Formation of (exo–)planets

Dullemond, C. P.

doi:10.1002/asna.201311899

Cited by 3 publications

(3 citation statements)

References 67 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Christophe Pinte indicated that a classical theory of planetesimal formation has shortcomings in the mechanism of collisional grain growth, which has not yet been resolved by observations (Pinte, 2015). Meter-sized dust aggregates collide so fast that they cannot stick to grow further, but they suffer from fragmentation, the so-called fragmentation barrier (e.g., Dullemond, 2013). However, Wada et al (2009) have shown that dust aggregates consisting of submicrometer-sized grains can go beyond the fragmentation barrier, if they are composed of ices.…”

Section: Protoplanetary Disksmentioning

confidence: 99%

Cosmic dust VIII

Kimura¹,

Kolokolova²,

Li³

et al. 2016

Planetary and Space Science

View full text Add to dashboard Cite

show abstract

Section: Protoplanetary Disksmentioning

confidence: 99%

Cosmic dust VIII

Kimura¹,

Kolokolova²,

Li³

et al. 2016

Planetary and Space Science

View full text Add to dashboard Cite

show abstract

“…But because dust grains migrate, this is not the case in discs. -The underlying growth model remains simple and does not consider more complex effects that have been shown to affect the evolution of the dust population in young discs (see Dullemond 2013, for a recent review): for instance, bouncing or fragmentation barrier, charging barrier or porosity evolution (Okuzumi et al 2012). -The radial gas flow, which may be important in the very central parts of the disc was not considered here.…”

Section: Model Limitationsmentioning

confidence: 99%

Diversity in the outcome of dust radial drift in protoplanetary discs

Pinte

Laibe

2014

A&A

View full text Add to dashboard Cite

The growth of dust particles into planet embryos needs to circumvent the "radial-drift barrier", i.e. the accretion of dust particles onto the central star by radial migration. The outcome of the dust radial migration is governed by simple criteria between the dust-to-gas ratio and the exponents p and q of the surface density and temperature power laws. The transfer of radiation provides an additional constraint between these quantities because the disc thermal structure is fixed by the dust spatial distribution. To assess which discs are primarily affected by the radial-drift barrier, we used the radiative transfer code MCFOST to compute the temperature structure of a wide range of disc models, stressing the particular effects of grain size distributions and vertical settling. We find that the outcome of the dust migration process is very sensitive to the physical conditions within the disc. For high dust-to-gas ratios ( 0.01) and/or flattened disc structures (H/R 0.05), growing dust grains can efficiently decouple from the gas, leading to a high concentration of grains at a critical radius of a few AU. Decoupling of grains from gas can occur at a large fraction (>0.1) of the initial radius of the particle, for a dust-to-gas ratio greater than ≈0.05. Dust grains that experience migration without significant growth (millimetre and centimetre-sized) are efficiently accreted for discs with flat surface density profiles (p < 0.7) while they always remain in the disc if the surface density is steep enough (p > 1.2). Between (0.7 < p < 1.2), both behaviours may occur depending on the exact density and temperature structures of the disc. Both the presence of large grains and vertical settling tend to favour the accretion of non-growing dust grains onto the central object, but it slows down the migration of growing dust grains. If the disc has evolved into a self-shadowed structure, the required dust-to-gas ratio for dust grains to stop their migration at large radius become much smaller, of the order of 0.01. All the disc configurations are found to have favourable temperature profiles over most of the disc to retain their planetesimals.

show abstract

“…Current formation theories postulate that proto-planetary cores form in metal-rich accretion disks surrounding the host star. These proto-planets co-evolve with the disk and can undergo orbital decay due to torque asymmetries in the surrounding disk material (Armitage 2011;Mordasini et al 2012;Dullemond 2013).…”

Section: Introductionmentioning

confidence: 99%

ROME/REA: A Gravitational Microlensing Search for Exoplanets Beyond the Snow Line on a Global Network of Robotic Telescopes

Tsapras¹,

Street

Hundertmark³

et al. 2019

PASP

View full text Add to dashboard Cite

Planet population synthesis models predict an abundance of planets with semi-major axes between 1-10 au, yet they lie at the edge of the detection limits of most planet finding techniques. Discovering these planets and studying their distribution is critical to understanding the physical processes that drive planet formation. ROME/REA is a gravitational microlensing project whose main science driver is to discover exoplanets in the cold outer regions of planetary systems. To achieve this, it uses a novel approach combining a multi-band survey with reactive follow-up observations, exploiting the unique capabilities of the Las Cumbres Observatory (LCO) global network of robotic telescopes combined with a Target and Observation Manager (TOM) system. We present the main science objectives and a technical overview of the project, including initial results.

show abstract

Formation of (exo–)planets

Abstract: In this small review I will address three recent topics in the field of theoretical planet formation studies. This review is not meant to be complete in any way. It is meant to give an idea where some of the recent developments are.

Cited by 3 publications

References 67 publications

Cosmic dust VIII

Cosmic dust VIII

Diversity in the outcome of dust radial drift in protoplanetary discs

ROME/REA: A Gravitational Microlensing Search for Exoplanets Beyond the Snow Line on a Global Network of Robotic Telescopes

Contact Info

Product

Resources

About