742-6596/950/4/042041.

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35

Vaitekhovich, P. E., D. V. Semenenko, and D. V. Yukhnevich. "Motion specifics of grinding bodies in vertical planetary mills." Chemical and Petroleum Engineering 45, no. 7-8 (2009): 395–401. http://dx.doi.org/10.1007/s10556-009-9199-7.

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36

Cole, G. H. A. "Concerning the occurrence of water in the planetary bodies." Surveys in Geophysics 8, no. 4 (1986): 439–57. http://dx.doi.org/10.1007/bf01903950.

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37

Englert, Peter A. J. "Planetary gamma ray spectrometry: remote sensing of elemental abundances." Proceedings in Radiochemistry 1, no. 1 (2011): 349–55. http://dx.doi.org/10.1524/rcpr.2011.0062.

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Abstract Planetary gamma ray spectrometry is a form of nuclear spectroscopy applied remotely to provide geochemical maps of planetary bodies. From early developments it has by now become a standard modality of planetary exploration. Basic and applied nuclear science has made significant contributions to the advancement of planetary gamma ray spectrometry, as outlined in this methodological and historical assessment.

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38

Ziglina, I. N., and O. Yu Schmidt. "Stochastic Behaviour of Planetary Orbits During the Accumulation Process." International Astronomical Union Colloquium 132 (1993): 137–48. http://dx.doi.org/10.1017/s025292110006601x.

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AbstractThe evolution of orbital elements of a growing planet during the accumulation process is considered. The planetary orbit undergoes perturbations because of random encounters and collisions with bodies of its accretion zone and also because of gravitational interaction with an already formed massive planet (“Jupiter”). The mass and velocity distributions of the swarm bodies are assumed to be given time-dependent functions. The Fokker-Planck equation describing the behaviour of the distribution function of orbital elements of the growing planet is worked out and solved. The present mean

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39

Bailey, Mark E. "Formation of Outer Solar System Bodies: Comets and Planetesimals." Symposium - International Astronomical Union 160 (1994): 443–59. http://dx.doi.org/10.1017/s0074180900046702.

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Observations of massive, extended discs around both pre-main-sequence and main-sequence stellar systems indicate that protoplanetary discs larger than the observed planetary system are a common phenomenon, while the existence of large comets suggests that the total cometary mass is much greater than previous estimates. Both observations suggest that theories of the origin of the solar system are best approached from the perspective provided by theories of star formation, in particular that the protoplanetary disc may have extended up to ~103 AU. A model with a surface density distribution simi

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40

Wilson, Alfred, Andrew Walker, Dario Alfè, and Chris Davies. "Solid-Liquid Interactions in Deep Planetary Interiors." Astronomy & Geophysics 65, no. 3 (2024): 3.18–3.22. http://dx.doi.org/10.1093/astrogeo/atae036.

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Abstract Alfred Wilson, Andrew Walker, Dario Alfè and Chris Davies report on a meeting bringing together experimental, theoretical, and observational studies of the deep mantles and cores of terrestrial bodies

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41

Richter, Robert, and Filip Maric. "Ecological Bodies and Relational Anatomies: Toward a Transversal Foundation for Planetary Health Education." Challenges 13, no. 2 (2022): 39. http://dx.doi.org/10.3390/challe13020039.

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As planetary health education enters medical and health professional training, transversal implementation across curricula is critical in developing its full potential and enabling future health professionals to meet the social, environmental, and health challenges of current and future generations in an integrated manner. To advance the transversal implementation of planetary health education, our study proceeded through: (1) a sequence analysis of documents framing physiotherapy education to identify relevant nexus points; (2) an explorative implementation of planetary health into foundation

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42

Beaugé, C., and S. J. Aarseth. "N-body simulations of planetary formation." Monthly Notices of the Royal Astronomical Society 245, no. 1 (1990): 30. http://dx.doi.org/10.1093/mnras/245.1.30.

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Summary We have performed numerical simulations of the last stage of terrestrial planetary formation using an N-body code similar to that of Lecar & Aarseth. An improved treatment of collisions has been applied, which allows fragmentation and cratering, as well as accretion. Initial models consist of 200 bodies of total mass 2.3 x 1028 g, distributed in a two-dimensional ring of size 1 au with initial circular orbits about the Sun. Planetary embryos begin to form by accretion in the early stages when the relative velocities are small. This growth is slowed down by the fragmentation process

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43

Gussie, Grant. "A Speculation into the Origin of Neutral Globules in Planetary Nebulae: Could the Helix’s Comets Really be Comets?" Publications of the Astronomical Society of Australia 12, no. 2 (1995): 170–73. http://dx.doi.org/10.1017/s1323358000020221.

