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Relevant bibliographies by topics / Planetology of uid planets

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Academic literature on the topic 'Planetology of uid planets'

Author: Grafiati

Published: 17 September 2021

Last updated: 6 February 2022

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Journal articles on the topic "Planetology of uid planets"

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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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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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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 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 (October 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, and Dipesh Chakrabarty. "Conflicts of Planetary Proportion – A Conversation." Journal of the Philosophy of History 14, no. 3 (November 19, 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, no. 2 (May 12, 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, 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 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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Dissertations / Theses on the topic "Planetology of uid planets"

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Bonsor, Amy Hannah Clay. "Post-main sequence evolution of planetary systems." Thesis, University of Cambridge, 2011. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.609856.

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Raymond, Sean Neylon. "Late-stage accretion and habitability of terrestrial planets /." Thesis, Connect to this title online; UW restricted, 2005. http://hdl.handle.net/1773/5438.

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Hodosán, Gabriella. "Lightning on exoplanets and brown dwarfs." Thesis, University of St Andrews, 2017. http://hdl.handle.net/10023/12079.

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Lightning is an important electrical phenomenon, known to exist in several Solar System planets. Amongst others, it carries information on convection and cloud formation, and may be important for pre-biotic chemistry. Exoplanets and brown dwarfs have been shown to host environments appropriate for the initiation of lightning discharges. In this PhD project, I aim to determine if lightning on exoplanets and brown dwarfs can be more energetic than it is known from Solar System planets, what are the most promising signatures to look for, and if these "exo-lightning" signatures can be detected from Earth. This thesis focuses on three major topics. First I discuss a lightning climatology study of Earth, Jupiter, Saturn, and Venus. I apply the obtained lightning statistics to extrasolar planets in order to give a first estimate on lightning occurrence on exoplanets and brown dwarfs. Next, I introduce a short study of potential lightning activity on the exoplanet HAT-P-11b, based on previous radio observations. Related to this, I discuss a first estimate of observability of lightning from close brown dwarfs, with the optical Danish Telescope. The final part of my project focuses on a lightning radio model, which is applied to study the energy and radio power released from lightning discharges in hot giant gas planetary and brown dwarf atmospheres. The released energy determines the observability of signatures, and the effect lightning has on the local atmosphere of the object. This work combines knowledge obtained from planetary and earth sciences and uses that to learn more about extrasolar systems. My main results show that lightning on exoplanets may be more energetic than in the Solar System, supporting the possibility of future observations and detection of lightning activity on an extrasolar body. My work provides the base for future radio, optical, and infrared search for "exo-lightning".

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

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La détection et la caractérisation d'exoplanètes apparaissent clairement comme des thèmes centraux de l'observation astronomique pour les années à venir. Les projets spatiaux ou au sol sont nombreux (HARPS, CoRoT, Kepler, JWST, SPHERE...), mais les études théoriques visant à l'analyse et à la compréhension des données recueillies et à venir sont nécessaires. Durant cette thèse j'ai étudié divers processus physiques affectant la structure interne et l'évolution des planètes géantes, aussi bien au sein, qu'à l'extérieur de notre système solaire. J'ai notamment modélisé en détail: -L'impact de l'irradiation intense émise par l'étoile sur l'atmosphère d'une planète à faible distance orbitale, et l'effet induit sur l'évolution interne de cette planète. -Le couplage par dissipation de marée de l'évolution orbitale et thermique d'une planète interagissant avec sa proche étoile parente. -L'effet de la déformation due aux marées sur les paramètres observables d'une planète en transit grâce au suivi photométrique de son passage devant l'étoile. -L'incidence sur la structure et l'évolution d'une diminution de l'efficacité du transport de chaleur par convection due à un gradient d'éléments lourd dans l'enveloppe gazeuse d'une planète géante, conduisant au phénomène de convection double-diffusive. A travers l'étude des ces divers processus, j'ai développé différents modèles analytiques et codes numériques qui sont à la fois flexibles et robustes, et qui permettent maintenant d'étudier certaines propriétés des nouveaux objets substellaires détectés à mesure qu'ils sont découverts.

