Relevant bibliographies by topics / Planets

Academic literature on the topic 'Planets'

Author: Grafiati
Published: 4 June 2021
Last updated: 29 July 2024

Create a spot-on reference in APA, MLA, Chicago, Harvard, and other styles

Select a source type:

Contents

Consult the lists of relevant articles, books, theses, conference reports, and other scholarly sources on the topic 'Planets.'

Next to every source in the list of references, there is an 'Add to bibliography' button. Press on it, and we will generate automatically the bibliographic reference to the chosen work in the citation style you need: APA, MLA, Harvard, Chicago, Vancouver, etc.

You can also download the full text of the academic publication as pdf and read online its abstract whenever available in the metadata.

Journal articles on the topic "Planets"

1

Kokaia, Giorgi, Melvyn B. Davies, and Alexander J. Mustill. "Effects of capturing a wide-orbit planet on planetary systems: system stability and habitable zone bombardment rates." Monthly Notices of the Royal Astronomical Society 511, no. 2 (December 31, 2021): 1685–93. http://dx.doi.org/10.1093/mnras/stab3659.

Full text
Abstract:
ABSTRACT A large fraction of stars are formed in dense clusters. In the cluster, close encounters between stars at distances less than 100 au are common. It has been shown that during close encounters planets can transfer between stars. Such captured planets will be on different orbits compared to planets formed in the system, often on very wide, eccentric, and inclined orbits. We examine how these captured planets affect Kuiper belt-like planetesimal belts in their new systems by examining the effects on habitable planets in systems containing an outer gas giant. We show that these captured planets can destabilize the belt, and we show that the fraction of the planetesimals that make it past the giant planets into the system to impact the habitable planet is independent of the captured planet’s orbital plane, whereas the fraction of the planetesimals that are removed and the rate at which they are removed depend strongly on the captured planet’s pericentre and inclination. We then examine a wide range of outcomes of planet capture and find that when a Jupiter-mass planet is captured it will in 40 per cent of cases destabilize the giant planets in the system and in 40 per cent of cases deplete the belt in a few Myr, i.e. not posing much risk to life on terrestrial planets that would be expected to develop later. In the final 20 per cent of cases, the result will be a flux of impactors 10–20 times greater than that on Earth that can persist for several Gyr, detrimental to the development of life on the planet.
APA, Harvard, Vancouver, ISO, and other styles
2

Barr, Amy C., Vera Dobos, and László L. Kiss. "Interior structures and tidal heating in the TRAPPIST-1 planets." Astronomy & Astrophysics 613 (May 2018): A37. http://dx.doi.org/10.1051/0004-6361/201731992.

Full text
Abstract:
Context. With seven planets, the TRAPPIST-1 system has among the largest number of exoplanets discovered in a single system so far. The system is of astrobiological interest, because three of its planets orbit in the habitable zone of the ultracool M dwarf. Aims. We aim to determine interior structures for each planet and estimate the temperatures of their rock mantles due to a balance between tidal heating and convective heat transport to assess their habitability. We also aim to determine the precision in mass and radius necessary to determine the planets’ compositions. Methods. Assuming the planets are composed of uniform-density noncompressible materials (iron, rock, H2O), we determine possible compositional models and interior structures for each planet. We also construct a tidal heat generation model using a single uniform viscosity and rigidity based on each planet’s composition. Results. The compositions for planets b, c, d, and e remain uncertain given the error bars on mass and radius. With the exception of TRAPPIST-1c, all have densities low enough to indicate the presence of significant H2O. Planets b and c experience enough heating from planetary tides to maintain magma oceans in their rock mantles; planet c may have surface eruptions of silicate magma, potentially detectable with next-generation instrumentation. Tidal heat fluxes on planets d, e, and f are twenty times higher than Earth’s mean heat flow. Conclusions. Planets d and e are the most likely to be habitable. Planet d avoids the runaway greenhouse state if its albedo is ≳0.3. Determining the planet’s masses within ~0.1–0.5 Earth masses would confirm or rule out the presence of H2O and/or iron. Understanding the geodynamics of ice-rich planets f, g, and h requires more sophisticated modeling that can self-consistently balance heat production and transport in both rock and ice layers.
APA, Harvard, Vancouver, ISO, and other styles
3

Jackson, Brian, Rory Barne, and Richard Greenberg. "Planetary Transits and Tidal Evolution." Proceedings of the International Astronomical Union 4, S253 (May 2008): 217–29. http://dx.doi.org/10.1017/s1743921308026434.

