Relevant bibliographies by topics / Formation of the solar system

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  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers
  6. Reports

Academic literature on the topic 'Formation of the solar system'

Author: Grafiati
Published: 25 May 2024

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Journal articles on the topic "Formation of the solar system"

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Smith, Keith T. "Timing Solar System formation." Science 370, no. 6518 (November 12, 2020): 805.13–807. http://dx.doi.org/10.1126/science.370.6518.805-m.

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Morfill, G. E. "Models of solar system formation." Chemical Geology 70, no. 1-2 (August 1988): 32. http://dx.doi.org/10.1016/0009-2541(88)90268-9.

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Rawal, J. J. "Formation of the solar system." Astrophysics and Space Science 119, no. 1 (January 1986): 159–66. http://dx.doi.org/10.1007/bf00648837.

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Pfalzner, S., M. B. Davies, M. Gounelle, A. Johansen, C. Münker, P. Lacerda, S. Portegies Zwart, L. Testi, M. Trieloff, and D. Veras. "The formation of the solar system." Physica Scripta 90, no. 6 (April 21, 2015): 068001. http://dx.doi.org/10.1088/0031-8949/90/6/068001.

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Russell, Sara S. "The Formation of the Solar System." Journal of the Geological Society 164, no. 3 (May 2007): 481–92. http://dx.doi.org/10.1144/0016-76492006-054.

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Chambers, John. "Making the Solar System." Astrophysical Journal 944, no. 2 (February 1, 2023): 127. http://dx.doi.org/10.3847/1538-4357/aca96f.

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Abstract We model the early stages of planet formation in the solar system, including continual planetesimal formation, and planetesimal and pebble accretion onto planetary embryos in an evolving disk driven by a disk wind. The aim is to constrain aspects of planet formation that have large uncertainties by matching key characteristics of the solar system. The model produces a good fit to these characteristics for a narrow range of parameter space. Planetary growth beyond the ice line is dominated by pebble accretion. Planetesimal accretion is more important inside the ice line. Pebble accretion inside the ice line is slowed by higher temperatures, partial removal of inflowing pebbles by planetesimal formation and pebble accretion further out in the disk, and increased radial velocities due to gas advection. The terrestrial planets are prevented from accreting much water ice because embryos beyond the ice line reach the pebble-isolation mass before the ice line enters the terrestrial-planet region. When only pebble accretion is considered, embryos typically remain near their initial mass or grow to the pebble-isolation mass. Adding planetesimal accretion allows Mars-sized objects to form inside the ice line, and allows giant-planet cores to form over a wider region beyond the ice line. In the region occupied by Mercury, pebble Stokes numbers are small. This delays the formation of embryos and stunts their growth, so that only low-mass planets can form here.
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Ida, Shigeru, and Eiichiro Kokubo. "Terrestrial Planet Formation: The Solar System and Other Systems." Symposium - International Astronomical Union 202 (2004): 159–66. http://dx.doi.org/10.1017/s0074180900217749.

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Accretion of terrestrial planets and solid cores of jovian planets is discussed, based on the results of our N-body simulations. Protoplanets accrete from planetesimals through runaway and oligarchic growth until they become isolated. The isolation mass of protoplanets in terrestrial planet region is about 0.2 Earth mass, which suggests that in the final stage of terrestrial planet formation giant impacts between the protoplanets occur. On the other hand, the isolation mass in jovian planet region is about a few to 10 Earth masses, which may be massive enough to form a gas giant. Extending the above arguments to disks with various initial masses, we discuss diversity of planetary systems. We predict that the extrasolar planets so far discovered may correspond to the systems formed from disks with large initial masses and that the other disks with smaller masses, which are the majority of the disks, may form Earth-like planets.
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Imaeda, Yusuke, and Toshikazu Ebisuzaki. "Tandem planet formation for solar system-like planetary systems." Geoscience Frontiers 8, no. 2 (March 2017): 223–31. http://dx.doi.org/10.1016/j.gsf.2016.06.011.

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Yu, Ziyuan, Jin Liu, Chao Pan, Lvqian Guo, Zhiwei Kang, and Xin Ma. "Solar TDOA measurement and integrated navigation for formation flying." Proceedings of the Institution of Mechanical Engineers, Part G: Journal of Aerospace Engineering 233, no. 12 (February 2019): 4635–45. http://dx.doi.org/10.1177/0954410019827148.

