The Solar Nebula as a Process–An Analytic Model

Stepinski, T. F.

doi:10.1006/icar.1998.5893

Cited by 58 publications

(88 citation statements)

References 17 publications

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“…Once m 0 and j 0 are specified, the analytic solution of Stepinski (1998) gives the gas surface density Σ g,0 (r) = Σ g (r, t = 0) that serves as an intial condition for the evolution of the gaseous disk.…”

Section: Methods Of Calculationmentioning

confidence: 99%

An alternative look at the snowline in protoplanetary disks

Kornet

Rozyczka

Stepinski

2004

A&A

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Abstract.We have calculated an evolution of protoplanetary disk from an extensive set of initial conditions using a timedependent model capable of simultaneously keeping track of the global evolution of gas and water-ice. A number of simplifications and idealizations allows for an embodiment of gas-particle coupling, coagulation, sedimentation, and evaporation/condensation processes. We have shown that, when the evolution of ice is explicitly included, the location of the snowline has to be calculated directly as the inner edge of the region where ice is present and not as the radius where disk's temperature equals the evaporation temperature of water-ice. The final location of the snowline is set by an interplay between all involved processes and is farther from the star than implied by the location of the evaporation temperature radius. The evolution process naturally leads to an order of magnitude enhancement in surface density of icy material.

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Section: Methods Of Calculationmentioning

confidence: 99%

An alternative look at the snowline in protoplanetary disks

Kornet

Rozyczka

Stepinski

2004

A&A

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“…In a process analogous to the water evaporation front discussed above, silicate material could have been comparably enhanced inside the silicate evaporation boundary ($1375 K for forsterite at total pressure of 10 À4 bars; Cuzzi et al 2003). Models of evolving nebulae by, for instance, Bell et al (1997), Stępiński (1998), andCassen (2001), and widely scattered observational data (Calvet et al 2000) tend to show mass accretion rates in the range of 10 À6 to 10 À7 M yr À1 for, typically, 10 4 -10 5 yr. For these accretion rates, midplane temperatures would be much higher than the photospheric temperatures directly observed and could exceed the evaporation temperature of forsterite in the terrestrial planet region (Woolum & Cassen (1999).…”

Section: Locally Early-and Late-stage 16 O-rich Environmentmentioning

confidence: 99%

Evolution of Oxygen Isotopic Composition in the Inner Solar Nebula

Krot¹,

Hutcheon²,

Yurimoto³

et al. 2005

ApJ

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Changes in the chemical and isotopic composition of the solar nebula with time are reflected in the properties of different constituents that are preserved in chondritic meteorites. CR-group carbonaceous chondrites are among the most primitive of all chondrite types and must have preserved solar nebula records largely unchanged. We have analyzed the oxygen and magnesium isotopes in a range of the CR constituents of different formation temperatures and ages, including refractory inclusions and chondrules of various types. The results provide new constraints on the time variation of the oxygen isotopic composition of the inner (<5 AU ) solar nebula-the region where refractory inclusions and chondrules most likely formed. A chronology based on the decay of short-lived 26 Al (t 1 = 2 $ 0:73 Myr) indicates that the inner solar nebula gas was 16 O-rich when refractory inclusions formed, but less than 0.8 Myr later, gas in the inner solar nebula became 16 O-poor, and this state persisted at least until CR chondrules formed $1-2 Myr later. We suggest that the inner solar nebula became 16 O-poor because meter-sized icy bodies, which were enriched in 17 O and 18 O as a result of isotopic self-shielding during the ultraviolet photodissociation of CO in the protosolar molecular cloud or protoplanetary disk, agglomerated outside the snow line, drifted rapidly toward the Sun, and evaporated at the snow line. This led to significant enrichment in 16 O-depleted water, which then spread through the inner solar system. Astronomical studies of the spatial and temporal variations of water abundance in protoplanetary disks may clarify these processes.

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“…(3-7) gives where Σ 0 , the surface density at 1 AU, depends on the mass accretion rate. Solving for the midplane temperature with realistic opacities yields Σ ∝ R −β with β ≈ 0.6-1 (e.g., Stepinski 1998;Chambers 2009). …”

Section: Viscously Heated Disksmentioning

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 Solar Nebula as a Process–An Analytic Model

Cited by 58 publications

References 17 publications

An alternative look at the snowline in protoplanetary disks

An alternative look at the snowline in protoplanetary disks

Evolution of Oxygen Isotopic Composition in the Inner Solar Nebula

From Disks to Planets

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