Zooming in on the place of rocky planet formation: infrared interferometric observations of protoplanetary disks

2021 ◽  
Author(s):  
Jacques Kluska
Keyword(s):  
Planet Formation ◽  
Angular Resolution ◽  
Protoplanetary Disks ◽  
Strong Interactions ◽  
Astronomical Unit ◽  
Mid Infrared ◽  
The Past ◽  
Spatially Resolved ◽  
Infrared Interferometry ◽  
Inner Parts

<div>Spatially resolved observations from ALMA or direct imaging instruments revealed an extreme diversity and complexity of structures and substructures in the outer parts of protoplanetary disks.</div> <div>However, these techniques do not resolve the inner regions of protoplanetary disks, typically at less than 5 astronomical units from the star.</div> <div>These inner regions are crucial to understand the formation of telluric planets.</div> <div>They are also the theatre of strong interactions between the star and the disk that can influence planet formation.</div> <div>Thanks to infrared interferometry we can reach an angular resolution of ~1mas reaching sub-astronomical unit physical scales.</div> <div>We can, therefore use infrared interferometry to reveal and study the structure, composition, and dynamics of the inner parts of protoplanetary disks.</div> <div>In the past few years, the advent of infrared interferometers combining four telescopes such as PIONIER, MATISSE or GRAVITY enabled us to study these disks with an unprecedented detail.</div> <div>In this talk, I will review the recent results of near and mid-infrared interferometric observations of protoplanetary disks.</div>

scholarly journals Herbig Ae/Be Star Disks at High Angular Resolution

2004 ◽  
Vol 221 ◽  
pp. 389-394
Author(s):  
C. P. Dullemond ◽  
C. Dominik ◽  
R. van Boekel ◽  
R. Waters ◽  
M. van den Ancker
Keyword(s):  
Angular Resolution ◽  
Protoplanetary Disks ◽  
Spectral Energy ◽  
High Angular Resolution ◽  
Be Stars ◽  
Spectral Energy Distributions ◽  
Energy Distributions ◽  
Spatially Resolved ◽  
Be Star ◽  
Geometric Picture

We show that there exists a simple geometric picture for the geometries of protoplanetary disks around Herbig Ae/Be stars that explains the two main kinds of spectral energy distributions found for these objects, and that makes predictions that are qualitatively in agreement with currently available spatially resolved images and/or interferometric measurements. Also it qualitatively explains the phenomenon of UX Orionis variability.

scholarly journals Radio Interferometry Observations of the Hallmarks of Planet Formation

2013 ◽  
Vol 8 (S299) ◽  
pp. 80-89
Author(s):  
Sean M. Andrews
Keyword(s):  
Planet Formation ◽  
Angular Resolution ◽  
Planetary System ◽  
Planetary Systems ◽  
Protoplanetary Disks ◽  
Circumstellar Disks ◽  
High Angular Resolution ◽  
Radio Interferometry ◽  
New Directions ◽  
And Migration

AbstractSome of the fundamental processes involved in the evolution of circumstellar disks and the assembly of planetary systems are just now becoming accessible to astronomical observations. The new promise of observational work in the field of planet formation makes for a very dynamic research scenario, which is certain to be amplified in the coming years as the revolutionary Atacama Large Millimeter/submillimeter Array (ALMA) facility ramps up to full operations. To highlight the new directions being explored in these fields, this brief review will describe how high angular resolution measurements at millimeter/radio wavelengths are being used to study several crucial aspects of the formation and early evolution of planetary systems, including: the gas and dust structures of protoplanetary disks, the growth and migration of disk solids, and the interactions between a young planetary system and its natal, gas-rich disk.

