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Journal articles on the topic 'Planetology of uid planets'

Author: Grafiati

Published: 17 September 2021

Last updated: 30 July 2025

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1

Zharkov, V. N., and T. V. Gudkova. "Comparative planetology in IPE RAS." Физика Земли, no. 1 (March 27, 2019): 61–77. http://dx.doi.org/10.31857/s0002-33372019161-77.

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The review of the studies on comparative planetology carried out in the Schmidt Institute of Physics of the Earth of the Russian Academy of Sciences is presented. The obtained results are described in accordance with the study objects: the Moon, terrestrial planets, Venus and Mars, Phobos and Deimos-moons of Mars, giant planets and their moons.

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Chakrabarti, Supriya, and G. Randall Gladstone. "EUV Studies of Solar System Objects: A Status Report." International Astronomical Union Colloquium 152 (1996): 449–56. http://dx.doi.org/10.1017/s025292110003637x.

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EUV studies have contributed substantially to our understanding of the physical and chemical properties the Sun, planets, and their satellites. Although the spectroscopic data set is limited to Venera 11/12, Voyager 1/2, Astro 1/2, EUVE, Galileo, and a handful of sounding rocket experiments, these data have provided important insights regarding the atmospheres and surfaces of several planets and satellites to the point where rudimentary comparative planetology can be conducted. In this paper we highlight some of these results.

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3

Kunimoto, Michelle, Zifan Lin, Sarah Millholland, et al. "Two Earth-size Planets and an Earth-size Candidate Transiting the nearby Star HD 101581*." Astronomical Journal 169, no. 1 (2024): 47. https://doi.org/10.3847/1538-3881/ad9266.

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Abstract We report the validation of multiple planets transiting the nearby (d = 12.8 pc) K5V dwarf HD 101581 (GJ 435, TOI–6276, TIC 397362481). This system consists of at least two Earth-size planets whose orbits are near a mutual 4:3 mean-motion resonance, HD 101581 b ( R p = 0.956 − 0.061 + 0.063 R ⊕ , P = 4.47 days) and HD 101581c ( R p = 0.990 − 0.070 + 0.070 R ⊕ , P = 6.21 days). Both planets were discovered in Sectors 63 and 64 TESS observations and statistically validated with supporting ground-based follow-up. We also identify a signal that probably originates from a third transiting

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Showstack, Randy. "Sleuths break barrier in extrasolar planetology, finding two Saturn-sized planets." Eos, Transactions American Geophysical Union 81, no. 15 (2000): 157. http://dx.doi.org/10.1029/00eo00107.

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5

Marov, M., and H. Rickman. "Interactions between Planets and Small Bodies: Introduction." Highlights of Astronomy 11, no. 1 (1998): 220–22. http://dx.doi.org/10.1017/s153929960002061x.

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The exploration of our Solar System is rapidly growing in importance as a scientific discipline. During the last decades, great progress has been achieved as the result of space missions to planets and small bodies and improved remote-sensing methods, as well as due to refined techniques of laboratory measurements and a rapid progress in theoretical studies, involving the development of various astrophysical and geophysical evolutionary models, based in particular on the approach of comparative planetology. In the crossroads of astronomy and geophysics, recent years have seen a growing underst

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6

Marcelin, Michel, Isabelle Boisse, Marc Ferrari, Guillaume Hebrard, and Emmanuel Hugot. "The first detection of an exoplanet that opened a new field in planetology." Photoniques, no. 119 (2023): 36–40. http://dx.doi.org/10.1051/photon/202311936.

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Periodic Radial Velocity oscillations of the star 51 Pegasi measured at OHP (Observatoire de Haute-Provence) in 1995 revealed a planet orbiting around it. This first detection of an exoplanet had been expected for a long time, since everyone was convinced that most of the stars were surrounded by planets. This success, leading to the Nobel Prize of physics in 2019, is the result of the evolution of technics for the measurement of radial velocities of stars during half a century at OHP.

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PLANCHON, Olivier. "Climatologie comparée des planètes : un bref état des connaissances." Climatologie 14 (January 23, 2018): 18–47. https://doi.org/10.4267/climatologie.1255.

