Theories of the origin of the solar system 1956- 1985

Brush, Stephen G.

doi:10.1103/revmodphys.62.43

Cited by 26 publications

(8 citation statements)

References 512 publications

(370 reference statements)

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“…One of the main questions in the latest stages of the formation processes in this nebula is how tiny grains of condensed material collide and accumulate into increasingly larger bodies and, finally, into a few large planetarysized objects. It is in the details of the proposed collective processes that the various models depart from one another (Brush, 1990).…”

Section: Introductionmentioning

confidence: 99%

Secular ring instability in the protoplanetary accretion disk

Willerding

1992

Earth Moon Planet

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The aim of the present paper is to show that an accretion disk, the material of which satisfies the Navier-Stokes equations of a compressible fluid, is secularly unstable to axisymmetric density disturbances even if Toomre's parameter Q is greater than one. This instability process, which can also be interpreted as negative diffusion, leads immediately to the formation of rings in the accretion disk as an intermediate step in the formation of planets, at least for the outer gaseous ones. We believe that the same process is also responsible for the ringlet-structure of planetary rings. Only a dynamical instability of axisymmetric density wave perturbations, represented by Toomre's condition Q < 1, does not exist in a viscous self-gravitating disk. On the base of a local theory we calculate the characteristic wave number and the corresponding time scale of the mode of maximum secular instability. In the global theory, we formulate a complex linear integral equation describing the diffusion instability in the accretion disk. The radial distances of the rings to the protosun obey in the outer range of the disk an exponential law provided that the quantity vo (the vertically integrated viscosity) is nearly constant throughout the disk. Our treatment gives arguments in favour for the result, that the spacing ratio 4 = r,,+I/r,, between two consecutive protoplanetary orbits is approximately given by the formula CJ = exp(2r+r"), where p is close to the ratio of the accreted ring-masses in the disk and the mass of the central body. We believe that the formation process is shorter for the outer gaseous than for the inner rocky planets, because the global secular ring instability is evanescent in the inner regions of the disk.

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Section: Introductionmentioning

confidence: 99%

Secular ring instability in the protoplanetary accretion disk

Willerding

1992

Earth Moon Planet

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“…Theories for the formation and evolution of planets depended primarily on geophysical data from the Solar System (see Brush 1990, and references therein). Starting in the 1940's, astrophysical data began to provide new insights.…”

Section: Introductionmentioning

confidence: 99%

From Disks to Planets

Youdin

Kenyon

2013

Planets, Stars and Stellar Systems

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This pedagogical chapter covers the theory of planet formation, with an emphasis on the physical processes relevant to current research. After summarizing empirical constraints from astronomical and geophysical data, we describe the structure and evolution of protoplanetary disks. We consider the growth of planetesimals and of larger solid protoplanets, followed by the accretion of planetary atmospheres, including the core accretion instability. We also examine the possibility that gas disks fragment directly into giant planets and/or brown dwarfs. We defer a detailed description of planet migration and dynamical evolution to other work, such as the complementary chapter in this series by Morbidelli (available at arXiv:1106.4114).Comment: 50 pages text plus 11 figures and table of symbols. To be published in "Planets, Stars and Stellar Systems", P. Kalas and L. French (eds.). Comments and suggestions for future revisions welcom

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“…The original sample of the four gas giants in our solar system has increased significantly and the core-accretion model is challenged to explain this varied sample of gas giant planets. Brush [20] has written a very interesting historical and comprehensive account of the evolution of planetary ideas and models which is well worth reading.…”

Section: Observational Constraints 103mentioning

confidence: 99%

Core‐Accretion Model

Hubickyj

2010

Formation and Evolution of Exoplanets

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IntroductionFifteen years ago planetary formation models were constrained by the observational data of the planets in the solar system. Since the discovery of the companion orbiting 51 Peg [1, 2], planetary formation models need to explain the planets in the solar system and the over 300 confirmed-observed exoplanets and over 30 candidates of multiple planet systems around stars other than the Sun. We have found that these exoplanets are diverse in their characteristics. The mission of searching for Earth-sized planets, Kepler, will increase the number and diversity of planets and pose new challenges to planetary formation models.The goal of this chapter is to review the core-accretion gas capture ((CAGC) or core accretion) model for the formation of the gas giant planets. In this model, planetesimals accrete into a solid core that eventually gravitationally accretes gas from the solar nebula. This chapter provides the basic information that an interested reader would need to acquire a robust understanding of the model in its theoretical and computational form.Section 5.2 contains a brief historical review of the progenitors of this model and the results of and the progress made by these early investigators. Section 5.3 describes the observational constraints on this proposed model. Section 5.4 provides an overview of the core-accretion model describing the protoplanet's growth from an embryo to a gas giant planet. Section 5.5 introduces the mathematical structure of the model, the boundary conditions, and the assumptions applied in the simulation. Section 5.6 discusses the results of the simulations, focusing on the description of the work by the NASA/ARC and UCSC group. Section 5.7 presents a discussion of topics related to the core-accretion model and final remarks. Historical Background of the Development of the Core Accretion ModelSince the time planets were distinguished from stars, people have thought about their origin. Descartes [3], Kant [4], Laplace [5], and Herschel [6] formalized the Formation and Evolution of Exoplanets. Edited by Rory Barnes

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Theories of the origin of the solar system 1956- 1985

Cited by 26 publications

References 512 publications

Secular ring instability in the protoplanetary accretion disk

Secular ring instability in the protoplanetary accretion disk

From Disks to Planets

Core‐Accretion Model

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