Observations of young stars hosting transition disks show that several them have high accretion rates, despite their presenting extended cavities in dust component. This represents a challenge for theoretical models, which struggle to reproduce both features. We explore if disk evolution model, including dead zone and dispersal by X-ray photoevaporation, can explain the rates large gaps (or cavities) measured disks. implement turbulence profile photoevaporative mass loss into numerical...

Context: In the last six years, VVV survey mapped 562 sq. deg. across bulge and southern disk of Galaxy. However, a detailed study these regions, which includes $\sim 36$ globular clusters (GCs) thousands open is by no means an easy challenge. High differential reddening severe crowding along line sight makes highly hamper to reliably distinguish stars belonging different populations and/or systems. Aims: The aim this separate that likely belong Galactic GC NGC 6544 from its surrounding...

Context. The water snowline divides dry and icy solid material in protoplanetary disks, has been thought to significantly affect planet formation at all stages. If particles break up more easily than ones, then the causes a traffic jam, because small grains drift inward lower speeds larger pebbles. Aims. We aim evaluate effect of high dust concentrations around onto gas dynamics. Methods. Using numerical simulations, we model global radial evolution an axisymmetric disk. Our includes...

[Abridged] Aims. We provide an important step toward a better understanding of the magnetorotational instability (MRI)-dust coevolution in protoplanetary disks by presenting proof concept that dust evolution ultimately plays crucial role MRI activity. Methods. First, we study how fixed power-law size distribution with varying parameters impacts activity, especially steady-state MRI-driven accretion, employing and improving our previous 1+1D turbulence model. Second, relax accretion...

Over the last years, large (sub-)millimetre surveys of protoplanetary disks have well constrained demographics disks, such as their millimetre luminosities, spectral indices, and disk radii. Additionally, several high-resolution observations revealed an abundance substructures in dust continuum. The most prominent are ring like structures, likely due to pressure bumps trapping particles. origins characteristics these bumps, nevertheless, need be further investigated. purpose this work is...

ABSTRACT Photoevaporative disc winds play a key role in our understanding of circumstellar evolution, especially the final stages, and they might affect planet formation process location planets. The study transition discs (i.e. with central dust cavity) is for photoevaporation dispersal. However, we need to distinguish cavities created by from those giant Theoretical models are necessary identify possible observational signatures two different processes, find differences between processes...

The radial velocities and direct imaging observations of exoplanets have suggested that the frequency giant planets may decrease for intermediate-mass stars ($2.5-8\,M_\odot$). key mechanism could hinder their formation remains unclear. From a theoretical point view, planet around take place on longer timescales, which -- coupled with fast migration efficient photoevaporation prevent planetary in these environments. In this letter, we investigate temporal evolution drift dust particles disks...

Context. The protoplanetary disk around the star HD 100546 displays prominent substructures in form of two concentric rings. Recent observations with Atacama Large Millimeter/sub-millimeter Array (ALMA) have revealed these features high angular resolution and resolved faint outer ring well. This allows us to study nature system further. Aims. Our aim is constrain some properties potential planets embedded disk, assuming that they induce observed rings gaps. Methods. We present...

Context . The dust in planet-forming disks is known to evolve rapidly through growth and radial drift. In the high irradiation environments of massive star-forming regions where most stars form, external photoevaporation also contributes rapid dispersal disks. This raises question why we still observe quite disk masses regions. Aims We test whether presence substructures enough explain survival component observed millimeter continuum emission protoplanetary located within characterize...

The growth of computational astrophysics and the complexity multi-dimensional data sets evidences need for new versatile visualization tools both analysis presentation data. In this work, we show how to use open-source software Blender as a three-dimensional (3D) tool study visualize numerical simulation results, focusing on astrophysical hydrodynamic experiments. With datacube input, can generate volume rendering 3D data, evolution in time, do fly-around camera animation highlight points...

Planets form in discs of gas and dust around stars, continue to grow by accretion disc material while available. Massive planets clear a gap their protoplanetary disc, but can still accrete through circumplanetary disk. For high enough rates the planet should be detectable at infrared wavelengths. As energy accreted on is released, surroundings heat up feedback process. We aim test how this affects coorbital region rate itself. modified 2D code FARGO-AD include prescription for luminosity...

Abstract RW Aur A has experienced various dimming events in recent years, decreasing its brightness by ∼2 mag for periods of months to years. Multiple observations indicate that a high concentration dust grains, from the protoplanetary disk’s inner regions, is blocking starlight during these events. We propose new mechanism can send large amounts close star on short timescales, through reactivation dead zone disk. Using numerical simulations, we model accretion gas and dust, along with...

Context . Photoevaporation and dust-trapping are individually considered to be important mechanisms in the evolution morphology of protoplanetary disks. However, it is not yet clear what kind observational features expected when both processes operate simultaneously. Aims We studied how presence (or absence) early substructures, such as gaps caused by planets, affects dust distribution flux millimeter continuum disks that undergoing photoevaporative dispersal. also tested if predicted...

[Abridged] Aims. We provide an important step toward a better understanding of the magnetorotational instability (MRI)-dust coevolution in protoplanetary disks by presenting proof concept that dust evolution ultimately plays crucial role MRI activity. Methods. First, we study how fixed power-law size distribution with varying parameters impacts activity, especially steady-state MRI-driven accretion, employing and improving our previous 1+1D turbulence model. Second, relax accretion...

Photoevaporative disc winds play a key role in our understanding of circumstellar evolution, especially the final stages, and they might affect planet formation process location planets. The study transition discs (i.e. with central dust cavity) is for photoevaporation dispersal. However, we need to distinguish cavities created by from those giant Theoretical models are necessary identify possible observational signatures two different processes, find differences between processes still...

[abridged]Photoevaporation and dust-trapping are individually considered to be important mechanisms in the evolution morphology of protoplanetary disks. We studied how presence early substructures affects dust distribution flux millimeter continuum disks that undergoing photoevaporative dispersal. also tested if predicted properties resemble those observed population transition used numerical code Dustpy simulate disk considering gas accretion, growth, at substructures, mass loss due X-ray...

The dust in planet-forming disks evolve rapidly through growth and radial drift, external photoevaporation also contributes to this evolution massive star-forming regions. We test whether the presence of substructures can explain survival component observed millimeter continuum emission protoplanetary located within characterize content removed by photoevaporative winds. For this, we performed hydrodynamical simulations subject irradiation fields $F_{UV} = 10^2$, $10^3$, $10^4\, G_0$, with...