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Journal articles on the topic 'Exploration of Saturn (Planet)'

Author: Grafiati

Published: 4 June 2021

Last updated: 28 July 2025

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1

Spilker, Linda. "Cassini-Huygens’ exploration of the Saturn system: 13 years of discovery." Science 364, no. 6445 (2019): 1046–51. http://dx.doi.org/10.1126/science.aat3760.

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The Cassini-Huygens mission to Saturn provided a close-up study of the gas giant planet, as well as its rings, moons, and magnetosphere. The Cassini spacecraft arrived at Saturn in 2004, dropped the Huygens probe to study the atmosphere and surface of Saturn’s planet-sized moon Titan, and orbited Saturn for the next 13 years. In 2017, when it was running low on fuel, Cassini was intentionally vaporized in Saturn’s atmosphere to protect the ocean moons, Enceladus and Titan, where it had discovered habitats potentially suitable for life. Mission findings include Enceladus’ south polar geysers, t

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Crotts, Katie A., Aarynn L. Carter, Kellen Lawson, et al. "Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam." Astrophysical Journal Letters 987, no. 2 (2025): L41. https://doi.org/10.3847/2041-8213/ade798.

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Abstract The young M star TWA 7 hosts a bright and near face-on debris disk, which has been imaged from the optical to the submillimeter. The disk displays multiple complex substructures such as three disk components, a large dust clump, and spiral arms, suggesting the presence of planets to actively sculpt these features. The evidence for planets in this disk was further strengthened with the recent detection of a point source compatible with a Saturn-mass planet companion using JWST/MIRI at 11 μm, at the location a planet was predicted to reside based on the disk morphology. In this Letter,

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de la Fuente Marcos, C., and R. de la Fuente Marcos. "Centaur 2013 VZ₇₀: Debris from Saturn’s irregular moon population?" Astronomy & Astrophysics 657 (January 2022): A59. http://dx.doi.org/10.1051/0004-6361/202142166.

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Context. Saturn has an excess of irregular moons. This is thought to be the result of past collisional events. Debris produced during such episodes in the neighborhood of a host planet can evolve into co-orbitals trapped in quasi-satellite and/or horseshoe resonant states. A recently announced centaur, 2013 VZ70, follows an orbit that could be compatible with those of prograde Saturn’s co-orbitals. Aims. We perform an exploration of the short-term dynamical evolution of 2013 VZ70 to confirm or reject a co-orbital relationship with Saturn. A possible connection with Saturn’s irregular moon popu

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Solórzano, Carlos Renato Huaura, Antonio Fernando Bertachini de Almeida Prado, and Alexander Alexandrovich Sukhanov. "Analysis of Electric Propulsion System for Exploration of Saturn." Mathematical Problems in Engineering 2009 (2009): 1–14. http://dx.doi.org/10.1155/2009/756037.

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Exploration of the outer planets has experienced new interest with the launch of the Cassini and the New Horizons Missions. At the present time, new technologies are under study for the better use of electric propulsion system in deep space missions. In the present paper, the method of the transporting trajectory is used to study this problem. This approximated method for the flight optimization with power-limited low thrust is based on the linearization of the motion of a spacecraft near a keplerian orbit that is close to the transfer trajectory. With the goal of maximizing the mass to be del

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Wakeford, H. R., and P. A. Dalba. "The exoplanet perspective on future ice giant exploration." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 378, no. 2187 (2020): 20200054. http://dx.doi.org/10.1098/rsta.2020.0054.

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Exoplanets number in their thousands, and the number is ever increasing with the advent of new surveys and improved instrumentation. One of the most surprising things we have learnt from these discoveries is not that small-rocky planets in their stars habitable zones are likely to be common, but that the most typical size of exoplanets is that not seen in our solar system—radii between that of Neptune and the Earth dubbed mini-Neptunes and super-Earths. In fact, a transiting exoplanet is four times as likely to be in this size regime than that of any giant planet in our solar system. Investiga

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Palotai, Csaba, Shawn Brueshaber, Ramanakumar Sankar, and Kunio Sayanagi. "Moist Convection in the Giant Planet Atmospheres." Remote Sensing 15, no. 1 (2022): 219. http://dx.doi.org/10.3390/rs15010219.