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To improve the positioning accuracy of autonomous celestial navigation systems when flying in formation, we exploit the fact that the sole light source in the solar system is the Sun to directly provide positioning information for relative navigation. We term this solar Time Difference of Arrival (TDOA) navigation for formation flying. Solar light has the potential to provide a solar Time of Arrival (TOA) because of its unstable intensity. However, the solar TOA cannot be used for navigation because it has no baseline. To solve this problem, we took the difference between the solar TOAs of two spacecraft (the solar TDOA) as the basis for navigational measurement. The solar TDOA represents the relative distance between two spacecraft in a radial direction. However, whilst the solar TDOA is insensitive to solar direction errors, a free-standing solar TDOA navigation system is not observable. We therefore combined the solar TDOA with the Mars direction and inter-satellite link navigation system, to form an integrated solar TDOA/Mars direction/inter-satellite link navigation method for formation flying. Simulation results indicate that solar TDOA-based integrated navigation for formation flying can provide highly accurate navigation information, especially under relative conditions.
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Smith, Keith T. "Two-part formation of the Solar System." Science 371, no. 6527 (January 21, 2021): 358.4–359. http://dx.doi.org/10.1126/science.371.6527.358-d.

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Dissertations / Theses on the topic "Formation of the solar system"

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Crida, Aurélien. "Planetary migration in solar system formation." Nice, 2006. http://www.theses.fr/2006NICE4076.

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Planetary migration seems to be unavoidable during planet formation in protoplanetary disks. Gravitational interactions between the planet embryos and the gas disk make the angular momentum of the embryo decrease, so that it spirals towards the central star. As the migration timescale is shorter than the disk life time, no planet should survive (chapters 1 and 2). In this thesis, we try to find mechanisms that prevent or slow down migration. In chapter 3, we show that a jump in the gas disk density stops migration and acts like a planet trap. Trapped there, a massif solid core may accrete a gaseous atmosphere and give birth to a giant planet. The planet is then massive enough to repel the gas and open a gap around its orbit. Through analysis of computer simulations, we enlighten the role of pressure effects in this process in chapter 4 ; a new generalized gap opening criterion is derived. After the presentation of a new, reliable and performing algorithm for numerical simulations in chapter 5, we use it in chapter 6 to study the migration of a giant planet and its influence on the disk evolution. The formation of a cavity appears to be less easy than previously expected, but we find a way of preventing migration. Last, in chapter 7, we focus on the case of Jupiter and Saturn, and we find in which conditions the interactions between both planets prevent their migration
La migration planétaire est un phénomène apparemment inévitable lors de la formation des planètes dans les disques protoplanétaires. Les interactions gravitationnelles entre les embryons de planète et le disque de gaz font décroître le moment cinétique de l'embryon, qui spirale vers l'étoile centrale. Le temps de migration étant plus court que la durée de vie du disque, aucune planète ne devrait survivre (chapitres 1 et 2). Dans cette thèse, nous essayons de trouver des mécanismes qui empêchent ou ralentissent la migration. Dans le chapitre 3, nous montrons qu'un saut dans le profil de densité du disque de gaz bloque la migration et agit comme un piège à planète. Ainsi bloqué, un coeur solide massif peut accrèter une atmosphère gazeuse et devenir une planète géante. La planète est alors assez massive pour repousser le gaz et ouvrir un sillon autour de son orbite. En analysant des simulations numériques, nous mettons en évidence le rôle des effets de pression dans ce processus dans le chapitre 4; un nouveau critère unifié d'ouverture du sillon en découle. Après la présentation dans le chapitre 5 d'un nouvel algorithme fiable et performant pour réaliser des simulations numériques, nous l'utilisons dans le chapitre 6 pour étudier la migration d'une planète géante et son impact sur l'évolution du disque. La formation d'une cavité s'avère moins facile que prévu, mais une possibilité d'arrêter la migration apparaît. Enfin, dans le chapitre 7, nous étudions le cas de Jupiter et Saturne, et trouvons dans quelles conditions les interactions entre les deux planètes en empêchent la migration
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Cyr, Kimberly Ellen 1964. "The distribution of water in the solar nebula: Implications for solar system formation." Diss., The University of Arizona, 1998. http://hdl.handle.net/10150/288870.

