Journal articles: '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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Guilera, O. M., A. Fortier, A. Brunini, and O. G. Benvenuto. "Simultaneous formation of solar system giant planets." Astronomy & Astrophysics 532 (August 2011): A142. http://dx.doi.org/10.1051/0004-6361/201015731.

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Keller, Horst Uwe. "Comets : A Key to Solar System Formation." Zeitschrift für Naturforschung A 44, no. 10 (October 1, 1989): 867–76. http://dx.doi.org/10.1515/zna-1989-1001.

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Abstract Four lines of information on comets are discussed: their orbits, their relation to other bodies of the planetary system, their physical state and chemical composition, and implications of recent observations of the nucleus of comet Halley. The in situ measurements during the flybys of comet Halley strongly support the assumption that comets are members of the solar system and were created during its formation. The region (heliocentric distance) of their formation is, however, still difficult to assess. The size, shape, and topography of the cometary nucleus suggest that it was formed from relatively large subnuclei in a region of the primordial solar nebula where relative velocities were sufficiently small. There are indications that some of the interplanetary dust particles in the Earth atmosphre may originate from comets.

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Griv, Evgeny, and Michael Gedalin. "Formation of the solar system by instability." Proceedings of the International Astronomical Union 2004, IAUC197 (August 2004): 97–106. http://dx.doi.org/10.1017/s1743921304008555.

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Levasseur-Regourd, A. Chantal. "Comets and Constraints on Solar System Formation." Highlights of Astronomy 9 (1992): 347–54. http://dx.doi.org/10.1017/s1539299600009187.

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AbstractNew and important data have been obtained during the 1985-1986 return of comet Halley, including in situ observations of the nucleus and the coma. Since the interpretation of the observations is not straightforward, the results are presented in a rather conservative manner. Some clues to the solar system formation are suggested, e.g. the shape of the nucleus, its low density, the estimated mass of the Oort cloud, the elemental abundances in comet Halley. Constraints related to isotopie abundances (deuterium enrichment, possible anomalies in carbon isotopes) and to cometary dust (complex organic compounds, submicron sized dust particles) are extensively discussed.

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Kenyon, Scott J. "Planet Formation in the Outer Solar System." Publications of the Astronomical Society of the Pacific 114, no. 793 (March 2002): 265–83. http://dx.doi.org/10.1086/339188.

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Heiden, David. "Homemade spinner demonstrates formation of solar system." Physics Teacher 38, no. 6 (September 2000): 378. http://dx.doi.org/10.1119/1.1531561.

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Schulz, R. "The Rosetta mission—Exploring solar system formation." Planetary and Space Science 66, no. 1 (June 2012): 1. http://dx.doi.org/10.1016/j.pss.2012.04.001.

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Barr, Amy C. "Formation of exomoons: a solar system perspective." Astronomical Review 12, no. 1-4 (October 2016): 24–52. http://dx.doi.org/10.1080/21672857.2017.1279469.

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ENCRENAZ, THÉRÈSE. "The formation and evolution of the Solar System." European Review 10, no. 2 (May 2002): 171–84. http://dx.doi.org/10.1017/s1062798702000133.

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Astronomers have built the main components of a scenario for the formation of the Solar System. Small planetary bodies accreted others by collisions within a rotating protoplanetary disk that formed at the same time as the Sun. While terrestrial planets near the warming Sun could accumulate only solid metallic and silicate material, the giant planets formed from ice and gas at lower temperatures. Each planet and satellite then followed its own specific evolution, depending upon the properties of its atmosphere and/or surface. Information about the origin and evolution of the Solar System is also provided by the comets, which can be considered as frozen fossils of the Solar System's early stages. On the borders of the outer Solar System, beyond the orbit of Neptune, the newly discovered Edgeworth–Kuiper belt is probably the reservoir where short-period comets are formed.