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The outer planets of our Solar System display a myriad of interesting cloud features, of different colors and sizes. The differences between the types of observed clouds suggest a complex interplay between the dynamics and chemistry at play in these atmospheres. Particularly, the stark difference between the banded structures of Jupiter and Saturn vs. the sporadic clouds on the ice giants highlights the varieties in dynamic, chemical and thermal processes that shape these atmospheres. Since the early explorations of these planets by spacecrafts, such as Voyager and Voyager 2, there are many ou

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Courtin, Régis, Melissa A. McGrath, Guy J. Consolmagno, et al. "COMMISSION 16: PHYSICAL STUDY OF PLANETS AND SATELLITES." Proceedings of the International Astronomical Union 4, T27A (2008): 163–68. http://dx.doi.org/10.1017/s1743921308025416.

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This report is divided in four parts: the first part summarizes the activities of the Commission between September 2006 and June 2008; the second part reports on recent advances in the physical study of planets and satellites. However, instead of attempting to cover the large body of new knowledge gathered over the last three years, we have chosen to highlight just a few exciting results – on Mercury, the exploration of unchartered terrains with ground-based imaging and a new measurement of its libration parameters, some spectacular findings from the Cassini mission inside the Saturnian system

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Encrenaz, T., R. Kallenbach, T. C. Owen, and C. Sotin. "A Comparative Study of the Outer Planets before the Exploration of Saturn by Cassini/Huygens: Introduction." Space Science Reviews 116, no. 1-2 (2005): 1–7. http://dx.doi.org/10.1007/s11214-005-1944-4.

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9

Eastland, Grant. "Considerations of undersea exploration of an extraterrestrial ocean." Journal of the Acoustical Society of America 153, no. 3_supplement (2023): A281. http://dx.doi.org/10.1121/10.0018848.

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Hypothetical investigations and simulations of the potential effects to acoustic propagation and modal structures in oceans on extraterrestrial planets and moons are presented. Europa, one of the many moons of Jupiter is thought to have a water-based ocean that has a depth of 60 to 150 km and covered by a suspected 15 to 25 km thick ice sheet. Another moon of Jupiter, Ganymede, is the largest moon in our solar system is thought to have an underground saltwater sea 100 km deep. Titan, a moon of Saturn, is also thought to have a water-based sea under an ice sheet in addition to surface, rivers,

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Bockelée-Morvan, Dominique. "Comet composition and Lab." Proceedings of the International Astronomical Union 11, A29A (2015): 227. http://dx.doi.org/10.1017/s1743921316002933.

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The XXIX IAU General Assembly took place during the golden year of the exploration of small solar system bodies. With the Rosetta ESA mission around comet 67P, NASA Dawn and New Horizons missions nearby dwarf planets Ceres and Pluto, respectively, and the NASA/Cassini mission in Saturn neighborhood, year 2015 marked an important step towards further understanding of small solar system bodies. On August 11-13, Focus meeting 9 "Highlights in the exploration of small worlds" gathered scientists of all over the world to present and discuss the spectacular results obtained from these missions, as w

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Hueso, R., T. Guillot, and A. Sánchez-Lavega. "Convective storms and atmospheric vertical structure in Uranus and Neptune." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 378, no. 2187 (2020): 20190476. http://dx.doi.org/10.1098/rsta.2019.0476.

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The ice giants Uranus and Neptune have hydrogen-based atmospheres with several constituents that condense in their cold upper atmospheres. A small number of bright cloud systems observed in both planets are good candidates for moist convective storms, but their observed properties (size, temporal scales and cycles of activity) differ from moist convective storms in the gas giants. These clouds and storms are possibly due to methane condensation and observations also suggest deeper clouds of hydrogen sulfide (H 2 S) at depths of a few bars. Even deeper, thermochemical models predict clouds of a

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Marchenko, Alexander N., Serhii Perii, Ivan Pokotylo, and Zoryana Tartachynska. "GEODYNAMICS." GEODYNAMICS 2(31)2021, no. 2(31) (2021): 5–15. http://dx.doi.org/10.23939/jgd2021.02.005.

