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Journal articles on the topic 'Formation and evolution of planetary systems'

Author: Grafiati

Published: 8 June 2024

Last updated: 31 July 2025

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1

Burke, Bernard F. "Planetary systems: Formation, evolution, and detection - introduction." Astrophysics and Space Science 212, no. 1-2 (1994): xi—xii. http://dx.doi.org/10.1007/bf00984502.

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Horedt, G. P. "The Formation and evolution of planetary systems." Physics of the Earth and Planetary Interiors 67, no. 3-4 (1991): 392–94. http://dx.doi.org/10.1016/0031-9201(91)90035-g.

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3

Owen, Tobias. "The formation and evolution of planetary systems." Icarus 91, no. 2 (1991): 334–35. http://dx.doi.org/10.1016/0019-1035(91)90029-s.

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Lipschutz, Michael E. "The formation and evolution of planetary systems." Geochimica et Cosmochimica Acta 54, no. 4 (1990): 1196. http://dx.doi.org/10.1016/0016-7037(90)90455-t.

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5

Kley, Wilhelm. "Formation and Orbital Evolution of Planets." Proceedings of the International Astronomical Union 7, S282 (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 pa

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Veras, Dimitri. "Post-main-sequence planetary system evolution." Royal Society Open Science 3, no. 2 (2016): 150571. http://dx.doi.org/10.1098/rsos.150571.

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The fates of planetary systems provide unassailable insights into their formation and represent rich cross-disciplinary dynamical laboratories. Mounting observations of post-main-sequence planetary systems necessitate a complementary level of theoretical scrutiny. Here, I review the diverse dynamical processes which affect planets, asteroids, comets and pebbles as their parent stars evolve into giant branch, white dwarf and neutron stars. This reference provides a foundation for the interpretation and modelling of currently known systems and upcoming discoveries.

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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 u

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Cuello, Nicolás, Antoine Alaguero, and Pedro P. Poblete. "Circumstellar and Circumbinary Discs in Multiple Stellar Systems." Symmetry 17, no. 3 (2025): 344. https://doi.org/10.3390/sym17030344.

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The interplay between stellar multiplicity and protoplanetary discs represents a cornerstone of modern astrophysics, offering key insights into the processes behind planet formation. Protoplanetary discs act as cradles for planetary systems, yet their evolution and capacity to form planets are profoundly affected by gravitational forces within multiple stellar systems. This review synthesizes recent advancements in observational and theoretical studies to explore the rich diversity of circumstellar and circumbinary discs within multiple stellar systems. We examine how stellar companions shape

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Marzari, Francesco, and Philippe Thebault. "Planets in Binaries: Formation and Dynamical Evolution." Galaxies 7, no. 4 (2019): 84. http://dx.doi.org/10.3390/galaxies7040084.

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Binary systems are very common among field stars, yet the vast majority of known exoplanets have been detected around single stars. While this relatively small number of planets in binaries is probably partly due to strong observational biases, there is, however, statistical evidence that planets are indeed less frequent in binaries with separations smaller than 100 au, strongly suggesting that the presence of a close-in companion star has an adverse effect on planet formation. It is indeed possible for the gravitational pull of the second star to affect all the different stages of planet form

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Kawai, Toshio. "Pattern Formation by Inelastic Collisions, Especially in Planetary Systems." International Journal of Modern Physics B 12, no. 03 (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

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Salnikova, T. V., S. Ya Stepanov, and E. I. Kugushev. "Possible models of the planetary systems formations." International Journal of Modern Physics A 35, no. 02n03 (2020): 2040061. http://dx.doi.org/10.1142/s0217751x20400618.