Full text
Abstract:
AbstractTransiting planets are generally close enough to their host stars that tides may govern their orbital and thermal evolution. We present calculations of the tidal evolution of recently discovered transiting planets and discuss their implications. The tidal heating that accompanies this orbital evolution can be so great that it controls the planet's physical properties and may explain the large radii observed in several cases, including, for example, TrES-4. Also, since a planet's transit probability depends on its orbit, it evolves due to tides. Current values depend sensitively on the physical properties of the star and planet, as well as on the system's age. As a result, tidal effects may introduce observational biases in transit surveys, which may already be evident in current observations. Transiting planets tend to be younger than non-transiting planets, an indication that tidal evolution may have destroyed many close-in planets. Also the distribution of the masses of transiting planets may constrain the orbital inclinations of non-transiting planets.
APA, Harvard, Vancouver, ISO, and other styles
4

Franchini, Alessia, Rebecca G. Martin, and Stephen H. Lubow. "Multiplanet disc interactions in binary systems." Monthly Notices of the Royal Astronomical Society 491, no. 4 (November 22, 2019): 5351–60. http://dx.doi.org/10.1093/mnras/stz3175.

Full text
Abstract:
ABSTRACT We investigate the evolution of a multiplanet–disc system orbiting one component of a binary star system. The planet–disc system is initially coplanar but misaligned to the binary orbital plane. The planets are assumed to be giants that open gaps in the disc. We first study the role of the disc in shaping the mutual evolution of the two planets using a secular model for low initial tilt. In general, we find that the planets and the disc do not remain coplanar, in agreement with previous work on the single planet case. Instead, the planets and the disc undergo tilt oscillations. A high-mass disc between the two planets causes the planets and the disc to nodally precess at the same average rate but they are generally misaligned. The amplitude of the tilt oscillations between the planets is larger while the disc is present. We then consider higher initial tilts using hydrodynamical simulations and explore the possibility of the formation of eccentric Kozai–Lidov (KL) planets. We find that the inner planet’s orbit undergoes eccentricity growth for a large range of disc masses and initial misalignments. For a low disc mass and large initial misalignment, both planets and the disc can undergo KL oscillations. Furthermore, we find that sufficiently massive discs can cause the inner planet to increase its inclination beyond 90° and therefore to orbit the binary in a retrograde fashion. The results have important implications for the explanation of very eccentric planets and retrograde planets observed in multiplanet systems.
APA, Harvard, Vancouver, ISO, and other styles
5

Schaefer, Laura K., and Vivien Parmentier. "The Air Over There: Exploring Exoplanet Atmospheres." Elements 17, no. 4 (August 1, 2021): 257–63. http://dx.doi.org/10.2138/gselements.17.4.257.

Full text
Abstract:
The atmospheric composition for a rocky exoplanet will depend strongly on the planet’s bulk composition and orbital position. Nontraditional gases may be present in the atmospheres of exceptionally hot planets. Atmospheres of more clement planets will depend on the abundance of volatiles acquired during planet formation and atmospheric removal processes, including escape, condensation, and reaction with the surface. To date, observations of exoplanet atmospheres have focused on giant planets, but future space-and ground-based observatories will revolutionize the precision and spectral resolution with which we can probe an exoplanet’s atmosphere. This article consolidates lessons learned from the study of giant planet atmospheres, and points to the observations and challenges on the horizon for terrestrial planets.
APA, Harvard, Vancouver, ISO, and other styles
6

Garrido-Deutelmoser, Juan, Cristobal Petrovich, Leonardo Krapp, Kaitlin M. Kratter, and Ruobing Dong. "Substructures in Protoplanetary Disks Imprinted by Compact Planetary Systems." Astrophysical Journal 932, no. 1 (June 1, 2022): 41. http://dx.doi.org/10.3847/1538-4357/ac6bfd.