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The basic goal of this study (as the first step) is to collect the appropriate set of the fundamental astronomic-geodetics parameters for their further use to obtain the components of the density distributions for the terrestrial and outer planets of the Solar system (in the time interval of more than 10 years). The initial data were adopted from several steps of the general way of the exploration of the Solar system by iterations through different spacecraft. The mechanical and geometrical parameters of the planets allow finding the solution of the inverse gravitational problem (as the second

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Briggs, Geoffrey A. "Future Solar System Missions." International Astronomical Union Colloquium 123 (1990): 297–306. http://dx.doi.org/10.1017/s0252921100077204.

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After a decade long hiatus in launches beyond Earth orbit, NASA’s planetary exploration program is again moving forward, beginning with the Magellan launch to Venus in May 1989 and the Galileo launch to Jupiter in October 1989. These spacecraft will reach their targets in August 1990 and December 1995, respectively. Both are missions of longstanding priority, Magellan to provide the first global high resolution mapping of the cloud-shrouded Venus surface, Galileo to make comprehensive measurements of the Jovian system in follow-up to the 1979/1980 Voyager flybys.Beyond these two missions there

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Melin, Henrik. "The upper atmospheres of Uranus and Neptune." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 378, no. 2187 (2020): 20190478. http://dx.doi.org/10.1098/rsta.2019.0478.

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We review the current understanding of the upper atmospheres of Uranus and Neptune, and explore the upcoming opportunities available to study these exciting planets. The ice giants are the least understood planets in the solar system, having been only visited by a single spacecraft, in 1986 and 1989, respectively. The upper atmosphere plays a critical role in connecting the atmosphere to the forces and processes contained within the magnetic field. For example, auroral current systems can drive charged particles into the atmosphere, heating it by way of Joule heating. Ground-based observations

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Bannova, Olga, Vera Mayorova, Veronika Pavlyuchenko, Mikhail Denisov, and Vladimir Igritsky. "A Conceptual Mission Architecture of a Robotic Spaceflight to Enceladus for Enabling Exploration of its Surface and Subglacial Ocean." Journal of the British Interplanetary Society 77, no. 6 (2024): 202–10. https://doi.org/10.59332/jbis-077-06-0202.

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Sixth-largest moon of Saturn Enceladus is one of the most promising destinations in the Solar System to search for possible presence of extraterrestrial life. The basis of such assumptions is the confirmed presence of a large accumulation of water around Enceladus South Pole under a layer of newly formed ice of 3 to 5 km thick. In the same region, many cryovolcanic sources have been observed, studying of which can provide understanding about development of life on Earth and searching for life on other planets in the Solar System. The paper presents a conceptual mission architecture to explore

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Karachevtseva, I. P., A. A. Kokhanov, J. F. Rodionova, A. Yu Zharkova, and M. S. Lazareva. "MAPPING OF INNER AND OUTER CELESTIAL BODIES USING NEW GLOBAL AND LOCAL TOPOGRAPHIC DATA DERIVED FROM PHOTOGRAMMETRIC IMAGE PROCESSING." ISPRS - International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences XLI-B4 (June 13, 2016): 411–15. http://dx.doi.org/10.5194/isprs-archives-xli-b4-411-2016.

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New estimation of fundamental geodetic parameters and global and local topography of planets and satellites provide basic coordinate systems for mapping as well as opportunities for studies of processes on their surfaces. The main targets of our study are Europa, Ganymede, Calisto and Io (satellites of Jupiter), Enceladus (a satellite of Saturn), terrestrial planetary bodies, including Mercury, the Moon and Phobos, one of the Martian satellites. In particular, based on new global shape models derived from three-dimensional control point networks and processing of high-resolution stereo images,

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Karachevtseva, I. P., A. A. Kokhanov, J. F. Rodionova, A. Yu Zharkova, and M. S. Lazareva. "MAPPING OF INNER AND OUTER CELESTIAL BODIES USING NEW GLOBAL AND LOCAL TOPOGRAPHIC DATA DERIVED FROM PHOTOGRAMMETRIC IMAGE PROCESSING." ISPRS - International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences XLI-B4 (June 13, 2016): 411–15. http://dx.doi.org/10.5194/isprsarchives-xli-b4-411-2016.