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We discuss extended model of planetary system formation. Gravitational collapse of protoplanets leads to the formation of planets and their satellite systems. We consider the hypothesis of a two-stage mechanism of formation of satellite system. Small satellites are formed from the remnants of a collapsing protoplanetary cloud, and large satellites are formed by capturing other relatively small protoplanets. In this paper we study the process of formation of the initial gas-dust cloud, whose evolution leads to the formation of a protoplanetary, and then a planetary system. The justification of

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12

Meyer, Michael R. "Circumstellar disk evolution: Constraining theories of planet formation." Proceedings of the International Astronomical Union 4, S258 (2008): 111–22. http://dx.doi.org/10.1017/s1743921309031767.

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AbstractObservations of circumstellar disks around stars as a function of stellar properties such as mass, metallicity, multiplicity, and age, provide constraints on theories concerning the formation and evolution of planetary systems. Utilizing ground- and space-based data from the far–UV to the millimeter, astronomers can assess the amount, composition, and location of circumstellar gas and dust as a function of time. We review primarily results from the Spitzer Space Telescope, with reference to other ground- and space-based observations. Comparing these results with those from exoplanet se

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13

Wang, Su, and Jianghui Ji. "The Configuration Formation of Planetary Systems Observed by Kepler." Proceedings of the International Astronomical Union 8, S293 (2012): 106–9. http://dx.doi.org/10.1017/s1743921313012635.

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AbstractThe Kepler mission has found many planetary systems, among them more than 80 systems host three planet candidates which reveal a configuration of near 4:2:1 mean motion resonance. In this paper, we focus on the configuration formation of resonant systems. As shown from our model and N-body simulations, we find that 3:2 mean motion resonance always forms at the early stage of star evolution and planets undergo high rate of migration, while 2:1 mean motion resonance happens at the late stage of the star formation, more often.

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Andrews, Sean M. "Radio Interferometry Observations of the Hallmarks of Planet Formation." Proceedings of the International Astronomical Union 8, S299 (2013): 80–89. http://dx.doi.org/10.1017/s1743921313007977.

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AbstractSome of the fundamental processes involved in the evolution of circumstellar disks and the assembly of planetary systems are just now becoming accessible to astronomical observations. The new promise of observational work in the field of planet formation makes for a very dynamic research scenario, which is certain to be amplified in the coming years as the revolutionary Atacama Large Millimeter/submillimeter Array (ALMA) facility ramps up to full operations. To highlight the new directions being explored in these fields, this brief review will describe how high angular resolution measu

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Emsenhuber, Alexandre, Christoph Mordasini, Remo Burn, Yann Alibert, Willy Benz, and Erik Asphaug. "The New Generation Planetary Population Synthesis (NGPPS)." Astronomy & Astrophysics 656 (December 2021): A70. http://dx.doi.org/10.1051/0004-6361/202038863.

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Context. Planetary formation and evolution is a combination of multiple interlinked processes. Constraining the mechanisms observationally requires statistical comparison to a large diversity of planetary systems. Aims. We want to understand global observable consequences of different physical processes (accretion, migration, and interactions) and initial properties (like disc masses and metallicities) on the demographics of the planetary population. We also want to study the convergence of our scheme with respect to one initial condition, the initial number of planetary embryo in each disc. M

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16

LePoire, David. "Geological Complexity: Bridging Cosmic Evolution and the Evolution of Life." Journal of Big History 8, no. 1 (2025): 45–50. https://doi.org/10.22339/jbh.v8i1.8107.

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Earth occupies a unique position in Big History as a bridge between cosmic evolution and the rise of complex life. While discussions often emphasize monumental events like the Big Bang or the rise of civilizations, the intermediate phase of planetary formation and life’s emergence reveals the intricate interplay of cosmic, geological, and biological processes. Earth’s development—from the chaotic dynamics of the early solar system, including the Moon-forming collision, to the establishment of a protective magnetic field and diverse energy gradients—created the conditions necessary for life to

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Zhou, J. L. "Formation and tidal evolution of hot super-Earths in multiple planetary systems." EAS Publications Series 42 (2010): 255–66. http://dx.doi.org/10.1051/eas/1042027.