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Mirzəli qızı Əliyeva, Türkanə, and Vəfa Əjdər qızı Qafarova. "The formation and evolution of the solar system." NATURE AND SCIENCE 03, no. 01 (March 5, 2021): 85–87. http://dx.doi.org/10.36719/2707-1146/06/85-87.

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The article provides extensive information on the formation, evolution and structure of the solar system. It also discusses the planets of the solar system and the dwarf planets. Its noted that the Kuiper objects are the celestial bodies which belongs to the solar system. NASA's New Horizons spacecraft is currently helps studying four objects in the Kuiper belt. There is also talked about TTauri type stars. The article discusses the future transformation of the Sun from a Red Giant to a White Dwarf. Key words: Kuiper Belt, T Tauri Star, Dwarf Planets, Planet X

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Blum, Jürgen, Dorothea Bischoff, and Bastian Gundlach. "Formation of Comets." Universe 8, no. 7 (July 15, 2022): 381. http://dx.doi.org/10.3390/universe8070381.

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Questions regarding how primordial or pristine the comets of the solar system are have been an ongoing controversy. In this review, we describe comets’ physical evolution from dust and ice grains in the solar nebula to the contemporary small bodies in the outer solar system. This includes the phases of dust agglomeration, the formation of planetesimals, their thermal evolution and the outcomes of collisional processes. We use empirical evidence about comets, in particular from the Rosetta Mission to comet 67P/Churyumov–Gerasimenko, to draw conclusions about the possible thermal and collisional evolution of comets.

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Zderic, Alexander, Maria Tiongco, Angela Collier, Heather Wernke, Aleksey Generozov, and Ann-Marie Madigan. "A Lopsided Outer Solar System?" Astronomical Journal 162, no. 6 (December 1, 2021): 278. http://dx.doi.org/10.3847/1538-3881/ac2def.

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Abstract Axisymmetric disks of eccentric orbits in near-Keplerian potentials are unstable and undergo exponential growth in inclination. Recently, Zderic et al. showed that an idealized disk then saturates to a lopsided mode. Here we show, using N-body simulations, that this apsidal clustering also occurs in a primordial Scattered Disk in the outer solar system, which includes the orbit-averaged gravitational influence of the giant planets. We explain the dynamics using Lynden-Bell's mechanism for bar formation in galaxies. We also show surface density and line-of-sight velocity plots at different times during the instability, highlighting the formation of concentric circles and spiral arms in velocity space.

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Zhong, Yini, and Rui Zhong. "Dynamics, Deployment and Retrieval Strategy for Satellite-Sail Transverse Formation with Model Inaccuracy." Aerospace 9, no. 10 (October 14, 2022): 602. http://dx.doi.org/10.3390/aerospace9100602.

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One of the important applications of the space tethered system is formation flying. To satisfy the requirement for interferometry of ground targets by remote-sensing satellites, a new type of tethered solar sail spacecraft has been proposed in recent research. The replacement of subsatellites of conventional tethered satellite systems with solar sail spacecraft allows for a special formation configuration in which the main satellite is in sun-synchronous orbit and the subsolar sail is in displaced orbit. If the solar sail is at the appropriate attitude, the main satellite and the solar sail spacecraft connected by metal tethers could move side by side, hence this formation system is called transverse formation. The relative baseline of this transverse formation system is perpendicular to the ground trajectory of the satellite, effectively solving the problem that the relative baseline of conventional orbital formations varies in a trigonometric cycle. Researchers on the past ignored the mass and elasticity of the tether, and considered the tether just a constraint in the model system. Since the solar sail is generally quite light compared to the other components of the system, the model inaccuracy caused by ignoring the mass of the tether on the dynamic model and control is extremely obvious. This paper investigates the relative dynamics and control of a proposed system during the deployment process with the mass of the tether. Two precise models of satellite-sail systems are established. One is based on the dumbbell model with the mass tether for the tethered satellite system, and the other is on the basis of the beads model of a tethered satellite system. The rigid one is for control design and the flexible one is for dynamic simulation. It is concluded that the length of the tether and attitude angle of the transverse formation configuration can be decoupled and controlled separately. On the basis of the models, a length rate and LQR control law is developed and the control of the deployment and retrieval process of the tethered solar sail system is investigated. Numerical simulations are performed to verify the accuracy of the conclusions.