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New estimation of fundamental geodetic parameters and global and local topography of planets and satellites provide basic coordinate systems for mapping as well as opportunities for studies of processes on their surfaces. The main targets of our study are Europa, Ganymede, Calisto and Io (satellites of Jupiter), Enceladus (a satellite of Saturn), terrestrial planetary bodies, including Mercury, the Moon and Phobos, one of the Martian satellites. In particular, based on new global shape models derived from three-dimensional control point networks and processing of high-resolution stereo images,

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Museyib Mammadova, Turkan, Turkana Mirzali Aliyeva, and Vafa Ajdar Gafarova. "SATURN PLANETİNİN MÜŞAHİDƏSİ VƏ TƏDQİQİ TARİXİNDƏN." NATURE AND SCIENCE 01, no. 01 (2019): 28–29. http://dx.doi.org/10.36719/aem/2019/01/28-29.

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Miller, Steve, Tom Stallard, Chris Smith, et al. ": the driver of giant planet atmospheres." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 364, no. 1848 (2006): 3121–37. http://dx.doi.org/10.1098/rsta.2006.1877.

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We present a review of recent developments in the use of molecular ion as a probe of physics and chemistry of the upper atmospheres of giant planets. This ion is shown to be a good tracer of energy inputs into Jupiter (J), Saturn (S) and Uranus (U). It also acts as a ‘thermostat’, offsetting increases in the energy inputs owing to particle precipitation via cooling to space (J and U). Computer models have established that is also the main contributor to ionospheric conductivity. The coupling of electric and magnetic fields in the auroral polar regions leads to ion winds, which, in turn, drive

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Roncato, Sergio. "Saturn and its Rings: Four Centuries of Imperfect Amodal Completion." i-Perception 10, no. 1 (2019): 204166951882208. http://dx.doi.org/10.1177/2041669518822084.

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The planet Saturn is a familiar image for us, but it presents perceptual peculiarities that impeded the discovery of its structure and which can still be misleading today. Saturn appears to be surrounded by rings which hide it to a certain extent and then continue behind the outline of the planet. What we perceive is the result of a double amodal completion in which the planetary globe and the rings exchange the roles of occluding and occluded surface. Saturn was hidden to 17th-century astronomers for half a century because their rudimentary telescopes did not reveal the pictorial clues that a

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Friedman, Louis. "Planet Exploration." Science 244, no. 4904 (1989): 515. http://dx.doi.org/10.1126/science.244.4904.515.a.

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Olmschenk, Greg, David P. Bennett, Ian A. Bond, et al. "MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert." Astronomical Journal 165, no. 4 (2023): 175. http://dx.doi.org/10.3847/1538-3881/acbcc8.

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Abstract We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio q = 3.17 − 0.26 + 0.28 × 10 − 4 , the planet lies near the peak of the mass-ratio function derived by the MOA collaboration and near the edge of expected sample sensitivity. For these estimates we provide results using two mass-law priors: one assuming that all stars have an equal planet-hosting probability, and the other assuming that planets are more likely to orbit around more massiv

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Khmelnik, Solomon. "Hexagonal Storm on Saturn." Papers of Independent Authors 43 (July 6, 2018): 111–26. https://doi.org/10.5281/zenodo.1306963.

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At the north pole of Saturn has more than 30 years there is a giant storm in the shape of a hexagon, each side of which is greater than the diameter of Earth. This hexagon does not move on the planet, rotates and maintains its shape. This phenomenon still has no explanation. The following is a mathematical model of such a storm similar to the mathematical model of an ocean whirlpool (proposed earlier by the author). Also in the article shows that the energy source, that allows the storm to spin for a long time, is the gravitational field of Saturn.

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Hill, Michelle L., Stephen R. Kane, Paul A. Dalba, et al. "The TESS–Keck Survey. XIX. A Warm Transiting Sub-Saturn-mass Planet and a Nontransiting Saturn-mass Planet Orbiting a Solar Analog." Astronomical Journal 167, no. 4 (2024): 151. http://dx.doi.org/10.3847/1538-3881/ad2765.