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18

Lewis, K. "Moon formation and orbital evolution in extrasolar planetary systems - A literature review." EPJ Web of Conferences 11 (2011): 04003. http://dx.doi.org/10.1051/epjconf/20101104003.

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Lewis, K. "Moon formation and orbital evolution in extrasolar planetary systems - A literature review." EPJ Web of Conferences 11 (2011): 04003. http://dx.doi.org/10.1051/epjconf/20111104003.

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Carpenter, John M., Jeroen Bouwman, Murray D. Silverstone, et al. "The Formation and Evolution of Planetary Systems: Description of theSpitzerLegacy Science Database." Astrophysical Journal Supplement Series 179, no. 2 (2008): 423–50. http://dx.doi.org/10.1086/592274.

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21

Chew, Yilen Gómez Maqueo, Francesca Faedi, Leslie Hebb, et al. "The HoSTS Project: A Homogeneous Study of Transiting Systems." Proceedings of the International Astronomical Union 8, S299 (2013): 285–86. http://dx.doi.org/10.1017/s1743921313008612.

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AbstractThe Homogeneous Study of Transiting Systems (HoSTS) will derive a consistent and homogeneous set of both the stellar and planetary physical properties for a large sample of bright transiting planetary systems with confirmed planetary masses and measured radii. Our resulting catalogs of the fundamental properties of these bright planets and their host stars will enable us to explore empirical correlations that will lead to a better understanding of planetary formation and evolution. We present our pilot study of the planet-hosting star WASP-13, and the framework of our project which wil

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Ercolano, Barbara, and Ilaria Pascucci. "The dispersal of planet-forming discs: theory confronts observations." Royal Society Open Science 4, no. 4 (2017): 170114. http://dx.doi.org/10.1098/rsos.170114.

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Discs of gas and dust around million-year-old stars are a by-product of the star formation process and provide the raw material to form planets. Hence, their evolution and dispersal directly impact what type of planets can form and affect the final architecture of planetary systems. Here, we review empirical constraints on disc evolution and dispersal with special emphasis on transition discs, a subset of discs that appear to be caught in the act of clearing out planet-forming material. Along with observations, we summarize theoretical models that build our physical understanding of how discs

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23

Baruteau, Clément, Xuening Bai, Christoph Mordasini, and Paul Mollière. "Formation, Orbital and Internal Evolutions of Young Planetary Systems." Space Science Reviews 205, no. 1-4 (2016): 77–124. http://dx.doi.org/10.1007/s11214-016-0258-z.

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Bouvier, J., G. Duchêne, J. C. Mermilliod, and T. Simon. "The formation and evolution of binary systems." Astronomy & Astrophysics 375, no. 3 (2001): 989–98. http://dx.doi.org/10.1051/0004-6361:20010915.

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25

Turrini, D., A. Zinzi, and J. A. Belinchon. "Normalized angular momentum deficit: a tool for comparing the violence of the dynamical histories of planetary systems." Astronomy & Astrophysics 636 (April 2020): A53. http://dx.doi.org/10.1051/0004-6361/201936301.

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Context. Population studies of the orbital characteristics of exoplanets in multi-planet systems have highlighted the existence of an anticorrelation between the average orbital eccentricity of planets and the number of planets of their host system, that is, its multiplicity. This effect was proposed to reflect the varying levels of violence in the dynamical evolution of planetary systems. Aims. Previous work suggested that the relative violence of the dynamical evolution of planetary systems with similar orbital architectures can be compared through the computation of their angular momentum d

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Parker, Richard J., and Emma C. Daffern-Powell. "Making BEASTies: dynamical formation of planetary systems around massive stars." Monthly Notices of the Royal Astronomical Society: Letters 516, no. 1 (2022): L91—L95. http://dx.doi.org/10.1093/mnrasl/slac086.