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Water is important in the solar nebula both because it is extremely abundant and because it condenses out at 5 AU, allowing all three phases of H₂O to play a role in the composition and evolution of the solar system. In this work, a thorough examination of the inward radial drift of ice particles from 5 AU is undertaken. Drift model results are then linked to the outward diffusion of vapor, in one overall model which is numerically evolved over the lifetime of the nebula. Results of the model indicate that while the inner nebula is generally depleted in water vapor, there is a zone in which the vapor is enhanced by ∼40-100%, depending on the choice of ice grain growth mechanisms and rates. This enhancement peaks in the region from 0.1-2 AU and gradually drops off out to 5 AU. Conversely, ice abundance is enhanced over 3-5 AU. Representative hot (early) and cool (later) conditions during the quiescent phase of nebular evolution are examined. Additionally, the effect of the radial dependence of water depletion on nebular chemistry is quantified using a chemical equilibrium code that computes abundances of nebular elements and major molecular C, N, S, etc. species over a range of temperatures. In particular, changes in the local C/O ratio and organics abundance due to the radially dependent decrease in oxygen fugacity are tracked and plotted. Generally, the diffusion-drift model results in a more complex water distribution than previous models, with both radial and temporal variations in the C/O ratio which produce both relatively oxidizing and reducing nebular conditions across 1-5 AU. Depending on the value assumed for the solar C/O ratio, modest to significant enhancements of CH₄ and other organics abundances are produced in the inner nebula. These results coupled with the revised ice distribution may explain the radial signatures of hydration detections and darkening in asteroids, and perhaps the oxidation states of enstatite chondrites. The results also indicate that the inner nebula could have supplied organics and water to the terrestrial planets, as well as possibly to Europa and beyond, via outward mixing processes.
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Elliott, Garrett T. "Detecting the debris of solar system formation via stellar occultation." Connect to resource, 2008. http://hdl.handle.net/1811/32191.

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Mehta, Anand Vivek 1966. "The role of vortices in the formation of the solar system." Thesis, Massachusetts Institute of Technology, 1998. http://hdl.handle.net/1721.1/50500.

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Thesis (Ph.D.)--Massachusetts Institute of Technology, Dept. of Physics, 1998.
Includes bibliographical references (p. 117-119).
An important part of explaining planet formation is understanding how small particles accumulate into larger bodies. Gas vortices are suggested as a mechanism to enhance the coagulation of dust particles in the solar nebula. An inviscid, barotropic, two-dimensional form of the vorticity equation is derived to study the gas flow. A pseudospectral numerical model uses this equation to calculate the evolution of the vorticity field. The calculations show that locally prograde elliptical vortices with the major axis parallel to the angular axis can persist for at least 103 years with less than 1% change in peak vorticity. The shape of the vortex depends on the strength, similar to analytical expressions for elliptical vortices in a linear shear. Stronger vortices are rounder while weaker vortices are elongated; With ratios of the peak vorticity to the background vorticity of 1.0 and 0.2, the aspect ratios are approximately 0.5 and 0.25. The vortex area is mostly constant, and the linear dimensions change as the shape changes. Two negative vortices within the same radial band tend to merge, forming a larger, stronger vortex in a few orbit periods. A random viscosity field tends to have a few strong vortices form, although not as efficiently as with merging vortices. Dust particles interact with the gas through the Stokes drag force, with the relaxation time specifying how quickly the particle velocity approaches the gas velocity. The particles tend to converge in high pressure vortices and drift out of low pressure systems. The convergence time is dependent on the vortex strength and the particle relaxation time. If the relaxation time is short compared to the period, the particles do not have an appreciable differential velocity compared to the gas, and the Stokes drag force is small. If the relaxation time is long, then the Stokes drag force is not large enough to have a significant effect. If, however, the relaxation time is of the same order as the period, so the dynamical and frictional timescales are similar, then the particles will have the shortest convergence times. This result can be seen analytically in the simple case of an axisymmetric pressure band and numerically in calculations involving the robust vortex. With a robust vortex, the convergence times are approximately 3-4 yr for relaxation times of 0.1-0.2 yr. For typical values of properties of the solar nebula, this relaxation time applies for particles with diameters of around 20 cm. Other particles, both smaller and larger, converge more slowly, but the different times result in more collisions, enhancing the coagulation of larger bodies.
by Anand Vivek Mehta.
Ph.D.
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Lawler, Samantha. "The leftovers of planet formation : small body populations of our solar system and exoplanet systems." Thesis, University of British Columbia, 2013. http://hdl.handle.net/2429/44760.