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The main parameters allowing to characterize and compare the climatic features over the terrestrial planets of the Solar System are developed according to the distance from the host star; the existence of an atmosphere, its composition and motion; and the orbital parameters allowing to identify seasonal more or less contrasted oscillations (obliquity and eccentricity). The comparative climatology of the Solar System planets shows some common features subjected to many changes depending on different parameters of every planet. Like this, the rotation period (day/night duration), the obliquity a

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8

Cloutier, R., N. Astudillo-Defru, X. Bonfils, et al. "Characterization of the L 98-59 multi-planetary system with HARPS." Astronomy & Astrophysics 629 (September 2019): A111. http://dx.doi.org/10.1051/0004-6361/201935957.

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Aims. L 98-59 (TIC 307210830, TOI-175) is a nearby M3 dwarf around which TESS revealed three small transiting planets (0.80, 1.35, 1.57 Earth radii) in a compact configuration with orbital periods shorter than 7.5 days. Here we aim to measure the masses of the known transiting planets in this system using precise radial velocity (RV) measurements taken with the HARPS spectrograph. Methods. We considered both trained and untrained Gaussian process regression models of stellar activity, which are modeled simultaneously with the planetary signals. Our RV analysis was then supplemented with dynami

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9

Edwards, Billy, and Giovanna Tinetti. "The Ariel Target List: The Impact of TESS and the Potential for Characterizing Multiple Planets within a System." Astronomical Journal 164, no. 1 (2022): 15. http://dx.doi.org/10.3847/1538-3881/ac6bf9.

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Abstract The ESA Ariel mission has been adopted for launch in 2029 and will conduct a survey of around 1000 exoplanetary atmospheres during its primary mission life. By providing homogeneous data sets with a high signal-to-noise ratio and wide wavelength coverage, Ariel will unveil the atmospheric demographics of these faraway worlds, helping to constrain planet formation and evolution processes on a galactic scale. Ariel seeks to undertake a statistical survey of a diverse population of planets; therefore, the sample of planets from which this selection can be made is of the utmost importance

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10

Tinetti, Giovanna, James Y.-K. Cho, Caitlin A. Griffith, et al. "The science of EChO." Proceedings of the International Astronomical Union 6, S276 (2010): 359–70. http://dx.doi.org/10.1017/s1743921311020448.

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AbstractThe science of extra-solar planets is one of the most rapidly changing areas of astrophysics and since 1995 the number of planets known has increased by almost two orders of magnitude. A combination of ground-based surveys and dedicated space missions has resulted in 560-plus planets being detected, and over 1200 that await confirmation. NASA's Kepler mission has opened up the possibility of discovering Earth-like planets in the habitable zone around some of the 100,000 stars it is surveying during its 3 to 4-year lifetime. The new ESA's Gaia mission is expected to discover thousands o

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11

Latour, Bruno, and Dipesh Chakrabarty. "Conflicts of Planetary Proportion – A Conversation." Journal of the Philosophy of History 14, no. 3 (2020): 419–54. http://dx.doi.org/10.1163/18722636-12341450.

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Abstract The introduction of the long-term history of the Earth into the preoccupations of historians has triggered a crisis because it has become impossible to keep the “planet” as one single entity outside of history properly understood. As soon as the planetary intruded into history, it became impossible to keep it as one naturalized background. By problematizing the planetary, Dipesh Chakrabarty has forced philosophers, historians and anthropologists to extend pluralism to the very ground on which history was supposed to unfold. Hence Bruno Latour’s attempt at counting the number of “plane

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12

Beltz, Hayley, and Emily Rauscher. "Comparative Planetology of Magnetic Effects in Ultrahot Jupiters: Trends in High-resolution Spectroscopy." Astrophysical Journal 976, no. 1 (2024): 32. http://dx.doi.org/10.3847/1538-4357/ad7ded.

