A5055530198- Stellar, planetary, and galactic studies
- Astrophysics and Star Formation Studies
- Astro and Planetary Science
- Astrophysical Phenomena and Observations
- Molecular Spectroscopy and Structure
- Astronomy and Astrophysical Research
- Planetary Science and Exploration
- Astronomical Observations and Instrumentation
- Galaxies: Formation, Evolution, Phenomena
- Gamma-ray bursts and supernovae
- Mechanics and Biomechanics Studies
- Botanical Research and Chemistry
- Space Science and Extraterrestrial Life
- Black Holes and Theoretical Physics
- History and Developments in Astronomy
- Tribology and Lubrication Engineering
- Aerodynamics and Acoustics in Jet Flows
- Cosmology and Gravitation Theories
- Fluid Dynamics and Turbulent Flows
- Impact of Light on Environment and Health
- Solar and Space Plasma Dynamics
- High-pressure geophysics and materials
- Spectroscopy and Laser Applications
- Adaptive optics and wavefront sensing
- Fluid Dynamics and Vibration Analysis
University of Valparaíso
2018-2023
Millenium Nucleus for Planet Formation
2018-2023
Viña del Mar University
2021-2023
Valparaiso University
2023
National Astronomical Observatories
2018-2021
Chinese Academy of Sciences
2021
Max Planck Institute for Astronomy
2018-2019
Max Planck Society
2018-2019
Pontificia Universidad Católica de Chile
2013-2018
University of Chile
2015-2017
The finding of residual gas in the large central cavity HD142527 disk motivates questions on origin its non-Keplerian kinematics, and possible connections with planet formation. We aim to understand physical structure that underlies intra-cavity gaseous flows, guided by new molecular-line data CO(6-5) unprecedented angular resolutions. Given warped inferred from identification scattered-light shadows cast outer disk, kinematics are consistent, first order, axisymmetric accretion onto inner...
The identification of ongoing planet formation requires the finest angular resolutions and deepest sensitivities in observations inspired by state-of-the-art numerical simulations. Hydrodynamic simulations planet–disk interactions predict circumplanetary disks (CPDs) around accreting planetary cores. These CPDs have eluded unequivocal detection—their predictions CPD tracers. In this work, we aim to assess observability embedded with Atacama Large Millimeter/submillimeter Array (ALMA) as...
We present 3D smoothed particle hydrodynamics simulations of protoplanetary discs undergoing a flyby by stellar perturber on parabolic orbit lying in plane inclined relative to the disc mid-plane. model as mixture gas and dust, with grains ranging from 1 |$\mu$|m 10 cm size. Exploring different orbital inclinations, periastron distances, mass ratios, we investigate dynamical response during after flyby. find that flybys induce evolving spiral structure both dust can persist for thousands...
Tidal encounters in star clusters perturb discs around young protostars. In Cuello et al. (2019a, Paper I) we detailed the dynamical signatures of a stellar flyby both gas and dust. Flybys produce warped discs, spirals with evolving pitch angles, increasing accretion rates, disc truncation. Here present corresponding observational these features optical/near-infrared scattered light (sub-) millimeter continuum CO line emission. Using representative prograde retrograde for direct comparison,...
Shadows and spirals seem to be common features of transition discs. Among the spiral-triggering mechanisms proposed, only one establishes a causal link between shadows so far. In fact, provided presence in disc, combined effect temperature gradient differential disc rotation, creates strong azimuthal pressure gradients. After several thousand years, grand-design develop gas phase. Previous works have considered static caused by an inclined inner disc. However, some cases, regions...
The mechanisms of planet formation are still under debate. We know little about how planets form, even if more than 4000 exoplanets have been detected to date. Recent investigations target the cot newly born planets: protoplanetary disk. At first stages their life, accrete material from gas-rich disk in which they embedded. Transitional disks indeed that show peculiarities, such as gaps, spiral arms, and rings, can be connected presence substellar companions. To investigate what is...
The vertical structure of debris disks provides clues about their dynamical evolution and the collision rate unseen planetesimals. Thanks to ever-increasing angular resolution contemporary instruments facilities, we are beginning constrain scale height a handful disks, either at near-infrared or millimeter wavelengths. Nonetheless, this is often done for individual targets only. We present here geometric modeling eight close edge-on, all observed with same instrument (SPHERE) using mode...
We present new data of the protoplanetary disc surrounding Herbig Ae/Be star HD 169142 obtained in very broad-band (VBB) with Zurich imaging polarimeter (ZIMPOL), a sub-system Spectro-Polarimetric High-contrast Exoplanet REsearch instrument (SPHERE) at Very Large Telescope (VLT). Our Polarimetric Differential Imaging (PDI) observations probe as close 0.03" (3.5au) to and are able trace out ~1.08" (~126au). find an inner hole, bright ring bearing substructures around 0.18" (21au),...
As planets grow the exchange of angular momentum with gaseous component protoplanetary disc produces a net torque resulting in variation semi-major axis planet. For low-mass not able to open gap this regime is known as type I migration. Pioneer works studied mechanism isothermal discs finding fast inward migration rates that were unable reproduce observed properties extrasolar planets. In last years, several improvements have been made order extend study non-isothermal discs. Moreover, it...
Context. Debris disks have commonly been studied around intermediate-mass stars. Their intense radiation fields are believed to efficiently remove the small dust grains that constantly replenished by collisions. For lower-mass stars, in particular M-stars, removal mechanism needs be further investigated given much weaker field produced these objects. Aims. We present new polarimetric observations of nearly edge-on disk pre-main sequence M-type star GSC 07396-00759, taken with VLT/SPHERE...