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The small body populations within a planetary system give information about the planet formation and migration history of the system. In our Solar System, we study these bodies (asteroids, comets, and trans-Neptunian objects), by directly observing them in reflected light. In other solar systems, dust traces the position of the planetesimal belts that produce it, and is observed as an excess above the stellar flux in the infrared. The dust is visible and not the planetesimals because of the much greater cross-sectional surface area of a swarm of dust particles. In this thesis, both leftover large planetesimals in our Solar System and dust around other stars are investigated. Data from the Canada-France Ecliptic Plane Survey (CFEPS) are used to measure the absolute populations of trans Neptunian objects (TNOs) in mean-motion resonances with Neptune, as well as constrain the internal orbital element distributions. Detection biases play a critical role because phase relationships with Neptune make object discovery more likely at certain longitudes. The plutinos (objects in the 3:2 resonance) are given particular attention because the presence of the secular Kozai resonance within the mean-motion resonance causes different detection biases that need to be accounted for to properly debias surveys that include detections of plutinos. Because the TNOs that are trapped in mean-motion resonances with Neptune were likely emplaced there during planet migration late in the giant planet formation process, the structure within and relative populations of the resonances should be a diagnostic of the timescale and method of giant planet migration. Exoplanet systems that host several rocky planets are those that did not experience giant planet migration, and thus are likely to host planetesimal belts which should be detectable as debris disks. The Kepler Mission has detected a host of such systems, and we use data from the Wide-field Infrared Survey Explorer (WISE) Mission to search for debris disks around these stars. Though we tentatively detect more excesses toward these stars than would be expected, contamination from warm dust in the Milky Way Galaxy makes detection unreliable for these systems, and will have to await future infrared space telescopes.
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Patzelt, Madelein [Verfasser], and Klaus [Akademischer Betreuer] Mezger. "Chondrule formation in the early Solar System / Madelein Patzelt ; Betreuer: Klaus Mezger." Münster : Universitäts- und Landesbibliothek Münster, 2015. http://d-nb.info/1138279943/34.

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Theis, Karen Julia. "Iron isotope fractionation of planetary bodies during early solar system formation processes." Thesis, University of Manchester, 2008. http://www.manchester.ac.uk/escholar/uk-ac-man-scw:163898.

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The aims of this research programme were twofold: to analyse the iron isotope compositions of metal grains from ordinary chondrite meteorites over a range of class and petrographic type to investigate redox reactions and thermal metamorphism during primitive planetesimal formation; and to analyse the iron isotope composition of secondary carbonate minerals in Martian meteorite ALH84001 to determine the formation temperature and thus constrain near surface conditions on early Mars. To analyse the iron isotope compositions of these materials it was necessary to develop a methodology using a Nu Plasma multi collector inductively coupled plasma mass spectrometer and a new technique for analysing natural iron-bearing samples without first purifying them by anion exchange chromatography. The purification process can cause fractionation within the sample which may mask small natural fractionation variations. The new methodology developed here yielded reproducible iron isotope ratios to within o.osroo (20) ensuring that small isotopic variations of (i56Fe -0.06roo to 0.3sroo were resolved during the analysis of the ordinary chondrite metal grains. The method for analysing samples containing matrix elements was successful and achieved an accuracy and precision comparable to pure analyte solutions for the analysis of the Martian carbonates. The analysis of the metal grains revealed a correlation between their iron isotope compositions and the redox and thermal metamorphism that these materials have experienced. The results indicate that the degree of iron isotope fractionation can be related to thermal metamorphism temperatures, except for metal grains from type 3 chondrites. This was interpreted as resulting from the type 3 chondrites not getting hot enough during thermal metamorphism to overprint the original igneous isotopic signatures. The a-rich carbonates in ALH84001 were petrographically characterised to place them within the known carbonate assemblage sequence which implied that the zoned carbonate deposition occurred during multiple phases. The zoned carbonates were then analysed for iron isotope composition and an isotopic fractionation variation for (i56Fe of -0.6%0 was determined relative to bulk Martian silicates. This indicated a formation temperature of approximately ±800( (20) and implied that liquid water was stable on or near the surface during this time.
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Gorlova, Nadiya Igorivna. "Debris Disks in Open Stellar Clusters." Diss., The University of Arizona, 2006. http://hdl.handle.net/10150/195908.

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Indirect searches for planets (such as radial velocity studies)show that their formation may be quite common. The planets are however too small and faint to be seen against the glare of their host stars; therefore, their direct detectionis limited to the nearest systems. Alternatively one can study planets by studying their "by-product" -- dust. We see raw material available for planets around young stars, anddebris dust around old stars betraying planet-induced activity. Dust has a larger surface area per unit mass compared with a large body; it can be spread over a largersolid angle, intercepting more starlight and emitting much more lightvia reprocessing. By studying dusty disks we can infer the presence of planets at larger distances.Here we present results of a survey conducted with the SpitzerSpace Telescope of debrisdisks in three open clusters. With ages of 30--100 Myrs, these clusters are old enough that the primordialdust should have accreted into planetesimals, fallen onto the star, or been blown away due to a numberof physical processes. The dust we observe must come from collisions or sublimation of larger bodies.The purpose of this study is to investigate the dustevolution in the terrestrial planet zone, analogous to the Zodiacal cloud in our Solar system. We are most sensitive to this zone becausethe peak of a 125 K black body radiation falls into the primary pass-band of our survey -- 24 micron. We investigate the fraction and amount of the infra-red excesses around intermediate- to solar-mass stars in open stellar clusterswith well defined ages. The results are analyzed in the context of disk studies at other wavelengths and ages, providing an understanding of the time-scale for diskdissipation and ultimately planet building and frequency.
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Miller, Kelly E., and Kelly E. Miller. "The R Chondrite Record of Volatile-Rich Environments in the Early Solar System." Diss., The University of Arizona, 2016. http://hdl.handle.net/10150/621016.