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Abstract Ultrahot Jupiters (UHJs), being the hottest class of exoplanets known, provide a unique laboratory for testing atmospheric interactions with internal planetary magnetic fields at a large range of temperatures. Thermal ionization of atmospheric species on the dayside of these planets results in charged particles becoming embedded in the planet’s mostly neutral wind. The charges will resist flow across magnetic field lines as they are dragged around the planet and ultimately alter the circulation pattern of the atmosphere. We model this process to study this effect on high-resolution em

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13

Eisner, N. L., B. A. Nicholson, O. Barragán, et al. "Planet Hunters TESS III: two transiting planets around the bright G dwarf HD 152843." Monthly Notices of the Royal Astronomical Society 505, no. 2 (2021): 1827–40. http://dx.doi.org/10.1093/mnras/stab1253.

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ABSTRACT We report on the discovery and validation of a two-planet system around a bright (V = 8.85 mag) early G dwarf (1.43 R⊙, 1.15 M⊙, TOI 2319) using data from NASA’s Transiting Exoplanet Survey Satellite (TESS). Three transit events from two planets were detected by citizen scientists in the month-long TESS light curve (sector 25), as part of the Planet Hunters TESS project. Modelling of the transits yields an orbital period of $11.6264 _{ - 0.0025 } ^ { + 0.0022 }$ d and radius of $3.41 _{ - 0.12 } ^ { + 0.14 }$ R⊕ for the inner planet, and a period in the range 19.26–35 d and a radius o

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14

Breuer, Doris. "Early planetary atmospheres and surfaces: Origin of the Earth’s water, crust and atmosphere." Proceedings of the International Astronomical Union 14, S345 (2018): 156–63. http://dx.doi.org/10.1017/s1743921319001807.

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AbstractThe origin of the planets atmosphere is a profound question of comparative planetology. There are two competing models, i.e. outgassing from the interior or late delivery from comets or volatiles-rich asteroids after most of the planet has been formed, of which the former is currently preferred. Meteorite compositions as well as radial mixing during accretion derived from accretion models suggest that the building blocks of the terrestrial planets contained some volatiles. Processes like dehydration by hydrous melting, oxidation, impact devolatilization, and in particular degassing dur

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15

Hunt, G., A. Brahic, D. Morrison, et al. "Commission 16: Physical Study of Planets and Satellites (Etude Physique Pes Planetes Et Satellites)." Transactions of the International Astronomical Union 20, no. 1 (1988): 167–78. http://dx.doi.org/10.1017/s0251107x00007112.

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The physical study of planets and satellites is probably one of the more active fields of research of the second half of this century. This is due to space exploration by spacecraft, but also to the use of modern detectors, of large ground-based telescopes, and of powerful computers by active researchers. Planetary research (or planetology) is a pluridisciplinary domain, which requires not only the competence of astronomers, but also of geophysicists, of mineralogists, of climatologists, of biologists, of chemists, of physicists, of “pure„ mathematicians, and many other scientists. Many result

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16

Edwards, Billy, Quentin Changeat, Angelos Tsiaras, et al. "Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets." Astrophysical Journal Supplement Series 269, no. 1 (2023): 31. http://dx.doi.org/10.3847/1538-4365/ac9f1a.

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Abstract We present analysis of the atmospheres of 70 gaseous extrasolar planets via transit spectroscopy with Hubble’s Wide Field Camera 3 (WFC3). For over half of these, we statistically detect spectral modulation that our retrievals attribute to molecular species. Among these, we use Bayesian hierarchical modeling to search for chemical trends with bulk parameters. We use the extracted water abundance to infer the atmospheric metallicity and compare it to the planet’s mass. We also run chemical equilibrium retrievals, fitting for the atmospheric metallicity directly. However, although previ

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17

Palle, E., G. Nowak, R. Luque, et al. "Detection and Doppler monitoring of K2-285 (EPIC 246471491), a system of four transiting planets smaller than Neptune." Astronomy & Astrophysics 623 (March 2019): A41. http://dx.doi.org/10.1051/0004-6361/201834001.

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Context. The Kepler extended mission, also known as K2, has provided the community with a wealth of planetary candidates that orbit stars typically much brighter than the targets of the original mission. These planet candidates are suitable for further spectroscopic follow-up and precise mass determinations, leading ultimately to the construction of empirical mass-radius diagrams. Particularly interesting is to constrain the properties of planets that are between Earth and Neptune in size, the most abundant type of planet orbiting Sun-like stars with periods of less than a few years. Aims. Amo

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18

Konstantinov, SI. "Quantum Theory of Gravity and Arthur Eddington's Fundamental Theory." Journal of Biomedical Research & Environmental Sciences 2, no. 11 (2021): 1092–100. https://doi.org/10.37871/jbres1353.

