A ring-like concentration of mm-sized particles in Sz 91

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F16%3A00540093" target="_blank" >RIV/67985815:_____/16:00540093 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1093/mnrasl/slw006" target="_blank" >https://doi.org/10.1093/mnrasl/slw006</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnrasl/slw006" target="_blank" >10.1093/mnrasl/slw006</a>

Jazyk výsledku

angličtina

Název v původním jazyce

A ring-like concentration of mm-sized particles in Sz 91

Popis výsledku v původním jazyce

Models of planet formation and disc evolution predict a variety of observables in the dust structure of protoplanetary discs. Here, we present Atacama Large Millimeter/submillimeter Array (ALMA) Band-6 and Band-7 observations of the transition disc Sz 91 showing that the continuum emission at 870 mu m, which is dominated by emission from large dust grains, is localized in an optically thin narrow ring. We find that most of the emission (similar to 95 per cent) is concentrated in a ring located at 110 au from the central star that is only about 44 au wide. In contrast, the (CO)-C-12 (2-1) emission peaks closer to the star and is detected up to similar to 488 au from the star. The concentration of large grains in a ring-like structure while the gas disc extends much further in and further out is in qualitative agreement with predictions of hydrodynamical models of planet-disc interactions including radial drift and gas drag.

Název v anglickém jazyce

A ring-like concentration of mm-sized particles in Sz 91

Popis výsledku anglicky

Models of planet formation and disc evolution predict a variety of observables in the dust structure of protoplanetary discs. Here, we present Atacama Large Millimeter/submillimeter Array (ALMA) Band-6 and Band-7 observations of the transition disc Sz 91 showing that the continuum emission at 870 mu m, which is dominated by emission from large dust grains, is localized in an optically thin narrow ring. We find that most of the emission (similar to 95 per cent) is concentrated in a ring located at 110 au from the central star that is only about 44 au wide. In contrast, the (CO)-C-12 (2-1) emission peaks closer to the star and is detected up to similar to 488 au from the star. The concentration of large grains in a ring-like structure while the gas disc extends much further in and further out is in qualitative agreement with predictions of hydrodynamical models of planet-disc interactions including radial drift and gas drag.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

—

Rok uplatnění

2016

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

1365-2966

e-ISSN

—

Svazek periodika

458

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

5

Strana od-do

"L29"-"L33"

Kód UT WoS článku

000374226300007

EID výsledku v databázi Scopus

2-s2.0-84963627696