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Chondritic meteorites are undifferentiated fragments of asteroids that contain the oldest solids formed in our Solar System. Their primitive, solar-like chemical compositions indicate that they experienced very little processing following accretion to their parent bodies. As such, they retain the best records of chemical and physical processes active in the protoplanetary disk during planet formation. Chondritic meteorites are depleted relative to the sun in volatile elements such as S and O. In addition to being important components of organic material, these elements exert a strong influence on the behavior of other more refractory species and the composition of planets. Understanding their distribution is therefore of key interest to the scientific community. While the bulk abundance of volatile elements in solid phases present in meteorites is below solar values, some meteorites record volatile-rich gas phases. The Rumuruti (R) chondrites record environments rich in both S and O, making them ideal probes for volatile enhancement in the early Solar System. Disentangling the effects of parent-body processing on pre-accretionary signatures requires unequilibrated meteorite samples. These samples are rare in the R chondrites. Here, I report analyses of unequilibrated clasts in two thin sections from the same meteorite, PRE 95404 (R3.2 to R4). Data include high resolution element maps, EMP chemical analyses from silicate, sulfide, phosphate, and spinel phases, SIMS oxygen isotope ratios of chondrules, and electron diffraction patterns from Cu-bearing phases. Oxygen isotope ratios and chondrule fO2 levels are consistent with type II chondrules in LL chondrites. Chondrule-sized, rounded sulfide nodules are ubiquitous in both thin sections. There are multiple instances of sulfide-silicate relationships that are petrologically similar to compound chondrules, suggesting that sulfide nodules and silicate chondrules formed as coexisting melts. This hypothesis is supported by the presence of phosphate inclusions and Cu-rich lamellae in both sulfide nodules and sulfide assemblages within silicate chondrules. Thermodynamic analyses indicate that sulfide melts reached temperatures up to 1138 °C and fS2 of 2 x 10^(-3) atm. These conditions require total pressures on the order of 1 atm, and a dust- or ice-rich environment. Comparison with current models suggest that either the environmental parameters used to model chondrule formation prior to planetesimal formation should be adjusted to meet this pressure constraint, or R chondrite chondrules may have formed through planetesimal bow shocks or impacts. The pre-accretionary environment recorded by unequilibrated R chondrites was therefore highly sulfidizing, and had fO2 higher than solar composition, but lower than the equilibrated R chondrites.Chalcopyrite is rare in meteorites, but forms terrestrially in hydrothermal sulfide deposits. It was previously reported in the R chondrites. I studied thin sections from PRE 95411 (R3 or R4), PCA 91002 (R3.8 to R5), and NWA 7514 (R6) using Cu X-ray maps and EMP chemical analyses of sulfide phases. I found chalcopyrite in all three samples. TEM electron diffraction data from a representative assemblage in PRE 95411 are consistent with this mineral identification. TEM images and X-ray maps reveal the presence of an oxide vein. A cubanite-like phase was identified in PCA 91002. Electron diffraction patterns are consistent with isocubanite. Cu-rich lamellae in the unequilibrated clasts of PRE 95404 are the presumed precursor materials for chalcopyrite and isocubanite. Diffraction patterns from these precursor phases index to bornite. I hypothesize that bornite formed during melt crystallization prior to accretion. Hydrothermal alteration on the parent body by an Fe-rich aqueous phase between 200 and 300°C resulted in the formation of isocubanite and chalcopyrite. In most instances, isocubanite may have transformed to chalcopyrite and pyrrhotite at temperatures below 210°C. This environment was both oxidizing and sulfidizing, suggesting that the R chondrites record an extended history of volatile-rich interaction. These results indicate that hydrothermal alteration of sulfides on the R chondrite parent body was pervasive and occurred even in low petrologic types. This high temperature aqueous activity is distinct from both the low temperature aqueous alteration of the carbonaceous chondrites and the high temperature, anhydrous alteration of the ordinary chondrites.
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Williams, Niel Hamilton. "Titanium isotope cosmochemistry." Thesis, University of Manchester, 2015. https://www.research.manchester.ac.uk/portal/en/theses/titanium-isotope-cosmochemistry(571ae148-1673-4b85-bc10-937284bb53fc).html.

