Inner dusty regions of protoplanetary discs - III. The role of non-radial radiation pressure in dust dynamics

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F47813059%3A19630%2F24%3AA0000347" target="_blank" >RIV/47813059:19630/24:A0000347 - isvavai.cz</a>

Result on the web

<a href="https://academic.oup.com/mnras/article/532/2/2388/7704459?login=true" target="_blank" >https://academic.oup.com/mnras/article/532/2/2388/7704459?login=true</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stae1635" target="_blank" >10.1093/mnras/stae1635</a>

Result language

angličtina

Original language name

Inner dusty regions of protoplanetary discs - III. The role of non-radial radiation pressure in dust dynamics

Original language description

We explore the dynamical behaviour of dust particles that populate the surface of inner optically thick protoplanetary discs. This is a disc region with the hottest dust and is of a great importance for planet formation and dust evolution, but we still struggle to understand all the forces that shape this environment. In our approach, we combine results from two separate numerical studies, one is the wind velocity and density distributions obtained from magnetohydrodynamical simulations of accretion discs, and the other is a high-resolution multigrain dust radiation transfer. In our previous paper in the series, we described the methodology for utilizing these results as an environmental input for the integration of dust trajectories driven by gravity, gas drag, and radiation pressure. Now we have two improvements, we incorporate time changes in the wind density and velocity, and we implement the non-radial radiation pressure force. We applied our analysis on the Herbig Ae and T Tau stars. We confirm that the radiation pressure force can lead to dust outflow, especially in the case of more luminous stars. Additionally, it opposes dust accretion at the inner disc edge and reduces dust settling. These effects are enhanced by the disc wind, especially in the zone where the stellar and the disc magnetic fields meet. Our results suggest that dust grains can stay in the hottest disc region for an extended period and then end up ejected into the outer disc regions.

Czech name

—

Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

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OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

<a href="/en/project/GX21-06825X" target="_blank" >GX21-06825X: Accreting Black Holes in the new era of X-ray polarimetry missions</a><br>

Continuities

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)<br>S - Specificky vyzkum na vysokych skolach<br>I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year

2024

Confidentiality

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

Name of the periodical

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

—

Volume of the periodical

532

Issue of the periodical within the volume

2

Country of publishing house

GB - UNITED KINGDOM

Number of pages

13

Pages from-to

2388-2400

UT code for WoS article

001271732700003

EID of the result in the Scopus database

2-s2.0-85198725747