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AbstractA novel explanation for the origin of the cometary globules within NGC 7293 (the ‘Helix’ planetary nebula) is examined, namely that these globules originate as massive cometary bodies at large astrocentric radii. The masses of such hypothetical cometary bodies would have to be several orders of magnitude larger than those of any such bodies observed in our solar system in order to supply the observed mass of neutral gas. It is, however, shown that comets at ‘outer Oort cloud’ distances are likely to survive past the red giant and asymptotic giant branch evolutionary phases of the centr

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44

Bergin, Edwin, Merel van’t Hoff, and Jes Jørgensen. "Searching For the t=0 of Planetary System Formation." EPJ Web of Conferences 265 (2022): 00043. http://dx.doi.org/10.1051/epjconf/202226500043.

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The composition of bodies in the solar system points to strong gradients in the volatile content within solid bodies hinting at the presence of gas-ice transitions across sublimation fronts in the young formative stages when the gas-rich disk was present. Terrestrial worlds are constructed out of the disk solids which are primarily silicate and water, but might also contain a significant fraction of organic material. These refractory organics are the source of carbon to Earth-like worlds, but have the potential to be destroyed if temperatures exceed 300-500 K (depending on pressure). These tem

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45

Mrozewski, Tomasz. "Planetary GIS and the USGS Astrogeology Science Center." Bulletin - Association of Canadian Map Libraries and Archives (ACMLA), no. 161 (April 1, 2019): 17–20. http://dx.doi.org/10.15353/acmla.n161.725.

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46

Sicardy, Bruno. "Small Bodies Around Other Stars." Symposium - International Astronomical Union 160 (1994): 429–42. http://dx.doi.org/10.1017/s0074180900046696.

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We briefly review recent advances in the observation and study of planetary bodies in extra-solar systems. We summarize in particular the main physical properties of the β-Pictoris dust disk, and the status of new disk observations. Theoretical implications of infalling discrete bodies are considered, in particular, the existence of possible perturbing planet(s) causing this influx. Such planets could spectacularly disturb circumstellar dust disks, thus revealing themselves in spite of their intrinsic faintness as mere point sources. Finally, we describe the recent possible discovery of at lea

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47

Doyle, Alexandra E., Edward D. Young, Beth Klein, Ben Zuckerman, and Hilke E. Schlichting. "Oxygen fugacities of extrasolar rocks: Evidence for an Earth-like geochemistry of exoplanets." Science 366, no. 6463 (2019): 356–59. http://dx.doi.org/10.1126/science.aax3901.

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Oxygen fugacity is a measure of rock oxidation that influences planetary structure and evolution. Most rocky bodies in the Solar System formed at oxygen fugacities approximately five orders of magnitude higher than a hydrogen-rich gas of solar composition. It is unclear whether this oxidation of rocks in the Solar System is typical among other planetary systems. We exploit the elemental abundances observed in six white dwarfs polluted by the accretion of rocky bodies to determine the fraction of oxidized iron in those extrasolar rocky bodies and therefore their oxygen fugacities. The results a

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48

Ji, Jianghui, L. Liu, and G. Y. Li. "On secular resonances of small bodies in the planetary systems." Proceedings of the International Astronomical Union 2, S236 (2006): 77–84. http://dx.doi.org/10.1017/s1743921307003092.

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AbstractWe investigate the secular resonances for massless small bodies and Earth-like planets in several planetary systems. We further compare the results with those of Solar System. For example, in the GJ 876 planetary system, we show that the secular resonances ν1 and ν2 (respectively, resulting from the inner and outer giant planets) can excite the eccentricities of the Earth-like planets with orbits 0.21≤ a <0.50 AU and eject them out of the system in a short timescale. However, in a dynamical sense, the potential zones for the existence of Earth-like planets are in the area 0.50≤ a ≤1

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49

Aliev, F. R., A. V. Lazurkevich, and I.-Kan An. "Planetary Gear on Basis of Diplane Meshing with Intermediate Bodies." Intellekt. Sist. Proizv. 15, no. 1 (2017): 4. http://dx.doi.org/10.22213/2410-9304-2017-1-4-8.

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Рассмотрена конструкция и предложена методика геометрического расчета и кинематического анализа одной из разновидностей планетарных передач с зацеплением промежуточных тел-шариков с улучшенными характеристиками [1]: высоким КПД за счет уменьшения потерь на трение, увеличенной нагрузочной способностью за счет многопарности зацепления, компактностью и т. д. Планетарная передача содержит два солнечных колеса, водило, сателлит и две группы промежуточных тел-шариков, контактирующихся с поверхностями зубьев, выполненных на обращенных друг к другу торцевых поверхностях солнечных колес и сателлита. Пр

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Yoshimitsu, Tetsuo, Takashi Kubota, and Ichiro Nakatani. "New Mobility System of Exploration Rover for Small Planetary Bodies." Journal of the Robotics Society of Japan 18, no. 2 (2000): 292–99. http://dx.doi.org/10.7210/jrsj.18.292.

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