Formation and Evolution of Protoplanetary Disks: Observations and Modeling of Jets, Disks, and Disk Substructures

2018 ◽  
Vol 14 (S345) ◽  
pp. 96-101
Author(s):  
Laura M. Pérez
Keyword(s):  
Planet Formation ◽  
Angular Resolution ◽  
Planetary System ◽  
Protoplanetary Disks ◽  
Solid Particles ◽  
High Angular Resolution ◽  
Rapid Progress ◽  
Disk Evolution ◽  
Formation And Evolution ◽  
Dusty Disks

AbstractPlanet formation takes place in the gaseous and dusty disks that surround young stars, known as protoplanetary disks. With the advent of sensitive observations and together with developments in theory, our field is making rapid progress in understanding how the evolution of protoplanetary disks takes place, from its inception to the end result of a fully-formed planetary system. In this review, I discuss how observations that trace both the dust and gas components of these systems inform us about their evolution, mass budget, and chemistry. Particularly, the process of disk evolution and planet formation will leave an imprint on the distribution of solid particles at different locations in a protoplanetary disk, and I focus on recent observational results at high angular resolution in the sub-millimeter regime, which have revealed a variety of substructures present in these objects.

scholarly journals Imaging the water snowline in protostellar envelopes

2017 ◽  
Vol 13 (S332) ◽  
pp. 88-94 ◽  
Author(s):  
Merel L. R. van ’t Hoff
Keyword(s):  
Formation Process ◽  
Planet Formation ◽  
Protoplanetary Disks ◽  
Central Star ◽  
Proof Of Concept ◽  
Spatially Resolved ◽  
Chemical Tracer ◽  
Chemical Effects

AbstractDetermining the locations of the major snowlines in protostellar environments is crucial to fully understand the planet formation process and its outcome. Despite being located far enough from the central star to be spatially resolved with ALMA, the CO snowline remains difficult to detect directly in protoplanetary disks. Instead, its location can be derived from N2H+emission, when chemical effects like photodissociation of CO and N2are taken into account. The water snowline is even harder to observe than that for CO, because in disks it is located only a few AU from the protostar, and from the ground only the less abundant isotopologue H218O can be observed. Therefore, using an indirect chemical tracer, as done for CO, may be the best way to locate the water snowline. A good candidate tracer is HCO+, which is expected to be particularly abundant when its main destructor, H2O, is frozen out. Comparison of H218O and H13CO+emission toward the envelope of the Class 0 protostar IRAS2A shows that the emission from both molecules is spatially anticorrelated, providing a proof of concept that H13CO+can indeed be used to trace the water snowline in systems where it cannot be imaged directly.

Unveiling the mid-plane temperature and mass distribution in the giant-planet formation zone

2017 ◽  
Vol 13 (S332) ◽  
pp. 103-108
Author(s):  
Ke Zhang ◽  
Edwin A. Bergin ◽  
Geoffrey A. Blake ◽  
L. Ilsedore Cleeves ◽  
Kamber R. Schwarz
Keyword(s):  
Mass Distribution ◽  
Planet Formation ◽  
Giant Planet ◽  
Line Emission ◽  
Protoplanetary Disks ◽  
Great Sensitivity ◽  
Spatially Resolved ◽  
Formation Zone ◽  
Core Accretion ◽  
Plane Temperature

AbstractCore-accretion theory predicts that the formation of giant planets predominantly occurs at the dense mid-plane of the inner ∼50 AU of protoplanetary disks. However, due to observational limitation, this critical region remains to be the least charted area in protoplanetary disks. With its great sensitivity, ALMA recently started to image optically thin line emissions arisen from the mid-plane of the inner 50AU in nearby disks, which unlocks an exciting new path to directly constrain the physical properties of the giant planet formation zone through gas tracers. Here we present the first spatially resolved observations of the 13C18O J=3-2 line emission in the TW Hya disk. We show that this emission is optically thin even inside the CO mid-plane snowline. Combining it with the C18O J=3-2 images and the previously detected HD J=1-0 flux, we directly constrain the mid-plane temperature and optical depths of the CO gas and dust. We report a mid-plane CO snowline at 20.5 ± 1.3 AU, a mid-plane temperature distribution of 27+4−3×(R/20.5AU)-0.47+0.06−0.07 K, and a gas mass distribution of 13+8−5×(R/20.5AU)-0.9+0.4−0.3 g cm−2 between 5-20.5 AU in the TW Hya protoplanetary disk. We find a total gas/mm-sized dust mass ratio of 140 ± 40 in this region, suggesting that ∼2.4 earth mass of dust aggregates have grown to > cm sizes (and perhaps much larger).