Full text
Abstract:
Abstract The substructures observed in protoplanetary disks may be the signposts of embedded planets carving gaps or creating vortices. The inferred masses of these planets often fall in the Jovian regime despite their low abundance compared to lower-mass planets, partly because previous works often assume that a single substructure (a gap or vortex) is caused by a single planet. In this work, we study the possible imprints of compact systems composed of Neptune-like planets (∼10–30 M ⊕) and show that long-standing vortices are a prevalent outcome when their interplanetary separation (Δa) falls below ∼8 times H p—the average disk’s scale height at the planet’s locations. In simulations where a single planet is unable to produce long-lived vortices, two-planet systems can preserve them for at least 5000 orbits in two regimes: (i) fully shared density gaps with elongated vortices around the stable Lagrange points L 4 and L 5 for the most compact planet pairs (Δa ≲ 4.6 H p), and (ii) partially shared gaps for more widely spaced planets (Δa ∼ 4.6–8 H p) forming vortices in a density ring between the planets through the Rossby wave instability. The latter case can produce vortices with a wide range of aspect ratios down to ∼3 and can occur for planets captured into the 3:2 (2:1) mean-motion resonances for disks’ aspects ratios of h ≳ 0.033 (h ≳ 0.057). We suggest that their long lifetimes are sustained by the interaction of spiral density waves launched by the neighboring planets. Overall, our results show that the distinguishing imprint of compact systems with Neptune-mass planets are long-lived vortices inside the density gaps, which in turn are shallower than single-planet gaps for a fixed gap width.
APA, Harvard, Vancouver, ISO, and other styles
7

Kozhanov, T. S., and Nizyarov N. "Mathematical Theory of Motion of Revolving Axes on the Surface of Planets." International Astronomical Union Colloquium 178 (2000): 619–22. http://dx.doi.org/10.1017/s0252921100061790.

Full text
Abstract:
Let a planet perform translational and rotational motions in the field of solar attraction. Let’s assume that the observer on the surface of the planet, knows (even approximately) an orbit and variations of orientation. It is necessary to clarify the motion of the instanteous rotation axis on the planet’s surface from the observer’s point of view on the planet’s surface.1. The coordinate system, to describe the translational and rotational motions of planets around the Sun we shall take into account the properties of orbits of solar system planets, namely: 1)All planets move in the same direction as the Sun revolves.2)At the present time, from June until December the Earth’s inhabitants see the north pole of the Sun and during the second half of year the southern one (Beleckei 1975, Menzel 1959).
APA, Harvard, Vancouver, ISO, and other styles
8

Li, Gongjie. "Tilting Planets during Planet Scattering." Astrophysical Journal Letters 915, no. 1 (June 25, 2021): L2. http://dx.doi.org/10.3847/2041-8213/ac0620.

Full text
APA, Harvard, Vancouver, ISO, and other styles
9

Fang, Julia, and Jean-Luc Margot. "PREDICTING PLANETS INKEPLERMULTI-PLANET SYSTEMS." Astrophysical Journal 751, no. 1 (April 30, 2012): 23. http://dx.doi.org/10.1088/0004-637x/751/1/23.

Full text
APA, Harvard, Vancouver, ISO, and other styles
10

Rauer, Heike, and Artie Hatzes. "Extrasolar planets and planet formation." Planetary and Space Science 55, no. 5 (April 2007): 535. http://dx.doi.org/10.1016/j.pss.2006.09.001.

Full text
APA, Harvard, Vancouver, ISO, and other styles
More sources

Dissertations / Theses on the topic "Planets"

1

Brickman, Jacklyn E. "Experiments in Biological Planet Formation and Plants: Nourishing Bodies, Nourishing Planets." The Ohio State University, 2020. http://rave.ohiolink.edu/etdc/view?acc_num=osu1595340630648528.

Full text
APA, Harvard, Vancouver, ISO, and other styles
2

Trotta, Leonardo Di Schiavi. "Modelo dinâmico 3-D para a evolução do sistema Plutão-Caronte /." Rio Claro, 2017. http://hdl.handle.net/11449/150604.

