Ionization and Dust Charging in Protoplanetary Disks

Ivlev, A. V.; Akimkin, V. V.; Caselli, P.

doi:10.3847/1538-4357/833/1/92

Cited by 30 publications

(32 citation statements)

References 60 publications

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“…Second, turbulence affects transport processes and, hence, the disk density and velocity structure. Third, dust grains are efficient absorbers of free electrons (Ivlev et al, 2016) and can modulate the ionization fraction and the development of the MRI. It is therefore non-trivial to predict the exact effect of turbulence on dust growth.…”

Section: Parameter Space Studymentioning

confidence: 99%

Early evolution of viscous and self-gravitating circumstellar disks with a dust component

Vorobyov

Akimkin

Stoyanovskaya

et al. 2018

A&A

136

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Aims. The long-term evolution of a circumstellar disk starting from its formation and ending in the T Tauri phase was simulated numerically with the purpose of studying the evolution of dust in the disk with distinct values of viscous α-parameter and dust fragmentation velocity v frag . Methods. We solved numerical hydrodynamics equations in the thin-disk limit, which are modified to include a dust component consisting of two parts: sub-micron-sized dust and grown dust with a maximum radius ar. The former is strictly coupled to the gas, while the latter interacts with the gas via friction. The conversion of small to grown dust, dust growth, and dust self-gravity are also considered. Results. We found that the process of dust growth known for the older protoplanetary phase also holds for the embedded phase of disk evolution. The dust growth efficiency depends on the radial distance from the star -ar is largest in the inner disk and gradually declines with radial distance. In the inner disk, ar is limited by the dust fragmentation barrier. The process of small-to-grown dust conversion is very fast once the disk is formed. The total mass of grown dust in the disk (beyond 1 AU) reaches tens or even hundreds of Earth masses already in the embedded phase of star formation and even a greater amount of grown dust drifts in the inner, unresolved 1 AU of the disk. Dust does not usually grow to radii greater than a few cm. A notable exception are models with α ≤ 10 −3 , in which case a zone with reduced mass transport develops in the inner disk and dust can grow to meter-sized boulders in the inner 10 AU. Grown dust drifts inward and accumulates in the inner disk regions. This effect is most pronounced in the α ≤ 10 −3 models where several hundreds of Earth masses can be accumulated in a narrow region of several AU from the star by the end of embedded phase. The efficiency of grown dust accumulation in spiral arms is stronger near corotation where the azimuthal velocity of dust grains is closest to the local velocity of the spiral pattern. In the framework of the adopted dust growth model, the efficiency of small-to-grown dust conversion was found to increase for lower values of α and v frag .

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Section: Parameter Space Studymentioning

confidence: 99%

Early evolution of viscous and self-gravitating circumstellar disks with a dust component

Vorobyov

Akimkin

Stoyanovskaya

et al. 2018

A&A

136

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“…regarding coagulation). Ivlev, Akimkin, & Caselli (2016) present an analytic model that yields the ionisation state of such dusty media, which could be incorporated into non-ideal MHD codes-offering an imminently achievable significant advance.…”

Section: Reduced Chemical Networkmentioning

confidence: 99%

Grand Challenges in Protoplanetary Disc Modelling

Haworth

Ilee

Forgan

et al. 2016

Publ. Astron. Soc. Aust.

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The Protoplanetary Discussions conference-held in Edinburgh, UK, from 2016 March 7th-11th-included several open sessions led by participants. This paper reports on the discussions collectively concerned with the multi-physics modelling of protoplanetary discs, including the self-consistent calculation of gas and dust dynamics, radiative transfer, and chemistry. After a short introduction to each of these disciplines in isolation, we identify a series of burning questions and grand challenges associated with their continuing development and integration. We then discuss potential pathways towards solving these challenges, grouped by strategical, technical, and collaborative developments. This paper is not intended to be a review, but rather to motivate and direct future research and collaboration across typically distinct fields based on community-driven input, to encourage further progress in our understanding of circumstellar and protoplanetary discs.

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“…In astrophysics, the influence of the dust component on the charge balance, dynamics, thermodynamics, and chemistry is crucial [1]. Furthermore, it has recently been realized that charges of dust particles with sizes of submicron and up are important during the planet formation process [2][3][4]. An 'electrostatic barrier' can hinder the dust growth [5].…”

Section: Introductionmentioning

confidence: 99%

Observation of metallic sphere–complex plasma interactions in microgravity

Schwabe¹,

Zhdanov²,

Hagl³

et al. 2017

New J. Phys.

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The PK-3 Plus laboratory on board the International Space Station is used to study the interaction between metallic spheres and a complex plasma. We show that the metallic spheres significantly affect both the local plasma environment and the microparticle dynamics. The spheres charge under the influence of the plasma and repel the microparticles, forming cavities surrounding the spheres. The size of the cavity around a sphere is used to study the force balance acting on microparticles at the cavity edge. We show that the ion drag force and pressure force from other microparticles balances with the electric force acting from the sphere to within 20%. At intermediate distances from the sphere surface, the interaction between the microparticles and the metallic spheres is attractive due to the drag force stemming from the ions which are moving towards the highly charged spheres. The spheres thus strongly affect the plasma fluxes. This modification of the plasma flux can lead to an effective surface tension acting on the microparticles, and to the excitation of dust-density waves near the spheres, as the local electric field crosses a threshold.

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Ionization and Dust Charging in Protoplanetary Disks

Cited by 30 publications

References 60 publications

Early evolution of viscous and self-gravitating circumstellar disks with a dust component

Early evolution of viscous and self-gravitating circumstellar disks with a dust component

Grand Challenges in Protoplanetary Disc Modelling

Observation of metallic sphere–complex plasma interactions in microgravity

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