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Anirban, Ankita. "Modelling the granular details of Solar System formation." Nature Reviews Physics 4, no. 2 (January 26, 2022): 82. http://dx.doi.org/10.1038/s42254-022-00424-8.

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Brown, W. K. "The Supernova Fragmentation Model of Solar System Formation." Publications of the Astronomical Society of the Pacific 98 (November 1986): 1102. http://dx.doi.org/10.1086/131888.

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Brown, W. K., and L. A. Gritzo. "The supernova fragmentation model of solar system formation." Astrophysics and Space Science 123, no. 1 (1986): 161–81. http://dx.doi.org/10.1007/bf00649132.

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Portegies Zwart, S. "The formation of solar-system analogs in young star clusters." Astronomy & Astrophysics 622 (January 30, 2019): A69. http://dx.doi.org/10.1051/0004-6361/201833974.

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The solar system was once rich in the short-lived radionuclide (SLR) 26Al but poor in 60Fe. Several models have been proposed to explain these anomalous abundances in SLRs, but none has been set within a self-consistent framework of the evolution of the solar system and its birth environment. The anomalous abundance in 26Al may have originated from the accreted material in the wind of a massive ≳20 M⊙ Wolf-Rayet star, but the star could also have been a member of the parental star-cluster instead of an interloper or an older generation that enriched the proto-solar nebula. The protoplanetary disk at that time was already truncated around the Kuiper-cliff (at 45 au) by encounters with other cluster members before it was enriched by the wind of the nearby Wolf-Rayet star. The supernova explosion of a nearby star, possibly but not necessarily the exploding Wolf-Rayet star, heated the disk to ≳1500 K, melting small dust grains and causing the encapsulation and preservation of 26Al in vitreous droplets. This supernova, and possibly several others, caused a further abrasion of the disk and led to its observed tilt of 5.6 ± 1.2° with respect to the equatorial plane of the Sun. The abundance of 60Fe originates from a supernova shell, but its preservation results from a subsequent supernova. At least two supernovae are needed (one to deliver 60Fe and one to preserve it in the disk) to explain the observed characteristics of the solar system. The most probable birth cluster therefore has N = 2500 ± 300 stars and a radius of rvir = 0.75 ± 0.25 pc. We conclude that systems equivalent to our solar system form in the Milky Way Galaxy at a rate of about 30 Myr−1, in which case approximately 36 000 solar-system analogs roam the Milky Way.

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Huss, Gary R., and Bruce T. Draine. "What can pre-solar grains tell us about the solar nebula?" Proceedings of the International Astronomical Union 2, no. 14 (August 2006): 353–56. http://dx.doi.org/10.1017/s1743921307010964.

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AbstractSeveral types of pre-solar grains, grains that existed prior to solar system formation, have been found in the fine-grained components of primitive meteorites, interplanetary dust particles (IDPs), and comet samples. Known pre-solar components have isotopic compositions that reflect formation from the ejecta of evolved stars. Other pre-solar materials may have isotopic compositions very similar to solar system materials, making their identification as pre-solar grains problematic. Pre-solar materials exhibit a range of chemical and thermal resistance, so their relative abundances can be used to probe the conditions in the solar nebula. Detailed information on the relative abundances of pre-solar and solar-system materials can provide information on the temperatures, radiation environment, and degree of radial mixing in the early solar system.

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Wei-biao, Hsu. "Short-lived radionuclides in the early solar system — A meteoritic perspective of the solar system formation." Chinese Astronomy and Astrophysics 27, no. 4 (October 2003): 365–73. http://dx.doi.org/10.1016/s0275-1062(03)90060-9.