Full text
Abstract:
Orientador: Tadashi Yokoyama
Banca: Nelson Callegari Junior
Banca: Rodney da Silva Gomes
Resumo: O sistema Plutão-Caronte é um par quase binário em estado de duplo sincronismo. Hoje sabe-se que Plutão possui cinco satélites: Caronte, Styx, Nix, Kerberos e Hydra, onde os últimos quatro são muito menores que Caronte. A origem mais plausível para o sistema Plutão-Caronte é a de um impacto de grandes proporções entre corpos de tamanhos similares, onde o impactador (que viria a ser Caronte) permanece quase intacto após o evento. Caronte iniciaria o movimento orbital próximo de Plutão (ex: a≈4 Rp) com ambos rotacionando rapidamente, como consequência da colisão mútua. Devido a intensa maré, suas distâncias irão evoluir e seus equadores (provavelmente desalinhados devido ao choque) irão também evoluir em consonância com seus respectivos spins. Alguns autores, por meio de um modelo bidimensional, tomando a maré modelada por Mignard (1980) e Peale (2007), usando dois métodos distintos, evoluíram Plutão-Caronte à partir deste cenário, reproduzindo os parâmetros orbitais e rotacionais atuais do sistema. Neste trabalho fazemos um estudo tridimensional, usando na parte rotacional as variáveis canônicas de Andoyer. Nesta abordagem, integramos a atitude de Plutão e Caronte por meio das equações de Hamilton, enquanto que a dinâmica translacional é feita classicamente via equações cartesianas de Newton. As contribuições dos torques, devidas às interações por efeito de maré entre Plutão e Caronte são inseridas nas equações de Hamilton. Como resultado mostramos o alinhamento dos equadores ... (Resumo completo, clicar acesso eletrônico abaixo)
Abstract: The Pluto-Charon system is almost a binary system in dual synchronous state. It is well known that Pluto has five satellites: Charon, Styx, Nix, Kerberos and Hydra, where the latter four are much smaller than Charon. The most plausible origin for the Pluto-Charon system is an oblique impact of great proportions between bodies with similar sizes. In this scenario, the impactor, which would later originate Charon, would remain almost intact after the collision. Initially the satellite would be revolving very close to Pluto (ex: a≈4Rp), with both bodies rotating very fast, as consequence of the mutual collision. The strong tidal effects, due to the initial approximation of both bodies combined with the fast rotation, expanded Charon's orbit, so as their equators aligned (probably misaligned due to the collision), in consonance with their respective spins. Some authors, using a two dimensional system and tidal forces modeled by Mignard (1980) and Peale (2007), with two distinct methods, evolved PlutoCharon from this scenario. They were able to reproduce the current orbital and rotational parameters of the system. In our work, a three-dimensional study was done, using the Andoyer's variable for the rotational problem. We integrated Pluto and Charon's atitude through Hamilton's equation, while the translational dynamics is calculated classically through Newton's cartesian equations. Torque's contributions due to tides raised on both Pluto and Charon are introduced in Hamilton's equ... (Complete abstract click electronic access below)
Mestre
APA, Harvard, Vancouver, ISO, and other styles
3

Joos, Franco. "Polarimetry of gas planets /." Zürich : ETH, 2007. http://e-collection.ethbib.ethz.ch/show?type=diss&nr=17051.

Full text
APA, Harvard, Vancouver, ISO, and other styles
4

Turner, Jake D., Robin M. Leiter, Lauren I. Biddle, Kyle A. Pearson, Kevin K. Hardegree-Ullman, Robert M. Thompson, Johanna K. Teske, et al. "Investigating the physical properties of transiting hot Jupiters with the 1.5-m Kuiper Telescope." OXFORD UNIV PRESS, 2017. http://hdl.handle.net/10150/626279.

Full text
Abstract:
We present new photometric data of 11 hot Jupiter transiting exoplanets (CoRoT-12b, HATP-5b, HAT-P-12b, HAT-P-33b, HAT-P-37b, WASP-2b, WASP-24b, WASP-60b, WASP-80b, WASP-103b and XO-3b) in order to update their planetary parameters and to constrain information about their atmospheres. These observations of CoRoT-12b, HAT-P-37b and WASP-60b are the first follow-up data since their discovery. Additionally, the first near-UV transits of WASP-80b and WASP-103b are presented. We compare the results of our analysis with previous work to search for transit timing variations (TTVs) and a wavelength dependence in the transit depth. TTVs may be evidence of a third body in the system, and variations in planetary radius with wavelength can help constrain the properties of the exoplanet's atmosphere. For WASP-103b and XO-3b, we find a possible variation in the transit depths which may be evidence of scattering in their atmospheres. The B-band transit depth of HAT-P-37b is found to be smaller than its near-IR transit depth and such a variation may indicate TiO/VO absorption. These variations are detected from 2-4.6s, so follow-up observations are needed to confirm these results. Additionally, a flat spectrum across optical wavelengths is found for five of the planets (HAT-P-5b, HAT-P-12b, WASP-2b, WASP-24b and WASP-80b), suggestive that clouds may be present in their atmospheres. We calculate a refined orbital period and ephemeris for all the targets, which will help with future observations. No TTVs are seen in our analysis with the exception of WASP-80b and follow-up observations are needed to confirm this possible detection.
APA, Harvard, Vancouver, ISO, and other styles
5

Ortiz, Álvarez Mauricio [Verfasser], and Andreas [Akademischer Betreuer] Quirrenbach. "Planets around giant stars: Two close-in transiting planets and one S-type planet in an eccentric binary system / Mauricio Ortiz Álvarez ; Betreuer: Andreas Quirrenbach." Heidelberg : Universitätsbibliothek Heidelberg, 2017. http://d-nb.info/118073890X/34.