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ABSTRACT Exoplanets display incredible diversity, from planetary system architectures around Sun-like stars that are very different from our Solar system, to planets orbiting post-main-sequence stars or stellar remnants. Recently, the B-star Exoplanet Abundance STudy (BEAST) reported the discovery of at least two super-Jovian planets orbiting massive stars in the Sco Cen OB association. Whilst such massive stars do have Keplerian discs, it is hard to envisage gas giant planets being able to form in such hostile environments. We use N-body simulations of star-forming regions to show that these

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Batygin, K., A. Morbidelli, and K. Tsiganis. "Formation and evolution of planetary systems in presence of highly inclined stellar perturbers." Astronomy & Astrophysics 533 (August 12, 2011): A7. http://dx.doi.org/10.1051/0004-6361/201117193.

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28

Hands, Thomas O., Richard D. Alexander, and Walter Dehnen. "Understanding the assembly of Kepler's tightly-packed planetary systems." Proceedings of the International Astronomical Union 9, S310 (2014): 90–92. http://dx.doi.org/10.1017/s1743921314007935.

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AbstractThe Kepler mission has recently discovered a number of exoplanetary systems, such as Kepler 11, in which ensembles of several planets are found in very closely packed orbits. These systems present a challenge for traditional formation and migration scenarios. We present a dynamical study of the evolution of these systems using an N-body approach, incorporating both smooth and stochastic migration forces and a variety of initial conditions, in order to assess the feasibility of assembling such systems via traditional, disc-driven migration.

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Haghighipour, Nader. "Habitable planet formation in extreme planetary systems: systems with multiple stars and/or multiple planets." Proceedings of the International Astronomical Union 3, S249 (2007): 319–24. http://dx.doi.org/10.1017/s1743921308016773.

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AbstractUnderstanding the formation and dynamical evolution of habitable planets in extrasolar planetary systems is a challenging task. In this respect, systems with multiple giant planets and/or multiple stars present special complications. The formation of habitable planets in these environments is strongly affected by the dynamics of their giant planets and/or their stellar companions. These objects have profound effects on the structure of the disk of planetesimals and protoplanetary objects in which terrestrial-class planets are formed. To what extent the current theories of planet format

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Sandford, Emily, David Kipping, and Michael Collins. "On planetary systems as ordered sequences." Monthly Notices of the Royal Astronomical Society 505, no. 2 (2021): 2224–46. http://dx.doi.org/10.1093/mnras/stab1480.

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ABSTRACT A planetary system consists of a host star and one or more planets, arranged into a particular configuration. Here, we consider what information belongs to the configuration, or ordering, of 4286 Kepler planets in their 3277 planetary systems. First, we train a neural network model to predict the radius and period of a planet based on the properties of its host star and the radii and period of its neighbours. The mean absolute error (MAE) of the predictions of the trained model is a factor of 2.1 better than the MAE of the predictions of a naive model that draws randomly from dynamica

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Zhu, Wei, and Subo Dong. "Exoplanet Statistics and Theoretical Implications." Annual Review of Astronomy and Astrophysics 59, no. 1 (2021): 291–336. http://dx.doi.org/10.1146/annurev-astro-112420-020055.

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In the past few years, significant advances have been made in understanding the distributions of exoplanet populations and the architecture of planetary systems. We review the recent progress of planet statistics, with a focus on the inner ≲1-AU region of planetary systems that has been fairly thoroughly surveyed by the Kepler mission. We also discuss the theoretical implications of these statistical results for planet formation and dynamical evolution.

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Izidoro, André, Bertram Bitsch, Sean N. Raymond, et al. "Formation of planetary systems by pebble accretion and migration." Astronomy & Astrophysics 650 (June 2021): A152. http://dx.doi.org/10.1051/0004-6361/201935336.