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Benítez, Llambay Pablo. "Formación y evolución de exoplanetas." Bachelor's thesis, 2011. http://hdl.handle.net/11086/45.

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Tesis (Lic. en Astronomía)--Universidad Nacional de Córdoba. Facultad de Matemática, Astronomía y Física, 2011.
En este trabajo se estudian principalmente los procesos de formación y evolución planetaria en diferentes etapas. En la etapa temprana, se estudia el proceso desde la formación del disco protoplanetario hasta la formación del embrión planetario. Se estudia la interacción planeta-disco y las consecuencias de ésta. Se estudia el concepto de trampas planetarias y su aplicación a problemas concretos. En la etapa tardía se estudian las fuerzas de marea generadas por la interacción gravitatoria planeta-estrella, y en particular se aplican estos resultados a planetas de corto período. Como aplicación se realiza un estudio de la distribución masa-período de los exoplanetas de corto período conocidos y se propone una explicación para la forma de tal distribución. Por último, se aplican los estudios realizados a un caso exoplanetario particular: CoRoT-7.
Pablo Benítez Llambay

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"Biochemical Networks Across Planets and Scales." Doctoral diss., 2018. http://hdl.handle.net/2286/R.I.51691.

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abstract: Biochemical reactions underlie all living processes. Their complex web of interactions is difficult to fully capture and quantify with simple mathematical objects. Applying network science to biology has advanced our understanding of the metabolisms of individual organisms and the organization of ecosystems, but has scarcely been applied to life at a planetary scale. To characterize planetary-scale biochemistry, I constructed biochemical networks using global databases of annotated genomes and metagenomes, and biochemical reactions. I uncover scaling laws governing biochemical diversity and network structure shared across levels of organization from individuals to ecosystems, to the biosphere as a whole. Comparing real biochemical reaction networks to random reaction networks reveals the observed biological scaling is not a product of chemistry alone, but instead emerges due to the particular structure of selected reactions commonly participating in living processes. I perform distinguishability tests across properties of individual and ecosystem-level biochemical networks to determine whether or not they share common structure, indicative of common generative mechanisms across levels. My results indicate there is no sharp transition in the organization of biochemistry across distinct levels of the biological hierarchy—a result that holds across different network projections. Finally, I leverage these large biochemical datasets, in conjunction with planetary observations and computational tools, to provide a methodological foundation for the quantitative assessment of biology’s viability amongst other geospheres. Investigating a case study of alkaliphilic prokaryotes in the context of Enceladus, I find that the chemical compounds observed on Enceladus thus far would be insufficient to allow even these extremophiles to produce the compounds necessary to sustain a viable metabolism. The environmental precursors required by these organisms provides a reference for the compounds which should be prioritized for detection in future planetary exploration missions. The results of this framework have further consequences in the context of planetary protection, and hint that forward contamination may prove infeasible without meticulous intent. Taken together these results point to a deeper level of organization in biochemical networks than what has been understood so far, and suggests the existence of common organizing principles operating across different levels of biology and planetary chemistry.
Dissertation/Thesis
Doctoral Dissertation Geological Sciences 2018

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"Hydrothermal Habitats: Measurements of Bulk Microbial Elemental Composition, and Models of Hydrothermal Influences on the Evolution of Dwarf Planets." Doctoral diss., 2015. http://hdl.handle.net/2286/R.I.35987.