Full text
APA, Harvard, Vancouver, ISO, and other styles
6

Lines, Stefan Matthew. "The formation of circumbinary planets." Thesis, University of Bristol, 2016. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.702118.

Full text
Abstract:
The discovery of nearly two thousand extrasolar planets over the last two decades is indicative that planets form everywhere. Exoplanet detections have been made of a plethora of planetary types and sizes across a wide range of orbital characteristics. One of the more exotic locations that planets have been discovered in is around stellar binaries. Their proximity to such a large time-dependent potential from the orbital motion of the stars can be problematic for their formation and long-term stability. Circumbinary planets, with orbits that fully encompass the binary, have been found to orbit as close as 0.3 au to the binary barycenter and are thus subject to strong gravitational perturbations. In the formation stage, the circumbinary protoplanetary disk experiences interactions with the binary which significantly alters the dynamics and hence collisional evolution of planetesimals which struggle to grow into the planets we see. To answer the question: Could observed circumbinary planets have formed in-situ? we perform a combination of N-body, hydro dynamical and subsequently hybrid simulations to investigate the feasibility of planet growth under these conditions. Our initial N-body simulations are performed in association with an advanced collision model to identify locations in the disk where planetesimals can accrete. We perform hydro dynamical simulations of circumbinary gas disks to investigate the structure and evolution of a fluid in response to a binary, across a wide range of fluid parameters. The resulting data, a quasi-steady-state surface density profile, is integrated in a semi-analytical way to account for gas feedback on planetesimals. Our work suggests that the majority of observed closely-orbiting circumbinary planets could not form in-situ due to an overwhelming number of erosive collisions caused by high impact velocities originating from the planetesimals' dynamical interaction with the binary and gas gravity. Planetary embryos must have formed further out in the disk, where velocities are lower, and this result indicates that migration is a necessary component of planetary evolution in these systems.
APA, Harvard, Vancouver, ISO, and other styles
7

Janes, Daniel Mark. "Tectonics of one-plate planets." Diss., The University of Arizona, 1990. http://hdl.handle.net/10150/185087.

Full text
Abstract:
The Voyager 2 encounter with Neptune and its moons in August of 1989 completed the discovery phase of planetary exploration. In the 25 years since Mariner 4 returned the first images of another planet, geophysical models for such basic processes as mantle convection and loading which were developed for the Earth have been strained beyond their limits by features such as the Tharsis rise on Mars and the coronae of Miranda which cover as much as a quarter of their planetary circumference. In this work I develop a general planetary shell model in spherical coordinates that is capable of treating shells of arbitrary thickness and driving forces of arbitrary breadth. I then present a methodology for finding the forces exerted on the shell from two processes. I first develop a treatment for mantle convection driven by a density anomaly within a viscous mantle. This model is applied to the small moon of Uranus, Miranda, to study the three large coronae which dominate its surface and for which several competing hypotheses were offered, two of which invoked mantle convection driven by density anomalies of opposite sign. I then develop a general model for loading of the lithosphere and examine the effects of a range of load breadths and lithosphere thicknesses. I map out the combinations of these two variables where classical approximations such as the flat-plate and thin-shell models are applicable as well as determine the nature and extent of the transition between these two regimes. Finally, I employ finite element modeling to investigate the coronae on Venus, showing that morphological aspects of these features reported in the literature can be produced by flexure of the lithosphere beneath a volcanic load and gravitational sliding of a cooled crust off these volcanic mounds. I then, however, produce independent characteristic topographic profiles for three of the more regular coronae which question how typical the reported morphologies are in the coronae in general.
APA, Harvard, Vancouver, ISO, and other styles
8

Fortney, Jonathan J. "The evolution of giant planets." Diss., The University of Arizona, 2004. http://hdl.handle.net/10150/290002.