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Kley, Wilhelm. "Formation and Orbital Evolution of Planets." Proceedings of the International Astronomical Union 7, S282 (July 2011): 429–36. http://dx.doi.org/10.1017/s1743921311027980.

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AbstractThe formation of planetary systems is a natural byproduct of the star formation process. Planets can form inside the protoplanetary disk by two alternative processes. Either through a sequence of sticking collisions, the so-called sequential accretion scenario, or via gravitational instability from an over-dense clump inside the protoplanetary disk. The first process is believed to have occurred in the solar system. The most important steps in this process will be outlined. The observed orbital properties of exoplanetary systems are distinctly different from our own Solar System. In particular, their small distance from the star, their high eccentricity and large mass point to the existence of a phase with strong mutual excitations. These are believed to be a result of early evolution of planets due to planet-disk interaction. The importance of this process in shaping the dynamical structure of planetary systems will be presented.

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Brennecka, Gregory A., Christoph Burkhardt, Gerrit Budde, Thomas S. Kruijer, Francis Nimmo, and Thorsten Kleine. "Astronomical context of Solar System formation from molybdenum isotopes in meteorite inclusions." Science 370, no. 6518 (November 12, 2020): 837–40. http://dx.doi.org/10.1126/science.aaz8482.

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Calcium-aluminum–rich inclusions (CAIs) in meteorites are the first solids to have formed in the Solar System, defining the epoch of its birth on an absolute time scale. This provides a link between astronomical observations of star formation and cosmochemical studies of Solar System formation. We show that the distinct molybdenum isotopic compositions of CAIs cover almost the entire compositional range of material that formed in the protoplanetary disk. We propose that CAIs formed while the Sun was in transition from the protostellar to pre–main sequence (T Tauri) phase of star formation, placing Solar System formation within an astronomical context. Our results imply that the bulk of the material that formed the Sun and Solar System accreted within the CAI-forming epoch, which lasted less than 200,000 years.

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Lichtenberg, Tim, Joanna Dra̧żkowska, Maria Schönbächler, Gregor J. Golabek, and Thomas O. Hands. "Bifurcation of planetary building blocks during Solar System formation." Science 371, no. 6527 (January 22, 2021): 365–70. http://dx.doi.org/10.1126/science.abb3091.

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TACHIBANA, Shogo. "Chondrule formation and evolution of the early solar system." Journal of Mineralogical and Petrological Sciences 101, no. 2 (2006): 37–47. http://dx.doi.org/10.2465/jmps.101.37.

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Woolfson, M. M. "Planet formation and the evolution of the Solar System." Physica Scripta 94, no. 11 (August 21, 2019): 113001. http://dx.doi.org/10.1088/1402-4896/ab1ee1.

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Bailey, Mark E. "Formation of Outer Solar System Bodies: Comets and Planetesimals." Symposium - International Astronomical Union 160 (1994): 443–59. http://dx.doi.org/10.1017/s0074180900046702.