Episodic accretion is a low-mass pre-main sequence phenomenon characterized by sudden outbursts of enhanced accretion. These objects are classified into two: protostars with elevated levels that lasts for decades or more, called FUors, and shorter repetitive bursts, EXors. HBC 494 FUor object embedded in the Orion Molecular Cloud. Earlier Atacama Large (sub-)Millimeter Array (ALMA) continuum observations showed an asymmetry disk at 0.''2 resolution. Here, we present follow-up ~0.''03,...
The evolution of an accretion disk, formed as a consequence the disruption star by black hole, is followed solving numerically hydrodynamic equations. present investigation aims to study dependence resulting light curves on dynamical and physical properties such transient disk during its existence. One main results derived from our simulations that blackbody fits X-ray data tend overestimate true mean temperature. In fact, temperature should be identified with color rather than average value...
In recent years, technical and theoretical work to detect moons rings around exoplanets has been attempted. The small mass/size ratios between planets means this is very challenging, having only one exoplanetary system where spotting an exomoon might be feasible (i.e. Kepler-1625b i). work, we study the dynamical evolution of ringed exomoons, dubbed "cronomoons" after their similarity with Cronus (Greek for Saturn), Chronos (the epitome time), following Transit Timing Variations (TTV)...
Rings around giant exoplanets (hereafter 'exorings') are still a missing planetary phenomenon among the vast number of discovered planets. Despite fact there exist large methods for identifying and characterizing these exorings, none them has been successful to date. Most those efforts focus on photometric signatures produced by rings transiting exoplanets; thus, little interest intended detectable that non-transiting ringed planets might cause owing excess scattered starlight from both...
Planets form in young circumstellar disks called protoplanetary disks. However, it is still difficult to catch planet formation in-situ. Nevertheless, from recent ALMA/SPHERE data, encouraging evidence of the direct and indirect presence embedded planets has been identified around stars: co-moving point sources, gravitational perturbations, rings, cavities, emission dips or shadows cast on The interpretation these observations needs a robust physical framework deduce complex disk geometry....
Context. Supermassive black holes are probably present in the centre of majority galaxies. There is consensus that these exotic objects formed by growth seeds either mass accretion from a circumnuclear disk and/or coalescences during merger episodes.
Context. Despite the recent discovery of spiral-shaped features in protoplanetary discs near-infrared and millimetric wavelengths, there is still an active discussion to understand how they formed. In fact, spiral waves observed around young stars can be due different physical mechanisms: planet/companion torques, gravitational perturbations or illumination effects. Aims. We study spirals formed gaseous phase two diametrically opposed shadows cast at fixed disc locations. The are created by...
Context. Debris disks are the signposts of collisionally eroding planetesimal circumstellar belts, whose study can put important constraints on structure extrasolar planetary systems. The best morphology such often obtained from spatially resolved observations in scattered light. In this paper, we investigate young (~16 Myr) bright gas-rich debris disk around HD 121617. Aims. We use new light VLT/SPHERE to characterize and dust properties disk. From these properties, then derive physical...
Abstract The cooler than expected optical–UV transient PS1-10jh detected by the Pan-STARRS1 survey is probably related to a tidal disruption event in which He-rich stellar core remnant implied. evolution of bound debris during disc-phase studied solving hydrodynamic equations. model provides good fit either raising part light curve bands gP1, rP1 and iP1 or early decay. parameters characterizing this optimized are mass central black hole, i.e. 6.3 × 106 M⊙, critical Reynolds number ${\cal R}...
Debris disks are the natural by-products of planet formation process. Scattered or polarized light observations mostly sensitive to small dust grains that released from grinding down bigger planetesimals. High angular resolution at optical wavelengths can provide key constraints on radial and azimuthal distribution grains. These help us better understand where most upon collisions. We present SPHERE/ZIMPOL debris disk around HR 4796 A, model profiles along several angles with a code accounts...
ABSTRACT Stellar binaries represent a substantial fraction of stellar systems, especially among young objects. Accordingly, play an important role in setting the architecture large number protoplanetary discs. Binaries coplanar and polar orientations with respect to circumbinary disc are stable configurations could induce non-axisymmetric structures dust gas distributions. In this work, we suggest that shown central region HD 169142 produced by presence inner binary (P-type) planet. We find...
In this paper I review and discuss the basic concepts of accretion disks, focused especially on case disks around black holes. The well known alpha-model is revisited, showing strengths weaknesses model. Other turbulent viscosity prescription, based Reynolds number, that may improve our understanding paradigm discussed. A simple but efficient mathematical model a self-gravitating disk, as observational evidence these objects, are also included.
We present polarized light observations of the transitional disk around Sz 91 acquired with VLT/NaCo at $H$ (1.7$\mu$m) and $K_s$ (2.2$\mu$m) bands. resolve detect emission up to $\sim$0."5 ($\sim$80 au) along a central cavity both computed radiative transfer model that accounts for main characteristics observations. found is best explained by small, porous grains distributed in $\sim$45 au cavity. Previous ALMA have revealed large sub-mm ($\sim$83 extended gas from innermost (<16 regions...
Trojans are defined as objects that share the orbit of a planet at stable Lagrangian points $L_4$ and $L_5$. In Solar System, these bodies show broad size distribution ranging from micrometer($μ$m) to centimeter(cm) particles (Trojan dust) up kilometer (km) rocks asteroids). It has also been theorized earth-like may be formed in extra-solar systems. The Trojan formation mechanism is still under debate, especially theories involving effects dissipative forces viscous gaseous environment. We...
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...