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At least 30% of main sequence stars host planets with sizes of between 1 and 4 Earth radii and orbital periods of less than 100 days. We use N-body simulations including a model for gas-assisted pebble accretion and disk–planet tidal interaction to study the formation of super-Earth systems. We show that the integrated pebble mass reservoir creates a bifurcation between hot super-Earths or hot-Neptunes (≲15 M⊕) and super-massive planetary cores potentially able to become gas giant planets (≳15 M⊕). Simulations with moderate pebble fluxes grow multiple super-Earth-mass planets that migrate inwa

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Boyle, L. A., and M. P. Redman. "Planet destruction and the shaping of planetary nebulae." Proceedings of the International Astronomical Union 12, S323 (2016): 193–96. http://dx.doi.org/10.1017/s1743921317000539.

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AbstractThe shaping of PNe as a result of an interaction with a planet is a hypothesis that has been suggested for nearly two decades. However, exploring the idea observationally is challenging due to the lack of capabilities needed to detect any evidence of such a scenario. Nonetheless, we propose that the hypothesis can be indirectly tested via a combination of exoplanet formation and evolution theories, the star and planet formation histories of the galaxy and the tidal evolution of star-planet systems. We present a calculation of the fraction of planetary nebulae in the galaxy today which

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Lambrechts, Michiel, Alessandro Morbidelli, Seth A. Jacobson, et al. "Formation of planetary systems by pebble accretion and migration." Astronomy & Astrophysics 627 (July 2019): A83. http://dx.doi.org/10.1051/0004-6361/201834229.

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Super-Earths – planets with sizes between the Earth and Neptune – are found in tighter orbits than that of the Earth around more than one third of main sequence stars. It has been proposed that super-Earths are scaled-up terrestrial planets that also formed similarly, through mutual accretion of planetary embryos, but in discs much denser than the solar protoplanetary disc. We argue instead that terrestrial planets and super-Earths have two clearly distinct formation pathways that are regulated by the pebble reservoir of the disc. Through numerical integrations, which combine pebble accretion

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Ciesla, Fred J. "Chemical evolution of planetary materials in a dynamic solar nebula." Proceedings of the International Astronomical Union 15, S350 (2019): 152–57. http://dx.doi.org/10.1017/s1743921319009499.

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AbstractAs observational facilities improve, providing new insights into the chemistry occurring in protoplanetary disks, it is important to develop more complete pictures of the processes that shapes the chemical evolution of materials during this stage of planet formation. Here we describe how primitive meteorites in our own Solar System can provide insights into the processes that shaped planetary materials early in their evolution around the Sun. In particular, we show how this leads us to expect protoplanetary disks to be very dynamic objects and what modeling and laboratory studies are n

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Ceccarelli, Cecilia, and Fujun Du. "We Drink Good 4.5-Billion-Year-Old Water." Elements 18, no. 3 (2022): 155–60. http://dx.doi.org/10.2138/gselements.18.3.155.

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Water is crucial for the emergence and evolution of life on Earth. Recent studies of the water content in early forming planetary systems similar to our own show that water is an abundant and ubiquitous molecule, initially synthesized on the surfaces of tiny interstellar dust grains by the hydrogenation of frozen oxygen. Water then enters a cycle of sublimation/freezing throughout the successive phases of planetary system formation, namely, hot corinos and protoplanetary disks, eventually to be incorporated into planets, asteroids, and comets. The amount of heavy water measured on Earth and in

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Poon, Sanson T. S., Richard P. Nelson, and Gavin A. L. Coleman. "In situ formation of hot Jupiters with companion super-Earths." Monthly Notices of the Royal Astronomical Society 505, no. 2 (2021): 2500–2516. http://dx.doi.org/10.1093/mnras/stab1466.

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ABSTRACT Observations have confirmed the existence of multiple-planet systems containing a hot Jupiter and smaller planetary companions. Examples include WASP-47, Kepler-730, and TOI-1130. We examine the plausibility of forming such systems in situ using N-body simulations that include a realistic treatment of collisions, an evolving protoplanetary disc, and eccentricity/inclination damping of planetary embryos. Initial conditions are constructed using two different models for the core of the giant planet: a ‘seed-model’ and an ‘equal-mass-model’. The former has a more massive protoplanet plac

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Urrutia-Fucugauchi, Jaime, and Ligia Pérez-Cruz. "Planetary Sciences, Geodynamics, Impacts, Mass Extinctions, and Evolution: Developments and Interconnections." International Journal of Geophysics 2016 (2016): 1–13. http://dx.doi.org/10.1155/2016/4703168.