Full text
Abstract:
As a whole this dissertation aims to understand giant planets as an entire class of astronomical objects. Initially we investigate the mechanics and evolutionary effects of phase separation in the deep interiors of giant planets. We present the first models of Saturn and Jupiter to couple their evolution to both a radiative-atmosphere grid and to high-pressure phase diagrams of hydrogen with helium and other admixtures. We find that previously calculated hydrogen-helium phase diagrams in which Saturn's interior reaches a region of predicted helium immiscibility do not allow enough energy release to prolong Saturn's cooling to its known age and effective temperature. We explore modifications to published phase diagrams that would lead to greater energy release. Alternatively, we also explore the evolutionary effects of the phase separation of an icy component. We then expand our inhomogeneous evolutionary models to the evolution of hypothetical extrasolar giant planets (EGPs) in the 0.15 to 3.0 Jupiter mass range, incorporating helium phase separation using the hydrogen-helium phase diagram we have calibrated to Jupiter and Saturn. We show how phase separation increases the luminosity, effective temperature, and radii, and decreases the atmospheric helium mass fraction, for various giant planets as a function of age. We also show the effects of irradiation and dense cores. Next we turn to the atmosphere of the transiting EGP, HD209458b. Using a self-consistent atmosphere code, we construct a new model of the planet's atmosphere to investigate the disparity between the observed strength of the sodium absorption feature at 589 nm and the predictions of previous models. For the atmospheric temperature-pressure profile we derive, silicate and iron clouds reside at a pressure of several mbar in the planet's atmosphere. These clouds lead to increased absorption in bands directly adjacent to the sodium line core. Using a non-LTE sodium ionization model, we show that ionization leads to a slight weakening of the sodium feature. The sensitivity of our conclusions to the derived atmospheric temperature-pressure profile is discussed. We show how our investigation leads to a better understanding of how the planetary radius measurements should be compared to model radii.
APA, Harvard, Vancouver, ISO, and other styles
9

Zaranek, Sarah Ellen. "Roles of convection in the evolution of planetary interiors and terrestrial lithospheres /." View online version; access limited to Brown University users, 2005. http://wwwlib.umi.com/dissertations/fullcit/3174708.

Full text
APA, Harvard, Vancouver, ISO, and other styles
10

Steffen, Jason. "Detecting new planets in transiting systems /." Thesis, Connect to this title online; UW restricted, 2006. http://hdl.handle.net/1773/9686.

Full text
APA, Harvard, Vancouver, ISO, and other styles
More sources

Books on the topic "Planets"

1

Peters, Elisa. The planets =: Los planetas. New York: PowerKids Press, 2013.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
2

Inc, World Book, ed. Neptune and the distant dwarf planets. 2nd ed. Chicago: World Book, 2007.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
3

Oxlade, Chris. Planets. London: Wayland, 2012.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
4

Sorensen, Lynda. Planets. Vero Beach, Fla: Rourke Corp., 1993.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
5

Stone, Lynn M. Planets. Vero Beach, FL: Rourke Pub., 2009.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
6

Jo, Rudy Lisa, ed. Planets! New York, NY: HarperCollins, 2005.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
7

Kerrod, Robin. Planets. Edited by Forsey Chris and Ross Veronica. London: Belitha, 2001.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
8

Tory, Gordon-Harris, ed. Planets. New York: Scholastic, 2012.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
9

National Geographic Society (U.S.), ed. Planets. Washington, D.C: National Geographic, 2016.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
10

Guillain, Charlotte. Planets. Oxford: Heinemann Library, 2010.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
More sources

Book chapters on the topic "Planets"

1

Economou, Eleftherios N. "Planets." In From Quarks to the Universe, 223–32. Cham: Springer International Publishing, 2015. http://dx.doi.org/10.1007/978-3-319-20654-7_13.

Full text
APA, Harvard, Vancouver, ISO, and other styles
2

Hubbard, John H., and Beverly H. West. "Planets." In MacMath 9.2, 111–20. New York, NY: Springer New York, 1993. http://dx.doi.org/10.1007/978-1-4613-8378-9_17.

Full text
APA, Harvard, Vancouver, ISO, and other styles
3

Hubbard, John H., and Beverly H. West. "Planets." In MacMath 9.0, 111–20. New York, NY: Springer New York, 1992. http://dx.doi.org/10.1007/978-1-4684-0390-9_17.

Full text
APA, Harvard, Vancouver, ISO, and other styles
4

Hubbard, John H., and Beverly H. West. "Planets." In MacMath 9.2, 111–20. Berlin, Heidelberg: Springer Berlin Heidelberg, 1993. http://dx.doi.org/10.1007/978-3-662-25368-7_17.

