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Zharkov, V. N., und T. V. Gudkova. „Comparative planetology in IPE RAS“. Физика Земли, Nr. 1 (27.03.2019): 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, und 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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Showstack, Randy. „Sleuths break barrier in extrasolar planetology, finding two Saturn-sized planets“. Eos, Transactions American Geophysical Union 81, Nr. 15 (2000): 157. http://dx.doi.org/10.1029/00eo00107.
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Marov, M., und H. Rickman. „Interactions between Planets and Small Bodies: Introduction“. Highlights of Astronomy 11, Nr. 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 understanding of the importance of impact phenomena throughout the history of the Solar System and, therefore, the necessity to get more insight into the problem of interactions of planets and small bodies. This importance is clearly manifested by the observed cratering records of planetary surfaces and such dramatic events as the explosions of the comet P/Shoemaker-Levy 9 fragments in Jupiter’s atmosphere in 1994, that of the Tunguska object over Siberia in 1908, and the Chicxulub event dating back to the end of the Cretaceous.
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Cloutier, R., N. Astudillo-Defru, X. Bonfils, J. S. Jenkins, Z. Berdiñas, G. Ricker, R. Vanderspek 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 dynamical simulations to provide strong constraints on the planets’ orbital eccentricities by requiring long-term stability. Results. We measure the planet masses of the two outermost planets to be 2.42 ± 0.35 and 2.31 ± 0.46 Earth masses, which confirms the bulk terrestrial composition of the former and eludes to a significant radius fraction in an extended gaseous envelope for the latter. We are able to place an upper limit on the mass of the smallest, innermost planet of <1.01 Earth masses with 95% confidence. Our RV plus dynamical stability analysis places strong constraints on the orbital eccentricities and reveals that each planet’s orbit likely has e < 0.1. Conclusions. L 98-59 is likely a compact system of two rocky planets plus a third outer planet with a lower bulk density possibly indicative of the planet having retained a modest atmosphere. The system offers a unique laboratory for studies of planet formation, dynamical stability, and comparative atmospheric planetology as the two outer planets are attractive targets for atmospheric characterization through transmission spectroscopy. Continued RV monitoring will help refine the characterization of the innermost planet and potentially reveal additional planets in the system at wider separations.
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Tinetti, Giovanna, James Y.-K. Cho, Caitlin A. Griffith, Olivier Grasset, Lee Grenfell, Tristan Guillot, Tommi T. Koskinen et al. „The science of EChO“. Proceedings of the International Astronomical Union 6, S276 (Oktober 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 of new planets around stars within 200 parsecs of the Sun. The key challenge now is moving on from discovery, important though that remains, to characterisation: what are these planets actually like, and why are they as they are?In the past ten years, we have learned how to obtain the first spectra of exoplanets using transit transmission and emission spectroscopy. With the high stability of Spitzer, Hubble, and large ground-based telescopes the spectra of bright close-in massive planets can be obtained and species like water vapour, methane, carbon monoxide and dioxide have been detected. With transit science came the first tangible remote sensing of these planetary bodies and so one can start to extrapolate from what has been learnt from Solar System probes to what one might plan to learn about their faraway siblings. As we learn more about the atmospheres, surfaces and near-surfaces of these remote bodies, we will begin to build up a clearer picture of their construction, history and suitability for life.The Exoplanet Characterisation Observatory, EChO, will be the first dedicated mission to investigate the physics and chemistry of Exoplanetary Atmospheres. By characterising spectroscopically more bodies in different environments we will take detailed planetology out of the Solar System and into the Galaxy as a whole.EChO has now been selected by the European Space Agency to be assessed as one of four M3 mission candidates.
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Latour, Bruno, und Dipesh Chakrabarty. „Conflicts of Planetary Proportion – A Conversation“. Journal of the Philosophy of History 14, Nr. 3 (19.11.2020): 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 “planets” whose attractions are simultaneously being felt today on any political question. Each of his eight planets are defined by the disconnect between where they are situated and where they are imagined to be moving, which means that each planet is led by a different and incommensurable philosophy of history. Such a “fictional planetology” is then discussed by Chakrabarty, who reviews the difficulties historians have had in taking the nonhuman (and hence the planet) as a historical agent and then adds to Latour’s count a new planetary body which further complicates the geopolitical situation. The result of their joint effort is to shift questions of philosophy of history to philosophy of geography.
