Tree-based solvers for adaptive mesh refinement code FLASH III: a novel scheme for radiation pressure on dust and gas and radiative transfer from diffuse sources

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F23%3A00571485" target="_blank" >RIV/67985815:_____/23:00571485 - isvavai.cz</a>

Result on the web

<a href="https://doi.org/10.1093/mnras/stad385" target="_blank" >https://doi.org/10.1093/mnras/stad385</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stad385" target="_blank" >10.1093/mnras/stad385</a>

Result language

angličtina

Original language name

Tree-based solvers for adaptive mesh refinement code FLASH III: a novel scheme for radiation pressure on dust and gas and radiative transfer from diffuse sources

Original language description

Radiation is an important contributor to the energetics of the interstellar medium, yet its transport is difficult to solve numerically. We present a novel approach towards solving radiative transfer of diffuse sources via backwards ray tracing. Here, we focus on the radiative transfer of infrared radiation and the radiation pressure on dust. The new module, TreeRay/RadPressure, is an extension to the novel radiative transfer method TreeRay implemented in the grid-based Magneto-Hydrodynamics code Flash. In TreeRay/RadPressure, every cell and every star particle is a source of infrared radiation. We also describe how gas, dust, and radiation are coupled via a chemical network. This allows us to compute the local dust temperature in thermal equilibrium, leading to a significantly improvement over the classical grey approximation. In several tests, we demonstrate that the scheme produces the correct radiative intensities as well as the correct momentum input by radiation pressure. Subsequently, we apply our new scheme to model massive star formation from a collapsing, turbulent core of 150 M-?. We include the effects of both, ionizing and infrared radiation on the dynamics of the core. We find that the newborn massive star prevents fragmentation in its proximity due to radiative heating. Over time, dust and radiation temperature equalize, while the gas temperature can be either warmer due to shock heating or colder due to insufficient dust-gas coupling. Compared to gravity, the effects of radiation pressure are insignificant for the stellar mass on the simulated time-scale in this work.

Czech name

—

Czech description

—

Type

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

CEP classification

—

OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

<a href="/en/project/GA19-15008S" target="_blank" >GA19-15008S: Star formation efficiency in massive star clusters</a><br>

Continuities

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year

2023

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

1365-2966

Volume of the periodical

21

Issue of the periodical within the volume

1

Country of publishing house

US - UNITED STATES

Number of pages

25

Pages from-to

160-184

UT code for WoS article

000951204600002

EID of the result in the Scopus database

2-s2.0-85160587738