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Observations of massive, extended discs around both pre-main-sequence and main-sequence stellar systems indicate that protoplanetary discs larger than the observed planetary system are a common phenomenon, while the existence of large comets suggests that the total cometary mass is much greater than previous estimates. Both observations suggest that theories of the origin of the solar system are best approached from the perspective provided by theories of star formation, in particular that the protoplanetary disc may have extended up to ~103 AU. A model with a surface density distribution similar to a minimum-mass solar nebula, but extending further in radius, is derived by considering the gravitational collapse of a uniform, slowly rotating molecular cloud. The boundary of the planetary system is determined not by lack of mass, as in previous ‘mass-limited’ models (i.e. those with a sharp decrease in surface density Σ beyond the radius of the observed planetary system), but instead by the increasing collision time between the comets or planetesimals initially formed by gravitational instability beyond the planetary zone. Bodies formed beyond ~50 AU have sizes on the order of 102 km and represent a collisionally unevolved population; they are composed of relatively small, unaltered clumps of interstellar dust and ices with individual sizes estimated to range up to ~10 m. By contrast, bodies formed closer in, for example in the Uranus-Neptune zone, consist of larger agglomerations of dust and ices with individual sizes ranging up to ~1 km. Planetesimals formed by gravitational instability at smaller heliocentric distances r are typically much smaller than those formed further out, the masses mp being proportional to Σ3r6, but subsequent collisional aggregation in the planetary region is expected to produce bodies with sizes ranging up to 102 km or more. In both cases the first-formed solid objects may be identified with observed cometary nuclei; some accumulate to produce the outer planets, but the majority are ejected, either to interstellar space or into the Oort cloud. Observed comets represent a dynamically well-mixed group from various sources; they are expected to comprise a heterogeneous mix of both pristine and relatively altered material and to have a broad mass distribution ranging up to the size of the largest planetesimals.

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Mandt, Kathleen E., Olivier Mousis, Dominique Bockelée-Morvan, and Christopher T. Russell. "Comets as Tracers of Solar System Formation and Evolution." Space Science Reviews 197, no. 1-4 (November 2, 2015): 5–7. http://dx.doi.org/10.1007/s11214-015-0215-2.

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Ruzmaikina, T. V. "Planetesimal formation in the solar nebula." International Astronomical Union Colloquium 173 (1999): 17–30. http://dx.doi.org/10.1017/s0252921100031195.

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AbstractTerrestrial planets, cores of giant planets and small bodies of the solar system − comets and asteroids − resulted from the coagulation of interstellar dust grains, and grains which were melted or evaporated and condensed again in the solar nebula.The paper describes the growth and processing of dust grains and their aggregates, starting from molecular cloud cores through the formation and evolution of the solar nebula and the accumulation of these aggregates in larger solid bodies − planetesimals. Discussed are the processes which could be responsible for the interruption of accumulation in the region of the asteroid belt, and processes which shaped the Kuiper belt.

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Owen, Tobias C., Paul Mahaffy, H. B. Niemann, S. K. Atreya, T. M. Donahue, A. Bar-Nun, and I. de Pater. "Chemistry in the Outer Solar System." Symposium - International Astronomical Union 197 (2000): 483–90. http://dx.doi.org/10.1017/s0074180900165040.

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The discovery by the Galileo Probe Mass Spectrometer that argon is enriched to the same extent as carbon and sulfur on Jupiter requires a revision of models for the formation of this giant planet. Evidently the excess heavy elements were carried to Jupiter in icy planetesimals that formed at temperatures ≤ 30 K. This result indicates that there is no original significance in the present position of Jupiter's orbit.

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Khoiriyah, Khilyatul. "Evolusi Bintang pada Pembentukan Tata Surya dan Sistem Keplanetan." Jurnal Ilmiah Pendidikan Fisika Al-Biruni 5, no. 2 (October 26, 2016): 245. http://dx.doi.org/10.24042/jpifalbiruni.v5i2.124.

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This research is the literature studies that provide an introduction to the theory of the formation and early evolution of solar system and planetary systems. Theories that discussed are limit on the theory which has been closed to the truth of observation result. Topics include the structure of solar system, star formation, the structure of evolution and dispersal of protoplanetary disks, planetesimals formation, terrestrial and giant planets formation, the formation of the smaller objects in the solar system and planet migration.Penelitian ini merupakan studi literatur yang membahas tentang masalah pembentukan dan evolusi awal tata surya dan sistem keplanetan dengan memberikan konsep dasar yang ringkas. Teori-teori yang dikaji secara khusus dibatasi pada teori yang telah mendekati kebenaran dari hasil pengamatan. Topik yang dibahas adalah struktur tata surya, pembentukan bintang, struktur evolusi dan pembubaran cakram protoplanet, pembentukan planetesimal, planet terestrial dan planet raksasa, pembentukan benda-benda kecil dalam tata surya dan migrasi planet.

