The distribution of mass in the planetary system and solar nebula

Weidenschilling, S. J.

doi:10.1007/bf00642464

Cited by 900 publications

(794 citation statements)

References 15 publications

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“…As our models assume p=3.5, an increase in the maximum dust grain size by a factor of ∼75, say, from 1 mm to 10 cm, could explain this drop in flux. This is borne out by a number of studies that have found cavities, gaps, spiral arms, and other asymmetries in Class II disks that may indicate the presence of planets (Isella et al 2010Andrews et al 2011Andrews et al , 2016Casassus et al 2013; Weidenschilling 1977). We find that our Class I disks, on average, are more massive than the Taurus Class II disks, likely due to dust grain processing hiding matter in larger bodies in the older Class II disks.…”

Section: Class I Versus Class Ii Disk Massesmentioning

confidence: 51%

“…An accounting of the material in our own solar system, which is dominated by the mass of Jupiter, suggests that disk masses of   -M 0.01 0.1 are needed to form a planetary system like our own (e.g., Weidenschilling 1977;Hayashi 1981;Desch 2007). The masses inferred from submillimeter observations of Class II disks are, on average, below this MMSN.…”

Section: Implications For Giant Planet Formationmentioning

confidence: 96%

“…In the past decade there has been a large effort, particularly with interferometers like the Combined Array for Research in Millimeter-wave Astronomy (CARMA), the SMA, and now ALMA, toward measuring Class II disk masses (Andrews & Williams 2005, 2007Eisner et al 2008;Mann & Williams 2010;Mann et al 2014;Ansdell et al 2016Ansdell et al , 2017Barenfeld et al 2016;Pascucci et al 2016). These studies typically find that the majority of these disks fall well below the  -M 0.01 0.1 needed to form planetary systems like our own (e.g., Weidenschilling 1977;Desch 2007).…”

Section: Introductionmentioning

confidence: 99%

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Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Sheehan

Eisner

2017

ApJ

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Class I protostars are thought to represent an early stage in the lifetime of protoplanetary disks, when they are still embedded in their natal envelope. Here we measure the disk masses of 10 Class I protostars in the Taurus Molecular Cloud to constrain the initial mass budget for forming planets in disks. We use radiative transfer modeling to produce synthetic protostar observations and fit the models to a multi-wavelength data set using a Markov Chain Monte Carlo fitting procedure. We fit these models simultaneously to our new Combined Array for Research in Millimeter-wave Astronomy 1.3 mm observations that are sensitive to the wide range of spatial scales that are expected from protostellar disks and envelopes so as to be able to distinguish each component, as well as broadband spectral energy distributions compiled from the literature. We find a median disk mass of  M 0.018 on average, more massive than the Taurus Class II disks, which have median disk mass of~ M 0.0025 . This decrease in disk mass can be explained if dust grains have grown by a factor of 75 in grain size, indicating that by the Class II stage, at a few Myr, a significant amount of dust grain processing has occurred. However, there is evidence that significant dust processing has occurred even during the Class I stage, so it is likely that the initial mass budget is higher than the value quoted here.

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Section: Class I Versus Class Ii Disk Massesmentioning

confidence: 51%

Section: Implications For Giant Planet Formationmentioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

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Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Sheehan

Eisner

2017

ApJ

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“…I adopt the minimum-mass solar nebula model (Weidenschilling 1977;Hayashi 1981), in which the surface density of the solar nebula, Σ, is estimated by adding sufficient hydrogen and helium to the solid bodies in the solar system to recover standard interstellar abundances and spreading this material smoothly in a disk. This yields an estimate of the minimum surface density needed in the solar nebula to form the solar system,…”

Section: Minimum-mass Solar Nebulamentioning

confidence: 99%

Magnetic fields in protoplanetary disks

Wardle

2007

Astrophys Space Sci

249

341

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Magnetic fields likely play a key role in the dynamics and evolution of protoplanetary disks. They have the potential to efficiently transport angular momentum by MHD turbulence or via the magnetocentrifugal acceleration of outflows from the disk surface. Magnetically-driven mixing has implications for disk chemistry and evolution of the grain population, and the effective viscous response of the disk determines whether planets migrate inwards or outwards. However, the weak ionisation of protoplanetary disks means that magnetic fields may not be able to effectively couple to the matter. I examine the magnetic diffusivity in a minimum solar nebula model and present calculations of the ionisation equilibrium and magnetic diffusivity as a function of height from the disk midplane at radii of 1 and 5 AU. Dust grains tend to suppress magnetic coupling by soaking up electrons and ions from the gas phase and reducing the conductivity of the gas by many orders of magnitude. However, once grains have grown to a few microns in size their effect starts to wane and magnetic fields can begin to couple to the gas even at the disk midplane. Because ions are generally decoupled from the magnetic field by neutral collisions while electrons are not, the Hall effect tends to dominate the diffusion of the magnetic field when it is able to partially couple to the gas, except at the disk surfaces where the low density of neutrals permits the ions to remain attached to the field lines.For a standard population of 0.1µm grains the active surface layers have a combined column Σ active ≈ 2 g cm −2 at 1 AU; by the time grains have aggregated to 3 µm, Σ active ≈ 80 g cm −2 . Ionisation in the active layers is dominated by stellar x-rays. In the absence of grains, x-rays maintain magnetic coupling to 10% of

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“…The planetesimal disk was populated by 266 M. Podolak & N. Haghighipour ∼ 10 4 objects with sizes of 1, 10, and 100 km at two regions; 3.7-4.0 AU and 6.2-6.6 AU. The radial profile of the disk surface density was set to r −3/2 (Hayashi 1981, Weidenschilling 1977a) and the orbital eccentricities and inclinations of the planetesimals, and their angular orientations were chosen randomly. The mass of the protoplanet was set equal to the mass of Jupiter, and the radius of the envelope was taken to be 0.47 AU.…”

Section: Numerical Simulationsmentioning

confidence: 99%

Planetesimal Capture by an Evolving Giant Gaseous Protoplanet

Podolak¹,

Haghighipour²

2012

Proc. IAU

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Abstract. Both the core-accretion and disk-instability models suggest that at the last stage of the formation of a gas-giant, the core of this object is surrounded by an extended gaseous envelope. At this stage, while the envelope is contracting, planetesimals from the protoplanetary disk may be scattered into the protoplanets atmosphere and deposit some or all of their materials as they interact with the gas. We have carried out extensive simulations of approximately 10 4 planetesimals interacting with a envelope of a Jupiter-mass protoplanet including effects of gas drag, heating, and the effect of the protoplanets extended mass distribution. Simulations have been carried out for different radii and compositions of planetesimals so that all three processes occur to different degrees. We present the results of our simulations and discuss their implications for the enrichment of ices in giant planets. We also present statistics for the probability of capture (i.e. total mass-deposition) of planetesimals as a function of their size, composition, and closest approach to the center of the protoplanetary body.

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The distribution of mass in the planetary system and solar nebula

Cited by 900 publications

References 15 publications

Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Magnetic fields in protoplanetary disks

Planetesimal Capture by an Evolving Giant Gaseous Protoplanet

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