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High precision measurements of Ti isotopes within terrestrial and extra-terrestrial materials were made in order to investigate the processes at work within the early solar system. Variations of Ti isotopes also enabled the investigation of the specific stellar sources that created the material that formed the solar system. Titanium was chosen as it is a refractory element, relatively resistant to secondary processes and found abundantly in all solar system materials. Measurements were performed using a Thermo Fischer Neptune MC-ICPMS at the Open University, Milton Keynes. Various samples of carbonaceous chondrites, ordinary chondrites, enstatite chondrites, achondrites, lunar, terrestrial and early solar system components were analysed. Mass independent measurements of various solar system materials revealed a correlation between ε50/47Ti49/47 and ε46/47Ti49/47 defining a best line with a slope of 5.34 ± 0.34. The correlation indicates that solar system materials contain nucleosynthetic components that match a SNII stellar source. Utilising aliquots previously analysed for Zr isotopes for Ti isotope analyses revealed a correlation between ε50/47Ti49/47 and ε96/90Zr94/90 for the carbonaceous chondrites that is controlled by the CAI content of the particular carbonaceous chondrite group. Step wise dissolution of ordinary chondrites and carbonaceous chondrites revealed multiple nucleosynthetic Ti components contributing to the solar system. Stepwise leachate dissolutions were conducted on the carbonaceous chondrites Allende, Murchison and Orgueil to compliment the study of the same samples for Zr by Schönbächler et al. (2005). In addition, sample aliquots of QUE 97008 and Murchison from the work of Qin et al. (2011) were also investigated for Ti. The two investigations allow the comparison of Ti in different phases to be compared with other isotope systems such as Zr (Schönbächler et al. 2005) and Cr, Sr, Ba, Sm, Nd and Hf (Qin et al. 2011).Mass dependent fractionation and absolute nucleosynthetic anomalies of Ti within solar system materials was determined by utilising the double spike procedure. Mass dependent analysis enabled the Stable isotope composition of terrestrial materials to be investigated, revealing mass dependent fractionation between terrestrial basalts and andesite’s. Utilising the double spike procedure also enabled the calculation of absolute nucleosynthetic anomalies for Ti within solar system materials. The absolute nucleosynthetic anomalies data revealed that CAI’s contain two different compositions with one representing an exotic stellar source and the other representing the mainstream solar system composition.
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Books on the topic "Formation of the solar system"

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Ferronsky, V. I., and S. V. Ferronsky. Formation of the Solar System. Dordrecht: Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5908-4.

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Rossi, Matteo De. Solar system: Structure, formation, and exploration. Hauppauge, N.Y: Nova Science Publisher's, 2011.

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Anfilogov, Vsevolod N., and Yurij V. Khachay. Some Aspects of the Formation of the Solar System. Cham: Springer International Publishing, 2015. http://dx.doi.org/10.1007/978-3-319-17831-8.

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Mandt, Kathleen, Olivier Mousis, Dominique Bockelée-Morvan, and Christopher Russell, eds. Comets as Tracers of Solar System Formation and Evolution. Dordrecht: Springer Netherlands, 2017. http://dx.doi.org/10.1007/978-94-024-1103-4.

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Pessah, Martin, and Oliver Gressel, eds. Formation, Evolution, and Dynamics of Young Solar Systems. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-60609-5.

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Formation of water and our solar system from a fission process with an. [Place of publication not identified]: Xlibris Corporation, 2011.

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ESLAB Symposium. (24th 1990 Friedrichshafen, Germany). Formation of stars and planets and the evolution of the solar system: Proceedings of the 24th ESLAB Symposium, 17 - 19 September 1990, Friedrichshafen, Germany. Edited by Battrick B. 1946-, Schwehm G, Stammes P, and European Space Agency. Noordwijk, The Netherlands: ESA Publications, 1990.

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1953-, Weaver Harold A., Danly L, and Space Telescope Science Institute (U.S.), eds. The formation and evolution of planetary systems: Proceedings of the Formation and Evolution of Planetary Systems Meeting, Baltimore, 1988, May 9-11. Cambridge: Cambridge University Press, 1989.

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United States. National Aeronautics and Space Administration., ed. Origins of interstellar and solar system carbonaceous materials: Final technical report. [Washington, DC: National Aeronautics and Space Administration, 1994.

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V, Ferronskiĭ S., ed. Formation of the solar system: A new theory of the creation and decay of the celestial bodies. Dordrecht: Springer, 2013.