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Research frontiers in geophysics are being expanded, with development of new fields resulting from technological advances such as the Earth observation satellite network, global positioning system, high pressure-temperature physics, tomographic methods, and big data computing. Planetary missions and enhanced exoplanets detection capabilities, with discovery of a wide range of exoplanets and multiple systems, have renewed attention to models of planetary system formation and planet’s characteristics, Earth’s interior, and geodynamics, highlighting the need to better understand the Earth system,

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Tolasa, Diriba, and Adugna Furi. "Exoplanets and Their Characterization in the Environment of Galaxy Formation." American Journal of Astronomy and Astrophysics 12, no. 1 (2025): 21–27. https://doi.org/10.11648/j.ajaa.20251201.13.

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The exploration of exoplanets has become a crucial domain in astrophysics, particularly in understanding their formation and evolution within the broader framework of galaxy formation. This paper offers a comprehensive analysis of the current methodologies employed for exoplanet detection and characterization, highlighting the intricate relationships between galactic dynamics and planetary systems. We introduce an innovative approach that integrates numerical simulations with analytical models to investigate how various galactic environments influence the properties of exoplanets. Our findings

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McMillan, Stephen L. W., P. N. McDermott, and Ronald E. Taam. "The formation and evolution of tidal binary systems." Astrophysical Journal 318 (July 1987): 261. http://dx.doi.org/10.1086/165365.

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Krot, Alexander M. "On the Analytical Models of Protoplanetary Formation in Extrasolar Systems." Space: Science & Technology 2022 (November 12, 2022): 1–19. http://dx.doi.org/10.34133/2022/9862389.

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In this work, we consider a statistical theory for a cosmogonical body formation (so-called spheroidal body) to develop the analytical models of protoplanetary formation in extrasolar systems. Within the framework of this theory, the models and evolution equations of the statistical mechanics have been proposed, while the well-known problem of gravitational condensation of infinite distributed cosmic substances has been solved. This paper derives the general equation of distribution of the specific angular momentum of forming protoplanets since the specific angular momentums (for particles or

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Meyer, Michael R., Lynne A. Hillenbrand, Dana Backman, et al. "The Formation and Evolution of Planetary Systems: Placing Our Solar System in Context withSpitzer." Publications of the Astronomical Society of the Pacific 118, no. 850 (2006): 1690–710. http://dx.doi.org/10.1086/510099.

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Kim, Jinyoung Serena, Dean C. Hines, Dana E. Backman, et al. "Formation and Evolution of Planetary Systems: Cold Outer Disks Associated with Sun‐like Stars." Astrophysical Journal 632, no. 1 (2005): 659–69. http://dx.doi.org/10.1086/432863.

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Carpenter, John M., Jeroen Bouwman, Eric E. Mamajek, et al. "FORMATION AND EVOLUTION OF PLANETARY SYSTEMS: PROPERTIES OF DEBRIS DUST AROUND SOLAR-TYPE STARS." Astrophysical Journal Supplement Series 181, no. 1 (2009): 197–226. http://dx.doi.org/10.1088/0067-0049/181/1/197.

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45

Absil, Olivier, and Dimitri Mawet. "Formation and evolution of planetary systems: the impact of high-angular resolution optical techniques." Astronomy and Astrophysics Review 18, no. 3 (2009): 317–82. http://dx.doi.org/10.1007/s00159-009-0028-y.

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46

Bonfanti, A., L. Fossati, D. Kubyshkina, and P. E. Cubillos. "Constraining stellar rotation and planetary atmospheric evolution of a dozen systems hosting sub-Neptunes and super-Earths." Astronomy & Astrophysics 656 (December 2021): A157. http://dx.doi.org/10.1051/0004-6361/202142010.

