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Relevant bibliographies by topics / Chaya Planets and Orbits

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Academic literature on the topic 'Chaya Planets and Orbits'

Author: Grafiati

Published: 5 June 2025

Last updated: 2 August 2025

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Journal articles on the topic "Chaya Planets and Orbits"

1

Dr., P. Thangavel Murugan. "IMPORTANCE OF ASCENDANT AND IT'S LORD TO BE STRENGTH." International Journal of Scientific Research and Modern Education (IJSRME) 7, no. 2 (2022): 8–12. https://doi.org/10.5281/zenodo.7489890.

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It is an astrological theory that man determines his life by the name of destiny. To define this, the planetary positions and combinations in Janana Jatakas/Natal Chart help us to some extent to confirm that. With characters of the planet, they are divided into two groups like Subar and Asubar. And further, within the nine planets there are benefic planets and malefic planets. Benefic and malefic are determined depending of its origin first, Athipatyam as they acquired is next and their placements in the Janana Jataka at the last. There are many times benefic planets doesn’t work with th

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Jones, B. W., and P. N. Sleep. "Terrestrial planet orbits in the habitable zones of exoplanetary system." Symposium - International Astronomical Union 202 (2004): 199–201. http://dx.doi.org/10.1017/s0074180900217841.

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We have investigated whether terrestrial planets can exist in orbits in known exoplanetary systems such that life could have emerged on those planets. We have shown that Rho CrB and 47 UMa could have terrestrial planets in orbits that remain confined to their habitable zones for biologically significant lengths of time. We have also shown that the Gliese 876 and Ups And systems are very unlikely to have such orbits.

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Naoz, Smadar. "Dynamical Effects of Stellar Companions." Proceedings of the International Astronomical Union 11, A29A (2015): 65–70. http://dx.doi.org/10.1017/s1743921316002416.

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AbstractThe fraction of stellar binaries in the field is extremely high (about 40% − 70% forM > 1M⊙ stars), and thus, given this frequency, a high fraction of all exoplanetary systems may reside in binaries. While close-in giant planets tend to be found preferentially in binary stellar systems it seems that the frequency of giant planets in close binaries (>100-1000 AU) is significantly lower than in the overall population. Stellar companions gravitational perturbations may significantly alter the planetary orbits around their partner on secular timescales. They can drive planets to larg

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Yang, Biao, Yu Jiang, Hengnian Li, et al. "Semi-Analytical Search for Sun-Synchronous and Planet Synchronous Orbits around Jupiter, Saturn, Uranus and Neptune." Mathematics 10, no. 15 (2022): 2684. http://dx.doi.org/10.3390/math10152684.

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With the development of aerospace science and technology, more and more probes are expected to be deployed around extraterrestrial planets. In this paper, some special orbits around Jupiter, Saturn, Uranus, and Neptune are discussed and analyzed. The design methods of some special orbits are sorted out, considering the actual motion parameters and main perturbation forces of these four planets. The characteristics of sun-synchronous orbits, repeating ground track orbits, and synchronous planet orbits surrounding these plants are analyzed and compared. The analysis results show that Uranus does

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Marzari, F., and M. Nagasawa. "Influence of general-relativity effects, dynamical tides, and collisions on planet–planet scattering close to the star." Astronomy & Astrophysics 625 (May 2019): A121. http://dx.doi.org/10.1051/0004-6361/201935065.

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Context. Planet–planet (P–P) scattering is an efficient and robust dynamical mechanism for producing eccentric exoplanets. Coupled to tidal interactions with the central star, this phenomenon can also explain close-in giant planets on circularized and potentially misaligned orbits. Aims. We explore scattering events occurring close to the star and test if they can reproduce the main features of the observed orbital distribution of giant exoplanets on tight orbits. Methods. In our modeling we exploited a numerical integration code based on the Hermite algorithm and including the effects of gene

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Li, Zixin. "Simulation of 3 Body Exo-Planetary System Orbits." Applied Physics Research 12, no. 2 (2020): 25. http://dx.doi.org/10.5539/apr.v12n2p25.

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To find out the general motion model of exo-planetary systems with one star and two planets, a computer program was used to carry out simulations and generate graphs showing the orbits of planets. When given the orbital periods and masses of the planets and stars, it is possible to predict the location of the planets over time and plot the shape of the orbit by considering the gravitational interactions between planets and the star, assuming that the planetary orbits are co-planar. I used the program to reproduce the result of transit timing variations (TTVs) of Kepler-46 system, I then invest

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Penzlin, Anna B. T., Sareh Ataiee, and Wilhelm Kley. "1:1 orbital resonance of circumbinary planets." Astronomy & Astrophysics 630 (September 23, 2019): L1. http://dx.doi.org/10.1051/0004-6361/201936478.