Full text
APA, Harvard, Vancouver, ISO, and other styles
5

Economou, Eleftherios N. "Planets." In A Short Journey from Quarks to the Universe, 93–97. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-20089-2_11.

Full text
APA, Harvard, Vancouver, ISO, and other styles
6

Harwood-Smith, Jennifer. "Planets." In The Routledge Companion to Imaginary Worlds, 169–76. New York: Routledge, 2018.: Routledge, 2017. http://dx.doi.org/10.4324/9781315637525-21.

Full text
APA, Harvard, Vancouver, ISO, and other styles
7

Ossendrijver, Mathieu. "Planets." In Babylonian Mathematical Astronomy: Procedure Texts, 55–109. New York, NY: Springer New York, 2012. http://dx.doi.org/10.1007/978-1-4614-3782-6_3.

Full text
APA, Harvard, Vancouver, ISO, and other styles
8

Kunth, Daniel, and Elena Terlevich. "Planets." In StarWords, 95–119. Cham: Springer International Publishing, 2024. http://dx.doi.org/10.1007/978-3-031-49024-8_9.

Full text
APA, Harvard, Vancouver, ISO, and other styles
9

Canavan, Gerry. "Planets." In The Routledge Companion to Politics and Literature in English, 419–29. London: Routledge, 2023. http://dx.doi.org/10.4324/9781003038009-44.

Full text
APA, Harvard, Vancouver, ISO, and other styles
10

Hanslmeier, Arnold. "Water on Planets and Dwarf Planets." In Water in the Universe, 37–69. Dordrecht: Springer Netherlands, 2011. http://dx.doi.org/10.1007/978-90-481-9984-6_3.

Full text
APA, Harvard, Vancouver, ISO, and other styles

Conference papers on the topic "Planets"

1

Shao, Michael. "Search for terrestrial planets with SIM Planet Quest." In SPIE Astronomical Telescopes + Instrumentation, edited by John D. Monnier, Markus Schöller, and William C. Danchi. SPIE, 2006. http://dx.doi.org/10.1117/12.671898.

Full text
APA, Harvard, Vancouver, ISO, and other styles
2

Seager, Sara, E. B. Ford, and E. L. Turner. "Characterizing Earth-like planets with terrestrial planet finder." In Astronomical Telescopes and Instrumentation, edited by Alan M. Dressler. SPIE, 2002. http://dx.doi.org/10.1117/12.456559.

Full text
APA, Harvard, Vancouver, ISO, and other styles
3

Miyazaki, Aya, and Kiyoshi Tomimatsu. "Onomato planets." In the 3rd International Conference. New York, New York, USA: ACM Press, 2009. http://dx.doi.org/10.1145/1517664.1517726.

Full text
APA, Harvard, Vancouver, ISO, and other styles
4

Dryomova, G. N., V. V. Dryomov, and A. V. Tutukov. "Interstellar planets." In Всероссийская с международным участием научная конференция студентов и молодых ученых, посвященная памяти Полины Евгеньевны Захаровой «Астрономия и исследование космического пространства». Ural University Press, 2021. http://dx.doi.org/10.15826/b978-5-7996-3229-8.26.

Full text
Abstract:
The lecture is devoted to the study of the role of gravitational scattering in the evolution of planetary systems. This mechanism explains the origin of the Oort cloud and free asteroids, comets, and planets (ACPs) from the parent star.
APA, Harvard, Vancouver, ISO, and other styles
5

Marcy, Geoff W., and R. Paul Butler. "First three planets." In Photonics West '96, edited by Stuart A. Kingsley and Guillermo A. Lemarchand. SPIE, 1996. http://dx.doi.org/10.1117/12.243440.

Full text
APA, Harvard, Vancouver, ISO, and other styles
6

Schmidt, Rainer, Andrew Lindley, Ross King, Andrew Jackson, Carl Wilson, and Fabian Steeg. "The Planets IF." In the 1st International Digital Preservation Interoperability Framework Symposium. New York, New York, USA: ACM Press, 2010. http://dx.doi.org/10.1145/2039263.2039273.

Full text
APA, Harvard, Vancouver, ISO, and other styles
7

Özgen, D. S., Y. Afacan, and E. Surer. "Save the Planets." In GoodTechs '20: 6th EAI International Conference on Smart Objects and Technologies for Social Good. New York, NY, USA: ACM, 2020. http://dx.doi.org/10.1145/3411170.3411253.