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Bockelee-Morvan, Dominique. "Water in small bodies of the Solar System." Proceedings of the International Astronomical Union 11, A29B (August 2015): 401. http://dx.doi.org/10.1017/s1743921316005640.

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AbstractWater in form of ice or vapour is observed in comets, transneptunian objects and icy satellites formed in the outer regions of the Solar System, as well as in objects orbiting in the inner Solar System, such as dwarf planet Ceres. I will present an overview of the water content and properties in these objects and the implications in terms of solar system formation and evolution.

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Wuchterl, Günther. "Giant planet formation — a theoretical timeline." Symposium - International Astronomical Union 202 (2004): 167–74. http://dx.doi.org/10.1017/s0074180900217750.

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Low mass circumstellar disks are a result of the star formation process. The growth of dust and solid planets in such pre-planetary disks determines many properties of our solar system. Models of the Solar System giant planets indicate an enrichment of heavy elements and imply heavy element cores. Detailed models therefore describe giant planet formation as a consequence of the formation of solid planets that have grown sufficiently large to permanently bind gas from the protoplanetary nebula. The diversity of Solar System and extrasolar giant planets is explained by variations in the core growth rates caused by a coupling of the dynamics of planetesimals and the contraction of the massive envelopes they dive into, as well as by changes in the hydrodynamical accretion behavior of the envelopes resulting from differences in nebula density, temperature and orbital distance. Detailed formation models are able to determine observables as luminosities, radii and effective temperatures of young giant planets. Present observational techniques do now allow to probe star formation regions at ages covering all evolutionary stages of the giant planet formation process.

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Lin, D. N. C. "Planetary Formation in Protostellar Disks." International Astronomical Union Colloquium 163 (1997): 321–30. http://dx.doi.org/10.1017/s0252921100042792.

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AbstractRecent discoveries of planets around other stars suggest that planets are ubiquitous and their dynamical properties are diverse. We reviewed the formation mechanism for protoplanets and the post-formation planet-disk tidal interaction which may have led the short-period planets to their present configuration. We suggest that these planets may be the survivors of a populations of similar planets which have plunged into and contaminated the stellar convection zone. In the context of the solar system, the mass of the giant planets and the present distribution of the minor planets may be used to infer the structure and evolution for the primordial solar nebula. The large eccentricity of 70 Vir and HD 114762 may be due to cohesive collisions in planetary systems which become unstable during their long term orbital evolution.

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Hamouda, Samir A., Eman A. Alsslam Alfadeel, and Mohamed Belhasan Mohamed. "PLANETARY MAGNETIC FIELD AND GRAVITY IN THE SOLAR SYSTEM." International Journal of Research -GRANTHAALAYAH 5, no. 9 (September 30, 2017): 145–51. http://dx.doi.org/10.29121/granthaalayah.v5.i9.2017.2224.

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Gravity plays a major role in the planetary formation and the development of the solar system. Gravity attraction is the essence of a power that holds and governs the universe; it makes the planets in the solar system revolve around the sun and the moons around their planets. Magnetic fields are also an important phenomenon in the solar system and beyond. Their causes are complex and have a variety of effects on their surroundings; they have become a critical tool for the exploration of solar system bodies. However, the study of the mechanisms of planets formation in the solar system is a difficult problem made more so by the inability to construct planetary-scale models for laboratory study. However, understanding the nature of the matter comprising the Solar System is crucial for understanding the mechanism that generates planetary magnetic fields and planetary gravity. In this study, a brief history about the development of planetary gravity is presented. Some data about the physical properties of planets in the solar system are presented and discussed. However, much work is still needed before the planetary gravity and planetary magnetic field processes are fully understood and full advantage be taken of the implications of both phenomena observations.