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Abstract The Transiting Exoplanet Survey Satellite (TESS) continues to increase dramatically the number of known transiting exoplanets, and is optimal for monitoring bright stars amenable to radial velocity (RV) and atmospheric follow-up observations. TOI-1386 is a solar-type (G5V) star that was detected via TESS photometry to exhibit transit signatures in three sectors with a period of 25.84 days. We conducted follow-up RV observations using Keck/High Resolution Echelle Spectrometer (HIRES) as part of the TESS–Keck Survey, collecting 64 RV measurements of TOI-1386 with the HIRES spectrograph

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Fischer, Debra A., R. Paul Butler, Geoffrey W. Marcy, Steven S. Vogt, and Gregory W. Henry. "A Sub‐Saturn Mass Planet Orbiting HD 3651." Astrophysical Journal 590, no. 2 (2003): 1081–87. http://dx.doi.org/10.1086/375027.

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Agiwal, Omakshi, Hao Cao, Hsiang-Wen Hsu, et al. "Current Events at Saturn: Ring–Planet Electromagnetic Coupling." Planetary Science Journal 5, no. 6 (2024): 134. http://dx.doi.org/10.3847/psj/ad4343.

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Abstract This study presents a synthesized analysis of in situ and ground-based observations to investigate electromagnetic coupling between Saturn and its rings. During the Cassini Grand Finale, the magnetometer detected gradients in the azimuthal magnetic field B ϕ connected to Saturn’s B-ring on 17 out of 21 orbits. The B ϕ gradients indicate that field-aligned currents are flowing into Saturn’s B-ring at ∼1.55–1.67 R S in the ring plane, preferentially in the southern hemisphere. On average, these currents are magnetically conjugate with ground-based observations of nonsolar enhancements i

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Sheppard, Scott S., David J. Tholen, Mike Alexandersen, and Chadwick A. Trujillo. "New Jupiter and Saturn Satellites Reveal New Moon Dynamical Families." Research Notes of the AAS 7, no. 5 (2023): 100. http://dx.doi.org/10.3847/2515-5172/acd766.

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Abstract Tens of new moons around both Jupiter and Saturn have been announced on Minor Planet Electronic Circulars (MPECs) in late 2022 and early 2023. Jupiter now has 95 and Saturn 146 confirmed moons. Many smaller and fainter moons have also been detected at these planets but not yet confirmed through MPECs. These discoveries nearly complete the small moon population of Jupiter to about 2 km and Saturn to about 3 km and show new dynamical satellite families. The once lone Carpo is now joined by S/2018 J4, making it a group of two small prograde moons around Jupiter. The Inuit prograde family

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Sedaghati, E., A. Sánchez-López, S. Czesla, et al. "Moderately misaligned orbit of the warm sub-Saturn HD 332231 b." Astronomy & Astrophysics 659 (March 2022): A44. http://dx.doi.org/10.1051/0004-6361/202142471.

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Measurements of exoplanetary orbital obliquity angles for different classes of planets are an essential tool in testing various planet formation theories. Measurements for those transiting planets on relatively large orbital periods (P > 10 d) present a rather difficult observational challenge. Here we present the obliquity measurement for the warm sub-Saturn planet HD 332231 b, which was discovered through Transiting Exoplanet Survey Satellite photometry of sectors 14 and 15, on a relatively large orbital period (18.7 d). Through a joint analysis of previously obtained spectroscopic data a

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Han, Cheongho, In-Gu Shin, Youn Kil Jung, et al. "KMT-2018-BLG-0748Lb: sub-Saturn microlensing planet orbiting an ultracool host." Astronomy & Astrophysics 641 (September 2020): A105. http://dx.doi.org/10.1051/0004-6361/202038173.

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Aims. We announce the discovery of a microlensing planetary system, in which a sub-Saturn planet is orbiting an ultracool dwarf host. Methods. We detected the planetary system by analyzing the short-timescale (tE ~ 4.4 days) lensing event KMT-2018-BLG-0748. The central part of the light curve exhibits asymmetry due to negative deviations in the rising side and positive deviations in the falling side. Results. We find that the deviations are explained by a binary-lens model with a mass ratio between the lens components of q ~ 2 × 10−3. The short event timescale, together with the small angular

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Oberst, J., H. Hussmann, B. Giese, et al. "ENCELADUS GEODETIC FRAMEWORK." ISPRS - International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences XLII-3/W1 (July 25, 2017): 113–18. http://dx.doi.org/10.5194/isprs-archives-xlii-3-w1-113-2017.