Full text
APA, Harvard, Vancouver, ISO, and other styles
8

Mazeh, Tsevi. "The Transiting Planets." In STELLAR ASTROPHYSICS WITH THE WORLD'S LARGEST TELESCOPES: First International Workshop on Stellar Astrophysics with the World's Largest Telescopes. AIP, 2005. http://dx.doi.org/10.1063/1.1893330.

Full text
APA, Harvard, Vancouver, ISO, and other styles
9

Kramer, Michael. "Planets around Pulsars." In PLANETARY SYSTEMS BEYOND THE MAIN SEQUENCE: Proceedings of the International Conference. AIP, 2011. http://dx.doi.org/10.1063/1.3556180.

Full text
APA, Harvard, Vancouver, ISO, and other styles
10

Kochte, M. "Imaging Terrestrial Planets." In THE SEARCH FOR OTHER WORLDS: Fourteenth Astrophysics Conference. AIP, 2004. http://dx.doi.org/10.1063/1.1774528.

Full text
APA, Harvard, Vancouver, ISO, and other styles

Reports on the topic "Planets"

1

Macintosh, B. Direct Imaging of Warm Extrasolar Planets. Office of Scientific and Technical Information (OSTI), April 2005. http://dx.doi.org/10.2172/15016011.

Full text
APA, Harvard, Vancouver, ISO, and other styles
2

Smullen, Rachel. Binaries, Planets, and Pluto, Oh my! Office of Scientific and Technical Information (OSTI), May 2021. http://dx.doi.org/10.2172/1783509.

Full text
APA, Harvard, Vancouver, ISO, and other styles
3

Hazi, A. Planets and Stars under the Magnifying Glass. Office of Scientific and Technical Information (OSTI), February 2007. http://dx.doi.org/10.2172/907853.

Full text
APA, Harvard, Vancouver, ISO, and other styles
4

Hills, J. G., M. P. Goda, and J. C. Solem. Close Encounters of Asteroids and Comets to Planets. Office of Scientific and Technical Information (OSTI), July 1999. http://dx.doi.org/10.2172/759193.

Full text
APA, Harvard, Vancouver, ISO, and other styles
5

Smullen, Rachel, and Soumi De. Black Holes, Crashing Galaxies, and Strange New Planets. Office of Scientific and Technical Information (OSTI), June 2021. http://dx.doi.org/10.2172/1787271.

Full text
APA, Harvard, Vancouver, ISO, and other styles
6

Celliers, P., J. Eggert, G. Collins, S. Brygoo, R. Jeanloz, R. McWilliams, P. Loubeyre, T. Boehly, and J. Miller. Creating the Core Conditions of Extra-solar and Solar Giant Planets. Office of Scientific and Technical Information (OSTI), February 2007. http://dx.doi.org/10.2172/902290.

Full text
APA, Harvard, Vancouver, ISO, and other styles
7

Ullom, J., M. Cunningham, B. Macintosh, T. Miyazaki, and S. Labov. ''High-Speed, Photon-Counting Camera for the Detection of Extrasolar Planets''. Office of Scientific and Technical Information (OSTI), February 2003. http://dx.doi.org/10.2172/15003349.

Full text
APA, Harvard, Vancouver, ISO, and other styles
8

Dutta, Sumit. Identifying Minor Planets in UCAC Data and Deriving Accurate O-C. Fort Belvoir, VA: Defense Technical Information Center, September 2006. http://dx.doi.org/10.21236/ada455924.

Full text
APA, Harvard, Vancouver, ISO, and other styles
9

Duckss, Weitter. Why do Hydrogen and Helium Migrate from Some Planets and Smaller Objects? Intellectual Archive, March 2019. http://dx.doi.org/10.32370/iaj.2055.

Full text
APA, Harvard, Vancouver, ISO, and other styles
10

Smullen, Rachel. We are made of star stuff: How stars (and planets) are created. Office of Scientific and Technical Information (OSTI), November 2021. http://dx.doi.org/10.2172/1833240.

Full text
APA, Harvard, Vancouver, ISO, and other styles
You might also be interested in the extended bibliographies on the topic 'Planets' for particular source types:
Journal articles Dissertations / Theses Books
We offer discounts on all premium plans for authors whose works are included in thematic literature selections. Contact us to get a unique promo code!

To the bibliography