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Journal articles on the topic 'Chaya Planets and Orbits/Planetary Positions'

Author: Grafiati

Published: 5 June 2025

Last updated: 2 August 2025

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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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Sharma, Pravesh, Suresh Kumar Sahani, Kameshwar Sahani, and Kritika Sharma. "Modeling Planetary and Stellar Motion Using Differential Equations." ARZUSIN 3, no. 6 (2023): 769–82. http://dx.doi.org/10.58578/arzusin.v3i6.1991.

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The report aims to explore the application of differential equations in modeling the motion of planets and stars within our universe, serving as an introduction to the captivating realm of celestial mechanics. We utilize differential equations to represent the movement and positions of celestial bodies within a gravitational field, grounding our analysis in Newton's laws of motion and gravitation. Moreover, we employ Kepler's laws of planetary motion to elucidate the orbits of planets around the sun. It is important to note that this report offers a simplified perspective, designed for educati

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Lazzoni, C., S. Desidera, F. Marzari, et al. "Dynamical models to explain observations with SPHERE in planetary systems with double debris belts." Astronomy & Astrophysics 611 (March 2018): A43. http://dx.doi.org/10.1051/0004-6361/201731426.

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Context. A large number of systems harboring a debris disk show evidence for a double belt architecture. One hypothesis for explaining the gap between the debris belts in these disks is the presence of one or more planets dynamically carving it. For this reason these disks represent prime targets for searching planets using direct imaging instruments, like the Spectro-Polarimetric High-constrast Exoplanet Research (SPHERE) at the Very Large Telescope.Aim. The goal of this work is to investigate this scenario in systems harboring debris disks divided into two components, placed, respectively, i

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Pitjeva, E. V. "Influence of trans-neptunian objects on motion of major planets and limitation on the total TNO mass from planet and spacecraft ranging." Proceedings of the International Astronomical Union 5, S263 (2009): 93–97. http://dx.doi.org/10.1017/s1743921310001560.

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AbstractPerturbations from asteroids and Trans-Neptunian Objects affect significantly on the orbits of planets and should be taken into account when high-accuracy planetary ephemerides are constructed. On the other hand, from an analysis of motion of the major planets by processing of precise measurements of spacecraft a limitation on the total TNO mass may be obtained. To estimate influence of TNO on motion of planets the largest 21 TNO have been included into the process of simultaneous numerical integration, and positions of planets obtained with taking for TNO have been compared with posit

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Bartram, Peter, Alexander Wittig, Jack J. Lissauer, Sacha Gavino, and Hodei Urrutxua. "Orbital stability of compact three-planet systems – II: post-instability impact behaviour." Monthly Notices of the Royal Astronomical Society 506, no. 4 (2021): 6181–94. http://dx.doi.org/10.1093/mnras/stab1465.

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ABSTRACT Recent observational missions have uncovered a significant number of compact multi-exoplanet systems. The tight orbital spacing of these systems has led to much effort being applied to the understanding of their stability; however, a key limitation of the majority of these studies is the termination of simulations as soon as the orbits of two planets cross. In this work we explore the stability of compact, three-planet systems, and continue our simulations all the way to the first collision of planets to yield a better understanding of the lifetime of these systems. We perform over 25

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McTier, Moiya A. S., David M. Kipping, and Kathryn Johnston. "8 in 10 Stars in the Milky Way Bulge experience stellar encounters within 1000 AU in a gigayear." Monthly Notices of the Royal Astronomical Society 495, no. 2 (2020): 2105–11. http://dx.doi.org/10.1093/mnras/staa1232.

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ABSTRACT The Galactic bulge is a tumultuous dense region of space, packed with stars separated by far smaller distances than those in the Solar neighbourhood. A quantification of the frequency and proximity of close stellar encounters in this environment dictates the exchange of material, disruption of planetary orbits, and threat of sterilizing energetic events. We present estimated encounter rates for stars in the Milky Way bulge found using a combination of numerical and analytical methods. By integrating the orbits of bulge stars with varying orbital energy and angular momentum to find the

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Socas-Navarro, Hector. "On the Connection between Planets, Dark Matter and Cancer: Comment on “Planetary Dependence of Melanoma”." Biophysical Reviews and Letters 14, no. 01 (2019): 1–9. http://dx.doi.org/10.1142/s1793048019200017.