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The recent detection of the third planet in Kepler-47 has shown that binary stars can host several planets in circumbinary orbits. To understand the evolution of these systems we have performed two-dimensional hydrodynamic simulations of the circumbinary disc with two embedded planets for several Kepler systems. In two cases, Kepler-47 and -413, the planets are captured in a 1:1 mean-motion resonance at the planet “parking position” near the inner edge of the disc. The orbits are fully aligned and have mean eccentricities of about 0.25 to 0.30; the planets are entangled in a horseshoe-type mot

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Xie, Ji-Wei, Subo Dong, Zhaohuan Zhu, et al. "Exoplanet orbital eccentricities derived from LAMOST–Kepler analysis." Proceedings of the National Academy of Sciences 113, no. 41 (2016): 11431–35. http://dx.doi.org/10.1073/pnas.1604692113.

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The nearly circular (mean eccentricity e¯≈0.06) and coplanar (mean mutual inclination i¯≈3°) orbits of the solar system planets motivated Kant and Laplace to hypothesize that planets are formed in disks, which has developed into the widely accepted theory of planet formation. The first several hundred extrasolar planets (mostly Jovian) discovered using the radial velocity (RV) technique are commonly on eccentric orbits (e¯≈0.3). This raises a fundamental question: Are the solar system and its formation special? The Kepler mission has found thousands of transiting planets dominated by sub-Neptu

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Kondratyev, B. P., V. S. Kornoukhov, and E. V. Basova. "Modified method of round Gaussian rings. Application to the two-planetary problem." Vestnik Moskovskogo Universiteta, Seriya 3: Fizika, Astronomiya, no. 5_2023 (October 14, 2024): 2350801–1. http://dx.doi.org/10.55959/msu0579-9392.78.2350801.

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A scheme of the modified method of round Gaussian rings, designed to study the secular evolution of orbits in systems consisting of a central star and two planets, is presented. The reason for the secular evolution of the nodes and inclinations of the orbits of the planets is their mutual gravitational attraction. The orbits of the planets are modeled by homogeneous round Gaussian rings, to which the masses, sizes and angles of inclination of the orbits, as well as orbital angular momenta of the planets, are transferred. The method takes into account the fact that, in general, the ascending no

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Mogan, Saahit, and J. J. Zanazzi. "Concealing Circumbinary Planets with Tidal Shrinkage." Astrophysical Journal 988, no. 2 (2025): 150. https://doi.org/10.3847/1538-4357/ade2e8.

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Abstract Of the 14 transiting planets that have been detected orbiting eclipsing binaries (“circumbinary planets”), none have been detected with stellar binary orbital periods shorter than 7 days, despite such binaries existing in abundance. The eccentricity–period data for stellar binaries indicate that short-period (<7 days) binaries have had their orbits tidally circularized. We examine here to what extent tidal circularization and shrinkage can conceal circumbinary planets, i.e. whether planets actually exist around short-period binaries, but are not detected because their transit proba

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Dissertations / Theses on the topic "Chaya Planets and Orbits"

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Underwood, David R. "The stability of orbits of putative Earth-mass planets or satellites of giant planets within known exoplanetary systems." Thesis, Open University, 2006. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.437779.

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Mouret, Serge. "Investigations on the dynamics of minor planets with Gaia : Orbits, masses and fundamental physics." Observatoire de Paris (1667-....), 2007. https://hal.science/tel-02071419.

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La mission de l’agence spatiale européenne Gaia, dont le lancement est prévu en 2011, observera 350 000 astéroïdes avec une précision inégalée (au niveau du milli-arseconde). Le but de la thèse est l’investigation de la science que les données très précises de Gaia permettront de traiter et l’élaboration des méthodes de réduction notamment pour la détermination de masses des astéroïdes. Dans le premier chapitre, nous présentons la mission Gaia et une synthèse de la détermination de masses des astéroïdes jusqu’à nos jours. La seconde partie décrit la sélection des passages proches entre les ast

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Morrison, Sarah Jane, and Sarah Jane Morrison. "The Dynamics and Implications of Gap Clearing via Planets in Planetesimal (Debris) Disks." Diss., The University of Arizona, 2017. http://hdl.handle.net/10150/625603.