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For the fi rst time, the article presents the Quantum Theory of Gravity, covering not only the microcosm of elementary particles, but also the macrocosm of planets, stars and black holes. This relational approach to gravity was consistently presented in Arthur Eddington's monograph “Fundamental Theory”. In the theory of quantum gravity proposes to consider instead of gravity holes in the curved space-time of Einstein's general relativity, gravitational funnels formed by the rotation of planets, stars and galaxies in a dark matter halo. The change in the gravitational potent

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19

Marov, Mikhail Ya. "Missions to Mars: an Overview and a Perspective at the Turn of the Century." International Astronomical Union Colloquium 161 (January 1997): 253–65. http://dx.doi.org/10.1017/s0252921100014779.

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AbstractThe principal objectives of Mars exploration and their potential benefits involve many problems of scientific importance, technological developments and the general trend for future human settlements beyond the Earth. The comparative planetology approach emphasizes Mars and Venus as two extreme models of the climate evolution on the inner planets which are of great ecological importance. The climatic history of Mars is of particular interest because of the implications for life and global change on the Earth. The origin of life on the early Earth can also be related to the similar cond

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20

De Vet, S. J., and W. Van Westrenen. "Introduction: Planetary geosciences, the Dutch contribution to the exploration of our solar system." Netherlands Journal of Geosciences - Geologie en Mijnbouw 95, no. 2 (2016): 109–12. http://dx.doi.org/10.1017/njg.2016.8.

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Planetary geoscience was effectively born when Christiaan Huygens took his first look at planet Mars on Friday 28 November 1659. As one of the leading scientists of his time, Huygens was known for constructing his own telescopes to observe stars, planets and nebulae whenever the clear and spacious skies above the Netherlands allowed. Huygens observed the planet Mars during the heydays of its 1659 opposition. On the night of 28 November he succeeded in sketching the first albedo feature on a different planet in our solar system. The roughly triangular dark-coloured patch was originally christen

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21

Paty, Carol, Chris S. Arridge, Ian J. Cohen, Gina A. DiBraccio, Robert W. Ebert, and Abigail M. Rymer. "Ice giant magnetospheres." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 378, no. 2187 (2020): 20190480. http://dx.doi.org/10.1098/rsta.2019.0480.

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The ice giant planets provide some of the most interesting natural laboratories for studying the influence of large obliquities, rapid rotation, highly asymmetric magnetic fields and wide-ranging Alfvénic and sonic Mach numbers on magnetospheric processes. The geometries of the solar wind–magnetosphere interaction at the ice giants vary dramatically on diurnal timescales due to the large tilt of the magnetic axis relative to each planet's rotational axis and the apparent off-centred nature of the magnetic field. There is also a seasonal effect on this interaction geometry due to the large obli

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22

Koutnik, Michelle R., and Asmin V. Pathare. "Contextualizing lobate debris aprons and glacier-like forms on Mars with debris-covered glaciers on Earth." Progress in Physical Geography: Earth and Environment 45, no. 2 (2021): 130–86. http://dx.doi.org/10.1177/0309133320986902.

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Debris-covered glaciers from around the world offer distinct environmental, climatic, and historical conditions from which to study the effects of debris on glacier-ice evolution. A rich literature on debris-covered glaciers exists from decades of field work, laboratory studies, remote-sensing observations, and numerical modeling. In general, the base of knowledge established by studying periglacial, glacial, and paraglacial landforms on Earth has been applied to aid interpretation of ice-rich or ice-remnant landforms on Mars, but research has progressed on both planets. For Mars, the spatial

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23

Marov, M. Ya. "Exploration of the Moon by Automatic Spacecraft." Космические исследования 61, no. 1 (2023): 52–77. http://dx.doi.org/10.31857/s0023420623010041.