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abstract: Finding habitable worlds is a key driver of solar system exploration. Many solar system missions seek environments providing liquid water, energy, and nutrients, the three ingredients necessary to sustain life. Such environments include hydrothermal systems, spatially-confined systems where hot aqueous fluid circulates through rock by convection. I sought to characterize hydrothermal microbial communities, collected in hot spring sediments and mats at Yellowstone National Park, USA, by measuring their bulk elemental composition. To do so, one must minimize the contribution of non-biological material to the samples analyzed. I demonstrate that this can be achieved using a separation method that takes advantage of the density contrast between cells and sediment and preserves cellular elemental contents. Using this method, I show that in spite of the tremendous physical, chemical, and taxonomic diversity of Yellowstone hot springs, the composition of microorganisms there is surprisingly ordinary. This suggests the existence of a stoichiometric envelope common to all life as we know it. Thus, future planetary investigations could use elemental fingerprints to assess the astrobiological potential of hydrothermal settings beyond Earth. Indeed, hydrothermal activity may be widespread in the solar system. Most solar system worlds larger than 200 km in radius are dwarf planets, likely composed of an icy, cometary mantle surrounding a rocky, chondritic core. I enhance a dwarf planet evolution code, including the effects of core fracturing and hydrothermal circulation, to demonstrate that dwarf planets likely have undergone extensive water-rock interaction. This supports observations of aqueous products on their surfaces. I simulate the alteration of chondritic rock by pure water or cometary fluid to show that aqueous alteration feeds back on geophysical evolution: it modifies the fluid antifreeze content, affecting its persistence over geological timescales; and the distribution of radionuclides, whose decay is a chief heat source on dwarf planets. Interaction products can be observed if transported to the surface. I simulate numerically how cryovolcanic transport is enabled by primordial and hydrothermal volatile exsolution. Cryovolcanism seems plausible on dwarf planets in light of images recently returned by spacecrafts. Thus, these coupled geophysical-geochemical models provide a comprehensive picture of dwarf planet evolution, processes, and habitability.
Dissertation/Thesis
Doctoral Dissertation Astrophysics 2015

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Books on the topic "Planetology of uid planets"

1

Moons & planets. 5th ed. Belmont, CA: Thomson Brooks/Cole, 2005.

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Hartmann, William K. Moons & planets. 4th ed. Belmont, CA: Wadsworth Pub. Co., 1999.

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Henbest, Nigel. The planets. London: Penguin Books, 1994.

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Hartmann, William K. Moons & planets. 3rd ed. Belmont, Calif: Wadsworth, 1993.

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M, Woolfson M., ed. Planetary science: The science of planets around stars. Bristol, [U.K.]: IoP, 2002.

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Planetology: Comparing other worlds to our own. New York: Franklin Watts, 1996.

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Frankel, Charles. Dernières nouvelles des planètes. Paris: Seuil, 2009.

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service), SpringerLink (Online, ed. The Transits of Extrasolar Planets with Moons. Berlin, Heidelberg: Springer-Verlag Berlin Heidelberg, 2011.

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Alan, Penny, ed. Planetary systems in the universe: Observation, formation and evolution : proceedings of the 202nd Symposium of the International Astronomical Union held at University of Manchester, Manchester, United Kingdom, August 7-10, 2000. [San Francisco, Calif.]: Published on behalf of the IAU by Astronomical Society of the Pacific, 2004.

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1914-, Emery K. O., ed. Morphology of the rocky members of the solar system. Berlin: Springer-Verlag, 1993.

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Book chapters on the topic "Planetology of uid planets"

1

Kaula, William M. "Formation of the Terrestrial Planets." In Comparative Planetology with an Earth Perspective, 1–11. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-017-1092-3_1.

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Greeley, Ronald. "Geology of Terrestrial Planets with Dynamic Atmospheres." In Comparative Planetology with an Earth Perspective, 13–27. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-017-1092-3_2.

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Ipatov, S. I. "Migration of Bodies in the Accumulation of Planets." In Comparative Planetology with an Earth Perspective, 217–19. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-017-1092-3_20.

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Encrenaz, T. "The Chemical Atmospheric Composition of the Giant Planets." In Comparative Planetology with an Earth Perspective, 77–87. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-017-1092-3_9.

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Scholz, Mathias. "Statistik, Klassifikation und Diversität von Exoplaneten." In Planetologie extrasolarer Planeten, 223–83. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-662-44445-0_4.

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Spilker, Thomas R. "NH3, H2S, and the Radio Brightness Temperature Spectra of the Giant Planets." In Comparative Planetology with an Earth Perspective, 89–94. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-017-1092-3_10.

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"5. Planetologie." In Erde und Planeten, 427–526. De Gruyter, 2001. http://dx.doi.org/10.1515/9783110198027.427.

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"Chapter 2 Petro-tectonic features of terrestrial planets." In High-Pressure Geochemistry and Mineral Physics - Basics for Planetology and Geo-material Science, 177–282. Elsevier, 2004. http://dx.doi.org/10.1016/s0921-3198(04)80004-8.

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