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Exoplanets and debris disks are examples of solar systems other than our own. As the dusty reservoirs of colliding planetesimals, debris disks provide indicators of planetary system evolution on orbital distance scales beyond those probed by the most prolific exoplanet detection methods, and on timescales $\sim$10 Myr to 10 Gyr. The Solar System possesses both planets and small bodies, and through studying the gravitational interactions between both, we gain insight into the Solar System's past. As we enter the era of resolved observations of debris disks residing around other stars, I add to

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JeongAhn, Youngmin, and Renu Malhotra. "Simplified Derivation of the Collision Probability of Two Objects in Independent Keplerian Orbits." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624717.

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Many topics in planetary studies demand an estimate of the collision probability of two objects moving on nearly Keplerian orbits. In the classic works of Opik and Wetherill, the collision probability was derived by linearizing the motion near the collision points, and there is now a vast amount of literature using their method. We present here a simpler and more physically motivated derivation for non-tangential collisions in Keplerian orbits, as well as for tangential collisions that were not previously considered. Our formulas have the added advantage of being manifestly symmetric in the pa

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Leconte, Jérémy. "Un nouveau regard sur la Structure interne et l'évolution des planètes géantes solaires et extrasolaires." Phd thesis, Ecole normale supérieure de lyon - ENS LYON, 2011. http://tel.archives-ouvertes.fr/tel-00707629.

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La détection et la caractérisation d'exoplanètes apparaissent clairement comme des thèmes centraux de l'observation astronomique pour les années à venir. Les projets spatiaux ou au sol sont nombreux (HARPS, CoRoT, Kepler, JWST, SPHERE...), mais les études théoriques visant à l'analyse et à la compréhension des données recueillies et à venir sont nécessaires. Durant cette thèse j'ai étudié divers processus physiques affectant la structure interne et l'évolution des planètes géantes, aussi bien au sein, qu'à l'extérieur de notre système solaire. J'ai notamment modélisé en détail: -L'impact de l'

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Batygin, Konstantin. "Orbits and Interiors of Planets." Thesis, 2012. https://thesis.library.caltech.edu/7056/1/thesis.pdf.

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<p>The focus of this thesis is a collection of problems of timely interest in orbital dynamics and interior structure of planetary bodies.</p> <p>The first three chapters are dedicated to understanding the interior structure of close-in, gaseous extrasolar planets (hot Jupiters). In order to resolve a long-standing problem of anomalously large hot Jupiter radii, we proposed a novel magnetohydrodynamic mechanism responsible for inflation. The mechanism relies on the electro-magnetic interactions between fast atmospheric flows and the planetary magnetic field in a thermally ionized atmospher

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Jansen, Tiffany Channelle. "It’s Not Just a Phase: Measuring the Properties of Short-Period Exoplanets from Full Orbital Phase Curves." Thesis, 2021. https://doi.org/10.7916/d8-r1cj-xm59.

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The amount of light an exoplanet reflects and emits towards an observer waxes and wanes as the planet orbits through its phases. The amplitude and profile of reflection phase curves constrain the albedo of planetary surfaces and atmospheres, while the thermal amplitude and profile reveal temperature distributions and heat transport efficiencies, all providing valuable insight into the nature of exoplanet surfaces and atmospheres. In this dissertation I highlight the usefulness of utilizing full orbital phase curves in addition to occultation measurements, which provides a higher sensitivity

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Books on the topic "Chaya Planets and Orbits"

1

Hegel, Georg Wilhelm Friedrich. Dissertatio philosophica de orbitis planetarum =: Philosophische Erörterung über die Planetenbahnen. Acta humaniora, 1986.

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2

Da, Su. Krayʻ taṃ khvanʻ nhaṅʻʹ ʼaukkā pyaṃ myāʺ. Cā pe bi mānʻ ʼa phvaiʹ, 1985.

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Thomas, Roatsch, ed. Data of the planetary system. Akademie Verlag Berlin, 1988.

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Martin, Vivian B. Astrocycles: How to make the major planetary cycles work for you. Ballantine Books, 1991.

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Fitzwalter, Bernard. Dark stars: Invisible focal points in astrology. Aquarian Press, 1988.

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Ferrini, Cinzia. Guida al De orbitis planetarum di Hegel ed alle sue edizioni e traduzioni: La pars destruens, confutazione dei fondamenti della meccanica celeste di Newton e dei suoi presupposti filosofici. P. Haupt, 1995.

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Rohde, James R. The satellite almanac users' guide. Nautical Almanac Office, U.S. Naval Observatory, 1988.

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Jardine, Nicholas. La guerre des astronomes: La querelle au sujet de l'origine du système géo-héliocentrique à la fin du XVIe siècle. Belles lettres, 2008.