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In a recent paper, Zioutas and Valachovic (2018) claim that dark matter is responsible for a significant fraction of the melanoma skin cancer. This conclusion is drawn from their observation of a significant correlation between skin melanoma incidence in the US and the inner planets positions (especially those of Mercury and Earth). Here, I present a number of objections to their interpretation. Some (but not all) of the counterarguments are based on the analysis of a larger dataset from the same source, considering more cancer types and separating by patient attributes, such as race. One of t

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Gordon, Tyler A., and Eric Agol. "Analytic Light Curve for Mutual Transits of Two Bodies Across a Limb-darkened Star." Astronomical Journal 164, no. 3 (2022): 111. http://dx.doi.org/10.3847/1538-3881/ac82b1.

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Abstract We present a solution for the light curve of two bodies mutually transiting a star with polynomial limb darkening. The term “mutual transit” in this work refers to a transit of the star during which overlap occurs between the two transiting bodies. These could be an exoplanet with an exomoon companion, two exoplanets, an eclipsing binary and a planet, or two stars eclipsing a third in a triple-star system. We include analytic derivatives of the light curve with respect to the positions and radii of both bodies. We provide code that implements a photodynamical model for a mutual transi

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Fienga, A., A. Di Ruscio, L. Bernus, et al. "New constraints on the location of P9 obtained with the INPOP19a planetary ephemeris." Astronomy & Astrophysics 640 (July 28, 2020): A6. http://dx.doi.org/10.1051/0004-6361/202037919.

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Context. We used the new released INPOP19a planetary ephemerides benefiting from Jupiter-updated positions by the Juno mission and reanalyzed Cassini observations. Aims. We test possible locations of the unknown planet P9. To do this, we used the perturbations it produces on the orbits of the outer planets, more specifically, on the orbit of Saturn. Methods. Two statistical criteria were used to identify possible acceptable locations of P9 according to (i) the difference in planetary positions when P9 is included compared with the propagated covariance matrix, and (ii) the χ2 likelihood of pos

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Tang, K., Y. Z. Song, K. X. Shen, et al. "The orbit of Triton with new precise observations and the INPOP19a ephemeris." Astronomy & Astrophysics 641 (September 2020): A108. http://dx.doi.org/10.1051/0004-6361/202038556.

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Aims. The Gaia catalogue brings new opportunities and challenges to high-precision astronomy and astrometry. The precision of data reduction is therefore improved by a large number of reference stars with high-precision positions and proper motions. Numerous precise positions for Triton are obtained from the latest observations using the Gaia catalogue. Furthermore, the new INPOP19a planetary ephemeris, which also fits the observations from the Gaia Data Release 2, has recently become available. In this paper, a new orbit of Triton is calculated using the latest precise charge-coupled device (

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Guo, Y. J., G. Y. Li, K. J. Lee, and R. N. Caballero. "Studying the Solar system dynamics using pulsar timing arrays and the LINIMOSS dynamical model." Monthly Notices of the Royal Astronomical Society 489, no. 4 (2019): 5573–81. http://dx.doi.org/10.1093/mnras/stz2515.

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ABSTRACT Pulsar timing arrays (PTAs) can be used to study the Solar system ephemeris (SSE), the errors of which can lead to correlated timing residuals and significantly contribute to the PTA noise budget. Most Solar system studies with PTAs assume the dominance of the term from the shift of the Solar system barycentre (SSB). However, it is unclear to which extent this approximation can be valid, since the perturbations on the planetary orbits may become important as data precision keeps increasing. To better understand the effects of SSE uncertainties on pulsar timing, we develop the linimoss

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Echeverri, Daniel, Jerry W. Xuan, John D. Monnier, et al. "Vortex Fiber Nulling for Exoplanet Observations: First Direct Detection of M Dwarf Companions around HIP 21543, HIP 94666, and HIP 50319." Astrophysical Journal Letters 965, no. 2 (2024): L15. http://dx.doi.org/10.3847/2041-8213/ad3619.