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Book chapters on the topic "Formation of the solar system"

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Crida, Aurélien. "Solar System Formation." In Reviews in Modern Astronomy, 215–27. Weinheim, Germany: Wiley-VCH Verlag GmbH & Co. KGaA, 2010. http://dx.doi.org/10.1002/9783527629190.ch12.

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Robert, François. "Solar System Formation (Chronology)." In Encyclopedia of Astrobiology, 1528–35. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-11274-4_1797.

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Southwood, D. J. "Formation of Magnetotails." In Magnetotails in the Solar System, 197–215. Hoboken, NJ: John Wiley & Sons, Inc, 2015. http://dx.doi.org/10.1002/9781118842324.ch12.

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Petit, Jean-Marc, and Alessandro Morbidelli. "Chronology of Solar System Formation." In Lectures in Astrobiology, 61–82. Berlin, Heidelberg: Springer Berlin Heidelberg, 2005. http://dx.doi.org/10.1007/10913406_3.

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Robert, François. "System Solar Formation, Chronology of." In Encyclopedia of Astrobiology, 2450–58. Berlin, Heidelberg: Springer Berlin Heidelberg, 2015. http://dx.doi.org/10.1007/978-3-662-44185-5_1797.

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Rawal, J. J. "Formation of the Solar System." In Third Asian-Pacific Regional Meeting of the International Astronomical Union, 159–66. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4630-9_37.

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Robert, François. "System Solar Formation, Chronology of." In Encyclopedia of Astrobiology, 1–9. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-642-27833-4_1797-2.

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Robert, François. "System Solar Formation, Chronology of." In Encyclopedia of Astrobiology, 2985–93. Berlin, Heidelberg: Springer Berlin Heidelberg, 2023. http://dx.doi.org/10.1007/978-3-662-65093-6_1797.

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Bally, John, Alan Boss, Dimitri Papanastassiou, Scott Sandford, and Anneila Sargent. "Star Formation and the Solar System." In Galactic and Extragalactic Star Formation, 311–27. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2973-9_19.

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Pirronello, Valerio. "Molecule Formation in Cometary Environments." In Ices in the Solar System, 261–72. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5418-2_17.

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Conference papers on the topic "Formation of the solar system"

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Palouš, Jan, Richard Wünsch, Vasile Mioc, Cristiana Dumitrache, and Nedelia A. Popescu. "Star Formation and Evolution of Galaxies." In EXPLORING THE SOLAR SYSTEM AND THE UNIVERSE. AIP, 2008. http://dx.doi.org/10.1063/1.2993679.

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Kadik, A. A. "Formation of carbon species in terrestrial magmas." In Volatiles in the Earth and solar system. AIP, 1995. http://dx.doi.org/10.1063/1.48734.

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Lunine, Jonathan I., Wei Dai, and Fatima Ebrahim. "Solar system formation and the distribution of volatile species." In Volatiles in the Earth and solar system. AIP, 1995. http://dx.doi.org/10.1063/1.48735.

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Bilenko, I. A., Vasile Mioc, Cristiana Dumitrache, and Nedelia A. Popescu. "Conditions for the formation of CMEs associated with filament eruptions." In EXPLORING THE SOLAR SYSTEM AND THE UNIVERSE. AIP, 2008. http://dx.doi.org/10.1063/1.2993659.

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Lichtenberg, Tim, Joanna Drążkowska, Maria Schönbächler, Gregor Golabek, and Thomas Hands. "Bifurcation of planetary building blocks during Solar System formation." In Goldschmidt2021. France: European Association of Geochemistry, 2021. http://dx.doi.org/10.7185/gold2021.4476.

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Li, Ming, Huizhu Yang, Gedong Jiang, Wenjun Wang, and Xuesong Mei. "Formation of nanostructures on the surface of CIGS films by picosecond laser with different beam patterns." In Photonics for Solar Energy Systems, edited by Ralf B. Wehrspohn and Alexander N. Sprafke. SPIE, 2018. http://dx.doi.org/10.1117/12.2306814.

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Takeichi, Noboru. "Feasibility Study of a Solar Power Satellite System Configured by Formation Flying." In 54th International Astronautical Congress of the International Astronautical Federation, the International Academy of Astronautics, and the International Institute of Space Law. Reston, Virigina: American Institute of Aeronautics and Astronautics, 2003. http://dx.doi.org/10.2514/6.iac-03-r.1.07.

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Young, Edward, and Michelle Jordan. "IRON ISOTOPE CONSTRAINTS ON PLANETESIMAL CORE FORMATION IN THE EARLY SOLAR SYSTEM." In GSA Annual Meeting in Denver, Colorado, USA - 2016. Geological Society of America, 2016. http://dx.doi.org/10.1130/abs/2016am-284424.