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Jardine, Nicholas. La guerre des astronomes: La querelle au sujet de l'origine du système géo-héliocentrique à la fin du XVIe siècle. Belles lettres, 2008.

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Jardine, Nicholas. La guerre des astronomes: La querelle au sujet de l'origine du système géo-héliocentrique à la fin du XVIe siècle. Belles lettres, 2008.

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Book chapters on the topic "Chaya Planets and Orbits"

1

Padmanabhan, Thanu. "Orbits of Planets are Circles!" In Sleeping Beauties in Theoretical Physics. Springer International Publishing, 2015. http://dx.doi.org/10.1007/978-3-319-13443-7_3.

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Corda, Christian. "Newton, Einstein and the Advance of Planets’ Orbits." In Springer Proceedings in Physics. Springer International Publishing, 2024. http://dx.doi.org/10.1007/978-3-031-38477-6_3.

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Kleczek, J. "The Position of the Planets in their Orbits." In Exercises in Astronomy. Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3769-7_13.

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Gustafson, Bo Å. S., and Larsg G. Adolfsson. "Radiation Pressure Correction to Meteor Orbits." In Worlds in Interaction: Small Bodies and Planets of the Solar System. Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0209-1_44.

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Manoukian, E. B. "Perihelion Precession of Planets Orbits and the Schwinger-Binet Equation." In 100 Years of Fundamental Theoretical Physics in the Palm of Your Hand. Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-51081-7_56.

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Zheng, J. Q., M. J. Valtonen, S. Mikkola, M. Korpi, and H. Rickman. "Orbits of Short Period Comets Captured from the Oort Cloud." In Worlds in Interaction: Small Bodies and Planets of the Solar System. Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0209-1_9.

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Sanchez-Espiga, Javier, Alberto Diez-Ibarbia, Ana de Juan, Pablo García, Alfonso Fernandez-del-Rincon, and Fernando Viadero. "Impact of the Load in the Orbits Described by the Sun Gear in a Planetary Gear Set with an Odd Number of Planets." In Mechanisms and Machine Science. Springer Nature Switzerland, 2024. http://dx.doi.org/10.1007/978-3-031-67295-8_36.

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Chambers, John, and Jacqueline Mitton. "Nursery for Planets." In From Dust to Life. Princeton University Press, 2017. http://dx.doi.org/10.23943/princeton/9780691175706.003.0008.

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This chapter illustrates how the solar system has a decidedly two-dimensional aspect to it. The orbits of the eight major planets all lie in almost the same plane, deviating by no more than seven degrees. Bodies in the asteroid belt and the Kuiper belt stray a little further afield, but these belts are arranged like flattened donuts, aligned with the same plane as the planets. Immanuel Kant and Pierre-Simon de Laplace noted the planar nature of the solar system and used this as the basis for their nebular theories in which the solar system grew out of a flattened disk of matter. Young stars li

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Jeshion, Robin. "Descriptive Descriptive Names." In Descriptions and Beyond. Oxford University PressOxford, 2004. http://dx.doi.org/10.1093/oso/9780199270514.003.0019.

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Abstract On June 5, 1599, in Sevilla, a baby boy let out his first wail. The next day, he was baptized. His parents, or a priest, proclaim that his name is Diego Vela´zquez. Fifty-six years later, we can imagine Vela´zquez before his newly finished fascinating masterpiece declaring that its name is Las Meninas. As we all know, Leverrier isolated discrepancies between the calculated orbits and the measured orbits of the other planets and hypothesized that there was another planet in our solar system whose gravitational force was responsible for the discrepancy. Prior to any telescopic identific

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Emelyanov, Nikolay. "The evolution of the orbits of the planetary satellites." In The Dynamics of Natural Satellites of the Planets. Elsevier, 2021. http://dx.doi.org/10.1016/b978-0-12-822704-6.00015-7.

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Conference papers on the topic "Chaya Planets and Orbits"

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Veljan, Darko. "Planets are (very likely) in orbits of stars." In 4th Croatian Combinatorial Days. University of Zagreb Faculty of Civil Engineering, 2023. http://dx.doi.org/10.5592/co/ccd.2022.10.

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Ipatov, S. "Migration of planetesimals in the TRAPPIST-1 exoplanetary system." In Modern astronomy: from the Early Universe to exoplanets and black holes. Special Astrophysical Observatory of the Russian Academy of Sciences, 2024. https://doi.org/10.26119/vak2024.135.