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Context. Planetary atmospheric evolution modelling is a prime tool for understanding the observed exoplanet population and constraining formation and migration mechanisms, but it can also be used to study the evolution of the activity level of planet hosts. Aims. We constrain the planetary atmospheric mass fraction at the time of the dispersal of the protoplanetary disk and the evolution of the stellar rotation rate for a dozen multi-planet systems that host sub-Neptunes and/or super-Earths. Methods. We employ a custom-developed PYTHON code that we have dubbed PASTA (Planetary Atmospheres and

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Jiang, Jonathan H., Remo Burn, Xuan Ji, Kristen A. Fahy, and Patrick Eggenberger. "Angular Momentum Distributions for Observed and Modeled Exoplanetary Systems." Astrophysical Journal 924, no. 2 (2022): 118. http://dx.doi.org/10.3847/1538-4357/ac3242.

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Abstract The distribution of angular momentum of planets and their host stars provides important information on the formation and evolution of the planetary system. However, mysteries still remain, partly due to bias and uncertainty of the current observational data sets and partly due to the fact that theoretical models for the formation and evolution of planetary systems are still underdeveloped. In this study, we calculate the spin angular momentum of host stars and the orbital angular momentum of their planets using data from the NASA Exoplanet Archive along with detailed analysis of obser

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Espinoza-Retamal, Juan I., Wei Zhu, and Cristobal Petrovich. "Prospects from TESS and Gaia to Constrain the Flatness of Planetary Systems." Astronomical Journal 166, no. 6 (2023): 231. http://dx.doi.org/10.3847/1538-3881/ad00b9.

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Abstract The mutual inclination between planets orbiting the same star provides key information to understand the formation and evolution of multiplanet systems. In this work, we investigate the potential of Gaia astrometry in detecting and characterizing cold Jupiters in orbits exterior to the currently known Transiting Exoplanet Survey Satellite (TESS) planet candidates. According to our simulations, out of the ∼3350 systems expected to have cold Jupiter companions, Gaia, by its nominal 5 yr mission, should be able to detect ∼200 cold Jupiters and measure the orbital inclinations with a prec

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Andrews, Michael, and Nader Haghighipour. "Secular Resonances and Terrestrial Planet Formation in Planetary Systems with Multiple Stars." Proceedings of the International Astronomical Union 18, S382 (2022): 116–22. http://dx.doi.org/10.1017/s1743921323004830.

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AbstractWe present the results of a study of secular resonances in a binary star system and their effects on the formation of terrestrial planets. The systems of our interest are binaries with moderate separations (i.e., smaller than 40 AU) where planets revolve around one of the stars. Using numerical simulations, we demonstrate the appearance and evolution of secular resonances in systems with two giant planets. Results indicate that the perturbation of the binary companion suppresses secular resonances and they do not play a significant role on the formation and orbital architecture of terr

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An, Dong-Sheng, Ji-Wei Xie, Yuan-Zhe Dai, and Ji-Lin Zhou. "Planetary Orbit Eccentricity Trends (POET). I. The Eccentricity–Metallicity Trend for Small Planets Revealed by the LAMOST–Gaia–Kepler Sample." Astronomical Journal 165, no. 3 (2023): 125. http://dx.doi.org/10.3847/1538-3881/acb533.

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Abstract Orbital eccentricity is one of the basic planetary properties, whose distribution may shed light on the history of planet formation and evolution. Here, in a series of works on Planetary Orbit Eccentricity Trends (dubbed POET), we study the distribution of planetary eccentricities and their dependence on stellar/planetary properties. In this paper, the first work of the POET series, we investigate whether and how the eccentricities of small planets depend on stellar metallicities (e.g., [Fe/H]). Previous studies on giant planets have found a significant correlation between planetary e

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