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Problems of the study and exploration of the Moon, which is of paramount interest for cosmogony, planetology, and Earth sciences in the context of a comprehensive study of the Solar System, are discussed. A historical review of lunar exploration is given, a fundamental contribution to which was made by the Soviet lunar program, carried out with the help of automatic spacecraft in the first decades of the space age. The review is timed to coincide with the revival of lunar exploration within the framework of the Russian national space program. The current state of knowledge about the Moon is co

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24

Runyon, Kirby, Caitlin Joannah Ahrens, Chloe B. Beddingfield, et al. "Comparative Planetology of Kuiper Belt Dwarf Planets Enabled by the Near-Term Interstellar Probe." Bulletin of the AAS 53, no. 4 (2021). http://dx.doi.org/10.3847/25c2cfeb.4873908b.

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25

Soderlund, Krista M., Sabine Stanley, Hao Cao, Michael A. Calkins, and Matthew K. Browning. "Puzzles in Planetary Dynamos: Implications for Planetary Interiors." Annual Review of Earth and Planetary Sciences, February 14, 2025. https://doi.org/10.1146/annurev-earth-111523-081635.

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Intrinsic magnetic fields were once commonplace across our Solar System, and many planetary bodies have sustained active dynamos to the present day. The nature and behavior of these dynamos vary widely, however, reflecting the diverse internal conditions of planets as summarized in this review. For the terrestrial planets, the existence of active dynamos and/or ancient remanent magnetization recorded in crustal rocks, or lack thereof, lead to questions about their timing and power sources. Paleomagnetic studies reveal that many small bodies in the Solar System exhibit remanent magnetization, o

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26

Yao, Zhonghua, Ruilong Guo, Yong Wei, et al. "Recent advances on the magnetic reconnection, dipolarization and auroral processes at giant planets from the perspective of comparative planetology." Earth and Planetary Physics, 2024, 0. http://dx.doi.org/10.26464/epp2024017.

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27

Luo, Yangcheng, Yongyun Hu, Jun Yang, Michael Zhang, and Yuk L. Yung. "Coupled atmospheric chemistry, radiation, and dynamics of an exoplanet generate self-sustained oscillations." Proceedings of the National Academy of Sciences 120, no. 51 (2023). http://dx.doi.org/10.1073/pnas.2309312120.

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Nonlinearity in photochemical systems is known to allow self-sustained oscillations, but they have received little attention in studies of planetary atmospheres. Here, we present a unique, self-oscillatory solution for ozone chemistry of an exoplanet from a numerical simulation using a fully coupled, three-dimensional (3D) atmospheric chemistry-radiation-dynamics model. Forced with nonvarying stellar insolation and emission flux of nitric oxide (NO), atmospheric ozone abundance oscillates by a factor of thirty over a multidecadal timescale. As such self-oscillations can only occur with biologi

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Davoult, Jeanne, Yann Alibert, and Lokesh Mishra. "Earth-like planets hosting systems: Architecture and properties." Astronomy & Astrophysics, August 2, 2024. http://dx.doi.org/10.1051/0004-6361/202449330.

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The discovery of Earth-like planets is a major focus of current planetology research and faces a significant technological challenge. Indeed, when it comes to detecting planets as small and cold as the Earth, the cost of observation time is massive. Understanding in what type of systems Earth-like planets (ELPs) form and how to identify them is crucial for preparing future missions such as PLATO, LIFE, or others. Theoretical models suggest that ELPs predominantly form within a certain type of system architecture. Therefore, the presence or absence of ELPs could be inferred from the arrangement

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29

Styczinski, M. J., S. D. Vance, and M. Melwani Daswani. "PlanetProfile: Self‐Consistent Interior Structure Modeling for Ocean Worlds and Rocky Dwarf Planets in Python." Earth and Space Science 10, no. 8 (2023). http://dx.doi.org/10.1029/2022ea002748.

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AbstractThe open‐source PlanetProfile framework was developed to investigate the interior structure of icy moons based on collectively matching their observed properties and comparative planetology. The software relates observed and measured properties, assumptions such as the type of materials present, and laboratory equation‐of‐state (EOS) data through geophysical and thermodynamic models to evaluate radial profiles of mechanical, thermodynamic, and electrical properties, as self‐consistently as possible. We have created a Python version of PlanetProfile. In the process, we have made optimiz

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