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Abstract Vortex fiber nulling (VFN) is a technique for detecting and characterizing faint companions at small separations from their host star. A near-infrared (∼2.3 μm) VFN demonstrator mode was deployed on the Keck Planet Imager and Characterizer (KPIC) instrument at the Keck Observatory and presented earlier. In this Letter, we present the first VFN companion detections. Three targets, HIP 21543 Ab, HIP 94666 Ab, and HIP 50319 B, were detected with host–companion flux ratios between 70 and 430 at and within one diffraction beamwidth (λ/D). We complement the spectra from KPIC VFN with flux r

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Poquet, Juan J. Schulz. "A test to the constancy of the velocity of light with our solar system." Physics Essays 36, no. 4 (2023): 377–84. http://dx.doi.org/10.4006/0836-1398-36.4.377.

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This article is a detailed proposal of an astronomical test to be carried out within our solar system to try to detect the eventual addition of the speed of a celestial body to that of its emitted light -that reflected of the Sun in this case. This eventuality could be determined by observing the consequent variation in its apparent position that could produce the variation of the angle of aberration, a consequence, in turn, of the variation of the velocity of its emitted light. This area is chosen, despite having here celestial bodies with lower speeds than those of the stars, and their conse

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Degnan, John J. "Multipurpose Laser Instrument for Interplanetary Ranging, Time Transfer, and Wideband Communications †." Photonics 10, no. 2 (2023): 98. http://dx.doi.org/10.3390/photonics10020098.

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In this paper, we discuss the design and feasibility of a multifunctional laser instrument capable of precision ranging, time transfer, and wideband communications over interplanetary distances throughout our solar system. To simplify the communications discussion, On-Off Keying (OOK) is assumed for the high bandwidth (MHz to GHz) modulation format, and the required laser powers and transmit and receive apertures are determined for each Earth–planet link as a function of data rate. Optimization of the transmitter and receiver antenna gains is reviewed. It is further assumed that the spacecraft

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Vaduvescu, O., L. Hudin, T. Mocnik, et al. "280 one-opposition near-Earth asteroids recovered by the EURONEAR with the Isaac Newton Telescope." Astronomy & Astrophysics 609 (January 2018): A105. http://dx.doi.org/10.1051/0004-6361/201731844.

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Context. One-opposition near-Earth asteroids (NEAs) are growing in number, and they must be recovered to prevent loss and mismatch risk, and to improve their orbits, as they are likely to be too faint for detection in shallow surveys at future apparitions. Aims. We aimed to recover more than half of the one-opposition NEAs recommended for observations by the Minor Planet Center (MPC) using the Isaac Newton Telescope (INT) in soft-override mode and some fractions of available D-nights. During about 130 h in total between 2013 and 2016, we targeted 368 NEAs, among which 56 potentially hazardous

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Ferreira, J. F., P. Tanga, F. Spoto, P. Machado, and D. Herald. "Asteroid astrometry by stellar occultations: Accuracy of the existing sample from orbital fitting." Astronomy & Astrophysics 658 (February 2022): A73. http://dx.doi.org/10.1051/0004-6361/202141753.

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Context. The technique of stellar occultations, greatly enhanced by the publication of the Gaia data releases, permits not only the determination of asteroid size and shape, but also the retrieval of additional, very accurate astrometry, with a possible relevant impact on the study of dynamical properties. The use of Gaia as reference catalogue and the recent implementation of an improved error model for occultation astrometry offer the opportunity to test its global astrometric performance on the whole existing data set of observed events, dominated by minor planets belonging to the main belt

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Grandjean, A., A. M. Lagrange, H. Beust, et al. "Constraining the properties of HD 206893 B." Astronomy & Astrophysics 627 (July 2019): L9. http://dx.doi.org/10.1051/0004-6361/201935044.

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Context. High contrast imaging enables the determination of orbital parameters for substellar companions (planets, brown dwarfs) from the observed relative astrometry and the estimation of model and age-dependent masses from their observed magnitudes or spectra. Combining astrometric positions with radial velocity gives direct constraints on the orbit and on the dynamical masses of companions. A brown dwarf was discovered with the VLT/SPHERE instrument at the Very Large Telescope (VLT) in 2017, which orbits at ∼11 au around HD 206893. Its mass was estimated between 12 and 50 MJ from evolutiona

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18

Heller, René. "Formation of hot Jupiters through disk migration and evolving stellar tides." Astronomy & Astrophysics 628 (August 2019): A42. http://dx.doi.org/10.1051/0004-6361/201833486.