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Kawai, Toshio. "Pattern Formation by Inelastic Collisions, Especially in Planetary Systems." International Journal of Modern Physics B 12, no. 03 (January 30, 1998): 309–60. http://dx.doi.org/10.1142/s0217979298000247.

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The Titius–Bode law governs the planet distribution in our Solar system. In this paper a possible explanation is proposed based on inelastic collision effects among planetessimals during the evolution of the Solar system. The main purpose of this paper is, however, to introduce a strategy to study phenomena driven by rare but drastic events such as colllisions in the planetary problem. Many complex systems evolve through rare but violent events, so that an efficient strategy to simulate such systems is desirable. An event-driven strategy is proposed in this article, and is used to produce many runs of 108 year evolution history of planetary systems. I have found that the Titius–Bode law holds approximately, if the gravitational effect (scattering) and the collisions are taken into account. The result illustrates the importance of inelastic collisions, which are often neglected in the standard classical mechanics courses. Therefore, for completeness, other simpler particle systems under the effect of inelastc collisions, such as one-dimensional systems, are also included.

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Coleman, Les. "Additional Solar System Gravitational Anomalies." Symmetry 13, no. 9 (September 14, 2021): 1696. http://dx.doi.org/10.3390/sym13091696.

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This article is motivated by uncertainty in experimental determinations of the gravitational constant, G, and numerous anomalies of up to 0.5 percent in Newtonian gravitational force on bodies within the solar system. The analysis sheds new light through six natural experiments within the solar system, which draw on published reports and astrophysical databases, and involve laboratory determinations of G, orbital dynamics of the planets and the moons of Earth and Mars, and non-gravitational acceleration (NGA) of ‘Oumuamua and comets. In each case, values are known for all variables in Newton’s Law , except for the gravitational constant, G. Analyses determine the gravitational constant’s observed value, , which—across the six settings—varies with the mass of the smaller, moving body, m, so that . While further work is required, this examination shows a scale-related Newtonian gravity effect at scales from benchtop to Solar System, which contributes to the understanding of symmetry in gravity and has possible implications for Newton’s Laws, dark matter, and formation of structure in the universe.

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Herndon, J. Marvin. "Making Sense of Chondrite Meteorites." Advances in Social Sciences Research Journal 9, no. 2 (February 13, 2022): 82–102. http://dx.doi.org/10.14738/assrj.92.11808.

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I describe the simplification of multitudes of complex data on hundreds of chondrite meteorites to obtain a fundamental relationship that underlies processes during solar system formation. From the relationship derived, generally, it can be concluded that only three processes, operant during solar system formation, are responsible for the diversity of matter in the solar system, as well as for planetary compositions , internal-structures, dynamics and magnetics: (1) Condensation at very high-pressures; (2) Condensation at very low-pressures; and (3) Scouring of the inner solar system by the T-Tauri eruptions during thermonuclear ignition of the sun.

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Russell, Sara S. "The Formation of the Solar System: A Recipe for Worlds." Elements 14, no. 2 (April 1, 2018): 113–18. http://dx.doi.org/10.2138/gselements.14.2.113.

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Duncan, M., T. Quinn, and S. Tremaine. "The formation and extent of the solar system comet cloud." Astronomical Journal 94 (November 1987): 1330. http://dx.doi.org/10.1086/114571.

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Bochkarev, Vladimir S. "Model of fireworks formation of the Earth and Solar system." Geosfernye issledovaniya, no. 4 (December 1, 2017): 58–63. http://dx.doi.org/10.17223/25421379/5/5.

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Gritschneder, M., D. N. C. Lin, S. D. Murray, Q. Z. Yin, and M. N. Gong. "THE SUPERNOVA TRIGGERED FORMATION AND ENRICHMENT OF OUR SOLAR SYSTEM." Astrophysical Journal 745, no. 1 (December 28, 2011): 22. http://dx.doi.org/10.1088/0004-637x/745/1/22.

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

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