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Eisner, N. L., B. A. Nicholson, O. Barragán, S. Aigrain, C. Lintott, L. Kaye, B. Klein et al. „Planet Hunters TESS III: two transiting planets around the bright G dwarf HD 152843“. Monthly Notices of the Royal Astronomical Society 505, Nr. 2 (12.05.2021): 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 of $5.83 _{ - 0.14 } ^ { + 0.14 }$ R⊕ for the outer planet, which was only seen to transit once. Each signal was independently statistically validated, taking into consideration the TESS light curve as well as the ground-based spectroscopic follow-up observations. Radial velocities from HARPS-N and EXPRES yield a tentative detection of planet b, whose mass we estimate to be $11.56 _{ - 6.14 } ^ { + 6.58 }$ M⊕, and allow us to place an upper limit of 27.5 M⊕ (99 per cent confidence) on the mass of planet c. Due to the brightness of the host star and the strong likelihood of an extended H/He atmosphere on both planets, this system offers excellent prospects for atmospheric characterization and comparative planetology.
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Hunt, G., A. Brahic, D. Morrison, J. L. Bertaux, J. Burns, Chen Dahoan, D. Cruikshank et al. „Commission 16: Physical Study of Planets and Satellites (Etude Physique Pes Planetes Et Satellites)“. Transactions of the International Astronomical Union 20, Nr. 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 results are at the boundary of those of other commissions such as the 15, 20, 7, 19, 33, 40, 44, 49 and 51 ones. The study of the main results obtained during this last triennum shows a perfect complementarity between space and ground-based observations. It should be arbitrary to separate space and ground-based scientists. The have the same goal and they study the same objects. Quite often, the same individuals use both techniques, depending on the most efficient one for the problem under study. It is remarkable to see that space data collected more than ten years ago are still analysed in connection with ground-based observations. The same remarks can apply for ground-based data. In addition to that, new theoretical models, new numerical simulations and new laboratory experiments have ben recently developed. They all contribute to a better understanding of planets and satellites physics.
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Breuer, Doris. „Early planetary atmospheres and surfaces: Origin of the Earth’s water, crust and atmosphere“. Proceedings of the International Astronomical Union 14, S345 (August 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 during magma ocean solidification will then lead to a significant volatile loss of the interior and to the formation of a dense atmosphere during the early stages of planetary evolution. These processes are also responsible for the oxidation state of this early atmosphere, i.e. whether it was more reduced or oxidized. Although this early volatile loss was very efficient, the interior probably retained some water. This was distributed in the subsequent evolution between interior and atmosphere, as well as on the surface as liquid water in case of favorable temperature and pressure conditions. The main processes responsible for the water distribution are volcanic outgassing driven by partial melting of the silicate mantle and formation of the crust and recycling of water-rich crustal material. Here, an important difference between the terrestrial planets is the tectonic style prevailing on the planet. For the Earth with its plate tectonics, recycling of water is very efficient and can even balance the outgassing. For terrestrial planets in the stagnant lid regime of mantle convection such as Mars, the exchange of water between the interior and the surface/atmosphere is mainly in one direction and results in a continuous depletion of the interior. In this talk, I will briefly review our current knowledge on these interactions between interior and atmosphere and on the problem we are facing to better understand the influence of the interior on the habitability of a planet.
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Palle, E., G. Nowak, R. Luque, D. Hidalgo, O. Barragán, J. Prieto-Arranz, T. Hirano et al. „Detection and Doppler monitoring of K2-285 (EPIC 246471491), a system of four transiting planets smaller than Neptune“. Astronomy & Astrophysics 623 (März 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. Among many other K2 candidates, we discovered a multi-planetary system around EPIC 246471491, referred to henceforth as K2-285, which contains four planets, ranging in size from twice the size of Earth to nearly the size of Neptune. We aim here at confirming their planetary nature and characterizing the properties of this system. Methods. We measure the mass of the planets of the K2-285 system by means of precise radial-velocity measurements using the CARMENES spectrograph and the HARPS-N spectrograph. Results. With our data we are able to determine the mass of the two inner planets of the system with a precision better than 15%, and place upper limits on the masses of the two outer planets. Conclusions. We find that K2-285b has a mass of Mb = 9.68−1.37+1.21 M⊕ and a radius of Rb = 2.59−0.06+0.06 R⊕, yielding a mean density of ρb = 3.07−0.45+0.45 g cm−3, while K2-285c has a mass of Mc = 15.68−2.13+2.28 M⊕, radius of Rc = 3.53−0.08+0.08 R⊕, and a mean density of ρc = 1.95−0.28+0.32 g cm−3. For K2-285d (Rd = 2.48−0.06+0.06 R⊕) and K2-285e (Re = 1.95−0.05+0.05 R⊕), the upper limits for the masses are 6.5 M⊕ and 10.7 M⊕, respectively. The system is thus composed of an (almost) Neptune-twin planet (in mass and radius), two sub-Neptunes with very different densities and presumably bulk composition, and a fourth planet in the outermost orbit that resides right in the middle of the super-Earth/sub-Neptune radius gap. Future comparative planetology studies of this system would provide useful insights into planetary formation, and also a good test of atmospheric escape and evolution theories.