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The small (approximately 500 km in diameter) satellite Enceladus is moving near the equatorial plane and deep in the gravity field of its parent planet Saturn. Owing to tidal interaction with its parent, Enceladus has adopted a pronounced 3-axial ellipsoidal shape and is tidally locked, with rotational and orbital periods of about 1.37 days. As the equator of Saturn is inclined to the planet’s orbital plane, Enceladus, like most of the other satellites of Saturn, undergoes pronounced seasons. This paper gives a summary of the current status as well as shortcomings of our current knowledge rega

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P., Chinnadurai* &. Dr. N. G. Kumaran**. "MARRIAGE LIFE THROUGH "BHRIGU NANDI NADI"." International Journal of Computational Research and Development (IJCRD) 8, no. 1 (2023): 4–7. https://doi.org/10.5281/zenodo.7509169.

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In this article, it is to learn about the “Marriage Confirmation by Bhrigu Nandi Nadi” method. Whether a person will get married or not can be answered very simply in this method.  In this method, only four planets are taken into account to check the marriage confirmation of a person. Jupiter: Jupiter is the life governing planet for Male so Jupiter is taken as Lagna for Male. Venus: Venus is the life governing planet for Female.So, Venus is taken as Lagna for Female and In male horoscope Venus should be taken as wife Saturn: Saturnis a Karmic (Karaka of karmic) planet for bot

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Zhang, Hui, and Ji-Lin Zhou. "Runaway migration in a multiple-protoplanet system." Proceedings of the International Astronomical Union 3, S249 (2007): 413–18. http://dx.doi.org/10.1017/s174392130801692x.

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AbstractWe investigate the migration of two giant planets embedded in a proto-stellar disk. The inner planet(initially located at R10=1) is of 1 Jupiter mass and the outer one(R20=1.5) is of 1 Saturn mass. We find that due to the existence of the inner massive planet, the outer planet can not open a clear gap. Instead of an inward migration and being captured by the mean motion resonance of the inner planet, the outer planet undergoes an outward runaway migration. We conclude that this runaway migration is caused by the co-rotation torque in the co-orbital region of the outer planet and sustai

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Peluso, Daniel O’Conner, Paul A. Dalba, Duncan Wright, et al. "Confirming the Warm and Dense Sub-Saturn TIC 139270665 b with the Automated Planet Finder and Unistellar Citizen Science Network." Astronomical Journal 167, no. 4 (2024): 170. http://dx.doi.org/10.3847/1538-3881/ad2772.

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Abstract We report the discovery and confirmation of the Transiting Exoplanet Survey Satellite (TESS) single-transit, warm and dense sub-Saturn, TIC 139270665 b. This planet is unusually dense for its size: with a bulk density of 2.13 g cm−3 (0.645R J , 0.463M J ), it is the densest warm sub-Saturn of the TESS family. It orbits a metal-rich G2 star. We also found evidence of a second planet, TIC 139270665 c, with a longer period of 1010 − 220 + 780 days and minimum mass M P sin i of 4.89 − 0.37 + 0.66 M J . First clues of TIC 139270665 b’s existence were found by citizen scientists inspecting

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Boss, Alan P. "Modes of Gaseous Planet Formation." Symposium - International Astronomical Union 202 (2004): 141–48. http://dx.doi.org/10.1017/s0074180900217725.

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The discovery of gas giant planets around nearby stars has launched a new era in our understanding of the formation and evolution of planetary systems. However, none of the over four dozen companions detected to date strongly resembles Jupiter or Saturn: their inferred masses range from sub-Saturn-mass to 10 Jupiter-masses or more, while their orbits extend from periods of a few days to a few years. Given this situation, it seems prudent to re-examine mechanisms for gas giant planet formation. The two extreme cases are top-down or bottom-up. The latter is the core accretion mechanism, long fav

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Rodríguez Martínez, Romy, Jason D. Eastman, Karen A. Collins, et al. "Discovery and Characterization of an Eccentric, Warm Saturn Transiting the Solar Analog TOI-4994*." Astronomical Journal 169, no. 2 (2025): 72. https://doi.org/10.3847/1538-3881/ad9b90.