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Cassen, Patrick, and Kenneth M. Chick. "The survival of presolar grains during the formation of the solar system." In ASTROPHYSICAL IMPLICATIONS OF THE LABORATORY STUDY OF PRESOLAR MATERIALS. ASCE, 1997. http://dx.doi.org/10.1063/1.53324.

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Tamura, M., M. Takami, K. Enya, T. Ootsubo, M. Fukagawa, M. Honda, Y. K. Okamoto, et al. "Key Sciences of SPICA Mission: Planetary Formation, Exoplanets, and our Solar System." In SPICA joint European/Japanese Workshop. Les Ulis, France: EDP Sciences, 2009. http://dx.doi.org/10.1051/spica/200902001.

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Reports on the topic "Formation of the solar system"

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Brown, W. K. High explosive simulations of supernovae and the supernova shell fragmentation model of solar system formation. Office of Scientific and Technical Information (OSTI), September 1987. http://dx.doi.org/10.2172/6019760.

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BARKHATOV, NIKOLAY, and SERGEY REVUNOV. A software-computational neural network tool for predicting the electromagnetic state of the polar magnetosphere, taking into account the process that simulates its slow loading by the kinetic energy of the solar wind. SIB-Expertise, December 2021. http://dx.doi.org/10.12731/er0519.07122021.

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Abstract:
The auroral activity indices AU, AL, AE, introduced into geophysics at the beginning of the space era, although they have certain drawbacks, are still widely used to monitor geomagnetic activity at high latitudes. The AU index reflects the intensity of the eastern electric jet, while the AL index is determined by the intensity of the western electric jet. There are many regression relationships linking the indices of magnetic activity with a wide range of phenomena observed in the Earth's magnetosphere and atmosphere. These relationships determine the importance of monitoring and predicting geomagnetic activity for research in various areas of solar-terrestrial physics. The most dramatic phenomena in the magnetosphere and high-latitude ionosphere occur during periods of magnetospheric substorms, a sensitive indicator of which is the time variation and value of the AL index. Currently, AL index forecasting is carried out by various methods using both dynamic systems and artificial intelligence. Forecasting is based on the close relationship between the state of the magnetosphere and the parameters of the solar wind and the interplanetary magnetic field (IMF). This application proposes an algorithm for describing the process of substorm formation using an instrument in the form of an Elman-type ANN by reconstructing the AL index using the dynamics of the new integral parameter we introduced. The use of an integral parameter at the input of the ANN makes it possible to simulate the structure and intellectual properties of the biological nervous system, since in this way an additional realization of the memory of the prehistory of the modeled process is provided.
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Moens, L., and D. Blake. Mechanism of Hydrogen Formation in Solar Paraboic Trough Receivers. Office of Scientific and Technical Information (OSTI), February 2008. http://dx.doi.org/10.2172/924987.

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Hamilton, C. Views of the solar system. Office of Scientific and Technical Information (OSTI), February 1995. http://dx.doi.org/10.2172/10116814.

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Sussman, Gerald J., and Jack Wisdom. Chaotic Evolution of the Solar System. Fort Belvoir, VA: Defense Technical Information Center, March 1992. http://dx.doi.org/10.21236/ada260055.

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Wesle, Max, and Robert Buchinger. INFO Sheet C03: One-World-Solar-System. IEA SHC Task 54, November 2017. http://dx.doi.org/10.18777/ieashc-task54-2017-0014.

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Mills, A., A. Botterud, J. Wu, Z. Zhou, B.-M. Hodge, and M. Heaney. Integrating Solar PV in Utility System Operations. Office of Scientific and Technical Information (OSTI), November 2013. http://dx.doi.org/10.2172/1107495.

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Baines, K. H., D. T. Gavel, A. M. Getz, S. G. Gibbartd, B. MacIntosh, C. E. Max, C. P. McKay, E. F. Young, and I. de Pater. Solar system events at high spatial resolution. Office of Scientific and Technical Information (OSTI), February 1999. http://dx.doi.org/10.2172/12548.

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Mills, A., A. Botterud, J. Wu, Z. Zhou, B.-M. Hodge, and M. Heany. Integrating Solar PV in Utility System Operations. Office of Scientific and Technical Information (OSTI), October 2013. http://dx.doi.org/10.2172/1164898.

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Skordos, Panayotis A. Multistep Methods for Integrating the Solar System. Fort Belvoir, VA: Defense Technical Information Center, July 1988. http://dx.doi.org/10.21236/ada201692.

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