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The calculations of the motion of planetesimals at the late stages of accumulation of planets in the TRAPPIST-1 system were made. In each calculation variant, initial orbits of planetesimals were near one of the planets. The number of collisions of planetesimals with the planets were calculated. The calculations has shown that the outer layers of neighboring exoplanets in the TRAPPIST-1 system can include similar material if there were a lot of planetesimals near their orbits at the late stages of the accumulation of the exoplanets.

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Marov, M. Ya, and I. I. Shevchenko. "Planets — a modern view." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.005.

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The modern view of planets goes far beyond the usual concept of the planets as bodies of the Solar system. The discovery ofexoplanets has immeasurably expanded the understanding of the architecture and properties of planetary systems. Majoradvances have been made in the study of the planets and minor bodies of the Solar system. However, no answers havebeen received to fundamental questions about the causes of various paths of evolution and formation of planetary naturalcomplexes. To give answers to these questions, research on exoplanets is called upon, of which more than 5000 have beendiscove

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Kuznetsov, E., and A. Perminov. "Investigation of the dynamical evolution of the compact planetary system K2-72." In Modern astronomy: from the Early Universe to exoplanets and black holes. Special Astrophysical Observatory of the Russian Academy of Sciences, 2024. https://doi.org/10.26119/vak2024.136.

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We consider the dynamic evolution of the compact four-planet system K2-72. The star K2-72 is an M-type dwarf. The system contains three Earth-like planets and one super-Earth. We searched for low-order resonances within the uncertainty of determining the periods of the planets. To determine the resonant combinations of the semimajor axes of the orbits, the ratio of the mean motions of neighboring planets was represented as a segment of a sequence of convergent fractions. We considered a few scenarios for the evolution of the K2-72 system over 100 Myr using the Posidonius software, which allows

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Abdulmyanov, T. "Formation of single stars and their planetary systems, typicality of the Solar system." In Modern astronomy: from the Early Universe to exoplanets and black holes. Special Astrophysical Observatory of the Russian Academy of Sciences, 2024. https://doi.org/10.26119/vak2024.044.

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In this paper, we determine the dynamic viscosity for the case of pulsating disturbances in the density of gas-dust disks. The characteristic velocities of the disk dust particles are divided into separate classes of orbits with Keplerian and near-Keplerian motions. For these classes, we obtain formulas for the dynamic viscosity. We analyze the distributions of exoplanets by their masses, major semi-axes, and eccentricities of their orbits. We conclude that hot giant planets can be located on complex, unstable orbits of accretion onto the central star.

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Ford, Eric B. "Quantifying the Uncertainty in the Orbits of Extrasolar Planets with Markov Chain Monte Carlo." In THE SEARCH FOR OTHER WORLDS: Fourteenth Astrophysics Conference. AIP, 2004. http://dx.doi.org/10.1063/1.1774494.

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Ipatov, S. I. "Formation of the terrestrial planets and the Moon." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.083.

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The amounts of material from diﬀerent parts of the zone from 0.7 to 1.5 AU from the Sun, which entered into almostformed the Earth and Venus, diﬀered for these planets by no more than 3 times. For the TRAPPIST exoplanetary system,the ratio of the fraction of planetesimals collided with the planet, around which orbit initial orbits of planetesimals werelocated, to the fraction of planetesimals collided with the neighbouring planet was typically less than 4. Embryos of theEarth and the Moon with a total mass equaled to about 0.01-0.1 Earth mass could be formed as a result of compressionof a rare

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Ipatov, S. "Exchange of meteorites between the terrestrial planets and the Moon." In Modern astronomy: from the Early Universe to exoplanets and black holes. Special Astrophysical Observatory of the Russian Academy of Sciences, 2024. https://doi.org/10.26119/vak2024.143.

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The evolution of the orbits of bodies ejected from the Earth, Moon, Mercury and Mars was studied. The probabilities of collisions of ejected bodies with planets depended on ejection velocities, ejection angles and points of ejection. At a velocity of ejection close to the parabolic velocity, most of bodies fell onto the planet from which they had been ejected. Below results are presented not for such small ejection velocities. At ejection velocities about 12-14 km/s, the fraction of bodies ejected from the Earth that fall back onto the Earth was about 0.15-0.25. The total number of bodies ejec

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Shao, Michael, Stephen C. Unwin, Charles Beichman, et al. "Finding Earth clones with SIM: The most promising near-term technique to detect, find masses for, and determine three-dimensional orbits of nearby habitable planets." In Optical Engineering + Applications, edited by Daniel R. Coulter. SPIE, 2007. http://dx.doi.org/10.1117/12.734671.

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