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Abstract We present the detection and characterization of TOI-4994b (TIC 277128619b), a warm Saturn-sized planet discovered by the NASA Transiting Exoplanet Survey Satellite. TOI-4994b transits a G-type star (V = 12.6 mag) with a mass, radius, and effective temperature of M ⋆ = 1.00 5 − 0.061 + 0.064 M ⊙ , R ⋆ = 1.05 5 − 0.037 + 0.040 R ⊙ , and T eff = 5640 ± 110 K. We obtained follow-up ground-based photometry from the Las Cumbres Observatory and the Antarctic Search for Transiting ExoPlanets telescopes, and we confirmed the planetary nature of TOI-4994b with multiple radial velocity observat

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Ga, Dheebakaran, Kokilavani S, Santosh Ganapati Patil, et al. "Planet activeness: a new concept to enhance the accuracy of Astromet weather forecast." F1000Research 13 (July 5, 2024): 746. http://dx.doi.org/10.12688/f1000research.149941.1.

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Background Astrometeorology is an ancient science, that deals the relationship between planet position and weather events. Several Indian studies proved that Astrometeorology could be a complementary method to improve numerical weather forecast accuracy. Since 2011, Tamil Nadu Agricultural University is conducting astrometeorological research and devised a novel concept “Planet Activeness Chart”. The principle is that “planets’ influence on a location’s weather varies throughout the day and may be negative, inactive, active, highly active and rule depending on their angle to that location”. Mo

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Hixenbaugh, Kyle, Xian-Yu Wang, Malena Rice, and Songhu Wang. "The Spin–Orbit Misalignment of TOI-1842b: The First Measurement of the Rossiter–McLaughlin Effect for a Warm Sub-Saturn around a Massive Star." Astrophysical Journal Letters 949, no. 2 (2023): L35. http://dx.doi.org/10.3847/2041-8213/acd6f5.

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Abstract The mechanisms responsible for generating spin–orbit misalignments in exoplanetary systems are still not fully understood. It is unclear whether these misalignments are related to the migration of hot Jupiters or are a consequence of general star and planet formation processes. One promising method to address this question is to constrain the distribution of spin–orbit angle measurements for a broader range of planets beyond hot Jupiters. In this work, we present the sky-projected obliquity ( λ = − 68 .° 1 − 14.7 + 21.2 ) for the warm sub-Saturn TOI-1842b, obtained through a measureme

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Clurman, Dan. "Scientists Discover That Saturn Is Actually a Bisexual Planet." Journal of Bisexuality 6, no. 4 (2007): 85. http://dx.doi.org/10.1300/j159v06n04_07.

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Lee, Jae Woo, Jae-Hyuck Youn, Seung-Lee Kim, Chung-Uk Lee, and Tobias Cornelius Hinse. "THE SUB-SATURN MASS TRANSITING PLANET HAT-P-12b." Astronomical Journal 143, no. 4 (2012): 95. http://dx.doi.org/10.1088/0004-6256/143/4/95.

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Miyake, N., T. Sumi, Subo Dong, et al. "A SUB-SATURN MASS PLANET, MOA-2009-BLG-319Lb." Astrophysical Journal 728, no. 2 (2011): 120. http://dx.doi.org/10.1088/0004-637x/728/2/120.

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Tripathi, A. K., R. P. Singhal, and K. P. Singh. "Pitch-angle diffusion coefficients from resonant interactions with electrostatic electron cyclotron harmonic waves in planetary magnetospheres." Annales Geophysicae 29, no. 2 (2011): 321–30. http://dx.doi.org/10.5194/angeo-29-321-2011.

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Abstract. Pitch-angle diffusion coefficients have been calculated for resonant interaction with electrostatic electron cyclotron harmonic (ECH) waves in the magnetospheres of Earth, Jupiter, Saturn, Uranus and Neptune. Calculations have been performed at two radial distances of each planet. It is found that observed wave electric field amplitudes in the magnetospheres of Earth and Jupiter are sufficient to put electrons on strong diffusion in the energy range of less than 100 eV. However, for Saturn, Uranus and Neptune, the observed ECH wave amplitude are insufficient to put electrons on stron

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Liu, Junjun, and Tapio Schneider. "Scaling of Off-Equatorial Jets in Giant Planet Atmospheres." Journal of the Atmospheric Sciences 72, no. 1 (2015): 389–408. http://dx.doi.org/10.1175/jas-d-13-0391.1.