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Since the discovery of Jupiter-sized planets in extremely close orbits around Sun-like stars, several mechanisms have been proposed to produce these “hot Jupiters”. Here we address their pile-up at 0.05 AU observed in stellar radial velocity surveys, their long-term orbital stability in the presence of stellar tides, and their occurrence rate of 1.2 ± 0.38% in one framework. We calculate the combined torques on the planet from the stellar dynamical tide and from the protoplanetary disk in the type-II migration regime. The disk is modeled as a 2D nonisothermal viscous disk parameterized to repr

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Kong, Zhihui, Anders Johansen, Michiel Lambrechts, H. Jonathan Jiang, and Zong-Hong Zhu. "How the presence of a giant planet affects the outcome of terrestrial planet formation simulations." Astronomy & Astrophysics, May 22, 2024. http://dx.doi.org/10.1051/0004-6361/202349043.

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The architecture and masses of planetary systems in the habitable zone could be strongly influenced by the presence of outer giant planets. Here, we investigate the impact of outer giants on terrestrial planet formation, under the assumption that the final assembly of the planetary system is set by a giant impact phase. Utilizing a state-of-the-art N-body simulation software, GENGA, we interpret how the late stage of terrestrial planet formation contributes to diversity among planetary systems. We designed two global model setups: 1) we placed a gas giant on the outer side of planetesimals and

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Emelyanov, N. V., M. Yu Kovalev, and M. I. Varfolomeev. "The orbits of outer planetary satellites using the Gaia data." Monthly Notices of the Royal Astronomical Society, March 30, 2023. http://dx.doi.org/10.1093/mnras/stad958.

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Abstract Launch of the Gaia space observatory started a new era in astrometry when the accuracy of star coordinates increased by thousands of times. Significant improvement of accuracy was also expected for the coordinates of the Solar system bodies. Gaia DR3 provided us with the data which could be used to test our expectations. In this work, we refine the orbits of a number of outer planetary salellites using both ground-based and Gaia observations. From thirteen outer satellites observed by Gaia, we chose six to obtain their orbits. Some specific moments in using observations of outer satel

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Krommydas, Dimitrios, and Fabio Scardigli. "Exponential distance relation (aka Titius-Bode rule) in extra solar planetary systems." Monthly Notices of the Royal Astronomical Society, March 11, 2025. https://doi.org/10.1093/mnras/staf405.

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Abstract In this paper we present phenomenological evidence for the validity of an exponential distance relation (also known as generalized Titius-Bode law) in the 32 planetary systems (31 extra solar, plus our Solar System) containing at least 5 planets each (known up to July 2023). We produce the semi-log fittings of the data, and we check them against the statistical indicators of R2 and Median. Then we compare them with the data of 4000 artificial planetary systems created at random. In this way, a possible origin by chance of the Titius-Bode rule (TBR) is reasonably excluded. We also poin

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Llorente de Andres, F., P. Cruz, D. Cuenda-Muñoz, E. J. Alfaro, C. Chavero, and C. Cifuentes. "The evolution of lithium in FGK dwarf stars. Influence of planets and Galactic migration." Astronomy & Astrophysics, February 5, 2024. http://dx.doi.org/10.1051/0004-6361/202346744.

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This work aims to investigate the behaviour of the lithium abundance in stars with and without detected planets. Our study is based on a sample of 1332 FGK main-sequence stars with measured lithium abundances, for 257 of which planets were detected. Our method reviews the sample statistics and is addressed specifically to the influence of tides and orbital decay, with special attention to planets on close orbits, whose stellar rotational velocity is higher than the orbital period of the planet. In this case, tidal effects are much more pronounced. The analysis also covers the orbital decay on

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Benedetti-Rossi, G., R. Ribeiro, O. C. Winter, H. S. Gaspar, and E. Vieira-Neto. "Accretion of ice giant planets from massive protoplanets whose migration is blocked by Jupiter and Saturn." Monthly Notices of the Royal Astronomical Society, October 5, 2023. http://dx.doi.org/10.1093/mnras/stad3017.

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Abstract The growth and dynamical evolution of protoplanets beyond Saturn through collisions and type I migration typically result in a highly chaotic dynamics, producing a diversity of outcomes depending on the initial conditions. Here we present the results of N-bodies numerical simulations aiming to make a detailed exploration of different initial conditions and potential outcomes for this dynamics. We consider Jupiter and Saturn at the imminence of crossing the 3:2 mean motion resonance in two possible positions based on the final and initial conditions of the Grand Tack and the Nice model

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