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Marov, Mikhail Ya. „Missions to Mars: an Overview and a Perspective at the Turn of the Century“. International Astronomical Union Colloquium 161 (Januar 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 conditions on the two planets during the early phase of Solar system evolution. Mars has been central to the space programs of the former USSR and USA since the beginning of the space age, the most successful being the two Viking mission in 1976. These robotic missions, representing a period of baseline data collection, significantly expanded our knowledge but also gave rise to many new important questions. Dramatic shortfalls in the funding of space programs changed a short period of excitement culminating in the proclaimed human mission to Mars when the Cold War was over. A new strategy for planetary exploration (the «faster-cheaper-better» concept) tends to modify the former programs significantly. This new strategy at the turn of the century which, projected into the new millenium, strictly confines the targets in the Solar system and specifically Mars exploration. Nonetheless, it represents a challenge for the launch of capable small missions with significant scientific returns. Human flight and Mars settlement, while being considered as a milestone in the history of humankind and a multifaced endeavour, would require, however, a great investment of international resources.
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De Vet, S. J., und W. Van Westrenen. „Introduction: Planetary geosciences, the Dutch contribution to the exploration of our solar system“. Netherlands Journal of Geosciences - Geologie en Mijnbouw 95, Nr. 2 (28.03.2016): 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 christened the Hourglass Sea, suggesting it to be an area of open water. Perhaps the landscape surrounding him in the Netherlands prompted Huygens to interpret the newly discovered feature as a wet area on the planet's surface. The attribution of traits to an albedo feature on another planet based on terrestrial landscapes may well be considered as the first-ever attempt at ‘comparative planetology’. The albedo feature can still be recognised at the surface of Mars today as Syrtis Major. Any modest amateur telescope can provide a view superior to that of Huygens’, allowing the observation of the very first geological feature ever identified on another rocky planet.
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Paty, Carol, Chris S. Arridge, Ian J. Cohen, Gina A. DiBraccio, Robert W. Ebert und Abigail M. Rymer. „Ice giant magnetospheres“. Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 378, Nr. 2187 (09.11.2020): 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 obliquity of each planet (especially Uranus). With in situ observations at Uranus and Neptune limited to a single encounter by the Voyager 2 spacecraft, a growing number of analytical and numerical models have been put forward to characterize these unique magnetospheres and test hypotheses related to the magnetic structures and the distribution of plasma observed. Yet many questions regarding magnetospheric structure and dynamics, magnetospheric coupling to the ionosphere and atmosphere, and potential interactions with orbiting satellites remain unanswered. Continuing to study and explore ice giant magnetospheres is important for comparative planetology as they represent critical benchmarks on a broad spectrum of planetary magnetospheric interactions, and provide insight beyond the scope of our own Solar System with implications for exoplanet magnetospheres and magnetic reversals. This article is part of a discussion meeting issue ‘Future exploration of ice giant systems'.
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Koutnik, Michelle R., und 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, Nr. 2 (17.02.2021): 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 distribution of lobate debris aprons and glacier-like forms, in particular, is critical to constraining past climate conditions when such features were active, reconstructing past ice extent, and estimating the total inventory of buried ice remaining in the mid-latitudes of Mars. This review spans a range of knowledge about debris-covered glaciers on Earth, in order to add context to investigations of dust and debris-covered ice on Mars and to put research on both planets in a perspective aimed at maximizing process-based understanding of glacier evolution. The state of knowledge and some gaps in knowledge on Mars are discussed in relation to possible avenues for future research in how landforms are classified, advances in comparative planetology, and new understanding from future missions. While this review is focused primarily on processes controlling active debris-covered glaciers, a key to understanding glacier change through time is to consider individual landforms in context with the full-system environment in which they are found. For Earth, this includes understanding local and regional controls on current glacier change, and how these processes relate to landform development in the past as well as what may develop in the future. For Mars, this includes evaluating how present-day landforms elucidate past ice activity and environmental conditions during epochs when orbital parameters, climate, and water ice distribution were substantially different.
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Runyon, Kirby, Caitlin Joannah Ahrens, Chloe B. Beddingfield, Joshua T. S. Cahill, Richard Cartwright, Ian Cohen, Bryan Holler et al. „Comparative Planetology of Kuiper Belt Dwarf Planets Enabled by the Near-Term Interstellar Probe“. Bulletin of the AAS 53, Nr. 4 (18.03.2021). http://dx.doi.org/10.3847/25c2cfeb.4873908b.
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