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Abstract In the off-equatorial region of Jupiter’s and Saturn’s atmospheres, baroclinic eddies transport angular momentum out of retrograde and into prograde jets. In a statistically steady state, this angular momentum transfer by eddies must be balanced by dissipation, likely produced by magnetohydrodynamic (MHD) drag in the planetary interior. This paper examines systematically how an idealized representation of this drag in a general circulation model (GCM) of the upper atmosphere of giant planets modifies jet characteristics, the angular momentum budget, and the energy budget. In the GCM,

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Aglyamov, Yury S., Jonathan Lunine, Sushil Atreya, et al. "Giant Planet Lightning in Nonideal Gases." Planetary Science Journal 4, no. 6 (2023): 111. http://dx.doi.org/10.3847/psj/acd750.

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Abstract Lightning has been directly observed or inferred on all giant planets, generally accepted to be occurring in their water clouds. However, much as Earth has both cloud–cloud and cloud–ground lightning, this does not mean all flashes occur in a narrow altitude range: on Jupiter, the Galileo spacecraft detected lightning flashes apparently below the cloud base, explicable as lightning due to precipitation, and the Juno SRU detected small flashes far above it, at pressures of only 1–2 bars. We use a computationally light 1D entraining plume model, incorporating particle growth and nonindu

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Kisseleva, T. P., V. V. Bobylev, N. M. Bronnikova, et al. "Pulkovo Programme for the Photographic Observations of Satellites of Planets." Symposium - International Astronomical Union 141 (1990): 73–74. http://dx.doi.org/10.1017/s007418090008623x.

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The satellites of Mars, the Galilean satellites of Jupiter and the first eight satellites of Saturn have been observed with the 26-inch refractor, the normal astrograph at Pulkovo and with the luni-planet telescope at the Ordubad station of the Pulkovo observatory since 1972.

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Shear, Eric M., and John E. Moores. "Saturn ice ring exploration network mission platform." International Journal of Space Science and Engineering 5, no. 1 (2018): 16. http://dx.doi.org/10.1504/ijspacese.2018.090547.

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Shear, Eric M., and John E. Moores. "Saturn ice ring exploration network mission platform." International Journal of Space Science and Engineering 5, no. 1 (2018): 16. http://dx.doi.org/10.1504/ijspacese.2018.10011643.

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Saunders, Nicholas, Samuel K. Grunblatt, Daniel Huber, et al. "TESS Giants Transiting Giants. VII. A Hot Saturn Orbiting an Oscillating Red Giant Star*." Astronomical Journal 169, no. 2 (2025): 75. https://doi.org/10.3847/1538-3881/ad9a87.

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Abstract We present the discovery of TOI-7041 b (TIC 201175570 b), a hot Saturn transiting a red giant star with measurable stellar oscillations. We observe solar-like oscillations in TOI-7041 with a frequency of maximum power of ν max = 218.50 ± 2.23 μHz and a large frequency separation of Δν = 16.5282 ± 0.0186 μHz. Our asteroseismic analysis indicates that TOI-7041 has a mass of 1.07 ± 0.05(stat) ± 0.02(sys) M ⊙ and a radius of 4.10 ± 0.06(stat) ± 0.05(sys) R ⊙, making it one of the largest stars around which a transiting planet has been discovered with the Transiting Exoplanet Survey Satell

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Tchernyi, Vladimir V., and Sergey V. Kapranov. "To the Problem of the Properties of Saturn's Rings’ Ice." Research Notes of the AAS 5, no. 10 (2021): 255. http://dx.doi.org/10.3847/2515-5172/ac348c.

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Abstract We are trying to determine the properties of the ice of the rings of Saturn based on the model of the origin of the rings, taking into account the magnetic field of the planet, as well as by choosing a suitable ice of the Earth.

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Brasser, R., and Man Hoi Lee. "TILTING SATURN WITHOUT TILTING JUPITER: CONSTRAINTS ON GIANT PLANET MIGRATION." Astronomical Journal 150, no. 5 (2015): 157. http://dx.doi.org/10.1088/0004-6256/150/5/157.

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Cloutier, Ryan, Daniel Tamayo, and Diana Valencia. "COULD JUPITER OR SATURN HAVE EJECTED A FIFTH GIANT PLANET?" Astrophysical Journal 813, no. 1 (2015): 8. http://dx.doi.org/10.1088/0004-637x/813/1/8.

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