Investigation by NMR spectroscopy of the structural characteristics of modified oligo-nucleotides with pendant porphyrins

2019 ◽  
Vol 23 (07n08) ◽  
pp. 797-812 ◽  
Author(s):  
Sonja Merkaš ◽  
Mladen Žinić ◽  
Régis Rein ◽  
Nathalie Solladié
Keyword(s):  
Nmr Spectroscopy ◽  
Structural Characteristics ◽  
Strong Interactions ◽  
Light Harvesting Complexes ◽  
The Past ◽  
Naturally Occurring ◽  
Nmr Data ◽  
Intermolecular Distances ◽  
Uracil Base ◽  
Biopolymer Scaffolds

During the past years, we focused on exerting control over the position and distance of porphyrins along our specifically designed oligonucleotidic scaffold. Indeed, in naturally occurring light-harvesting complexes, biopolymer scaffolds hold pigments at intermolecular distances that optimize photon capture, electronic coupling, and energy transfer. To this end, four uridine-porphyrin conjugates (a monomer, a dimer, a tetramer and an octamer) were subjected to a comprehensive conformational analysis by using NMR spectroscopy. The collected NOE NMR data highlighted characteristic and strong interactions indicating that the glycosidic angle between the ribose and uracil base is anti. In order to further investigate the conformation of this family of molecules, NMR experiments were carried out at variable temperatures. At low temperature, the signals of the porphyrinic protons decoalesce, showing two sets of [Formula: see text]-pyrrolic protons. Similar observations are made for signals corresponding to sugar moieties and especially the H1′ protons, indicating molecular motions within our porphyrin-uridin arrays. These results testify in favor of the existence of a dynamic process between C3′-endo and C2′-endo conformations.

scholarly journals The Disk Substructures at High Angular Resolution Project (DSHARP). VI. Dust Trapping in Thin-ringed Protoplanetary Disks

2018 ◽  
Vol 869 (2) ◽  
pp. L46 ◽  
Author(s):  
Cornelis P. Dullemond ◽  
Tilman Birnstiel ◽  
Jane Huang ◽  
Nicolás T. Kurtovic ◽  
Sean M. Andrews ◽  
...  
Keyword(s):  
Angular Resolution ◽  
Protoplanetary Disks ◽  
High Angular Resolution ◽  
Dust Trapping

Mid-infrared interferometry on the Chajnantor plateau: the ALIRA project

2003 ◽  
Author(s):  
Vincent Coude du Foresto ◽  
Jean L. Schneider ◽  
Guy S. Perrin ◽  
Pierre J. Lena ◽  
Anne Dutrey
Keyword(s):  
Mid Infrared ◽  
Infrared Interferometry

scholarly journals Chandra Studies of Supernova Remnants and Pulsars

2001 ◽  
Vol 205 ◽  
pp. 358-365
Author(s):  
Patrick Slane ◽  
John P. Hughes ◽  
Cara E. Rakowski ◽  
David N. Burrows ◽  
John A. Nousek ◽  
...  
Keyword(s):  
Time Resolution ◽  
Supernova Remnants ◽  
Angular Resolution ◽  
Fast Time ◽  
X Ray ◽  
Spatially Resolved ◽  
Unique Capability

With sub-arcsecond angular resolution accompanied by fast time resolution and spatially resolved spectral capabilities, the Chandra X-ray Observatory provides a unique capability for the study of supernova remnants (SNRs) and pulsars. Though in its relative infancy, Chandra has already returned stunning images of SNRs which reveal the distribution of ejecta synthesized in the stellar explosions, the distinct properties of the forward and reverse shocks, and the presence of faint shells surrounding compact remnants. Pulsar observations have uncovered jet features as well as small-scaled structures in synchrotron nebulae. In this brief review we discuss results from early Chandra studies of pulsars and SNRs.

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