Dust Grain Growth and Dusty Supernovae in Low-metallicity Molecular Clouds

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F22%3A00559605" target="_blank" >RIV/67985815:_____/22:00559605 - isvavai.cz</a>

Výsledek na webu

<a href="https://hdl.handle.net/11104/0333346" target="_blank" >https://hdl.handle.net/11104/0333346</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-4357/ac77fe" target="_blank" >10.3847/1538-4357/ac77fe</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Dust Grain Growth and Dusty Supernovae in Low-metallicity Molecular Clouds

Popis výsledku v původním jazyce

We present 3D hydrodynamical models of the evolution of superbubbles powered by stellar winds and supernovae from young coeval massive star clusters within low-metallicity (Z = 0.02 Z(circle dot)), clumpy molecular clouds. We explore the initial stages of the superbubble evolution, including the occurrence of pair-instability and core-collapse supernovae. Our aim is to study the occurrence of dust grain growth within orbiting dusty clumps, and in the superbubble's swept-up supershell. We also aim to address the survival of dust grains produced by sequential supernovae. The model accounts for the star cluster gravitational potential and self-gravity of the parent cloud. It also considers radiative cooling (including that induced by dust) and a state-of-the-art population synthesis model for the coeval cluster. As shown before, a superbubble embedded into a clumpy medium becomes highly distorted, expanding mostly due to the hot gas streaming through low-density channels Our results indicate that in the case of massive (similar to 10 M-circle dot) molecular clouds, hosting a super star cluster (similar to 5.6 x 10(5) M-circle dot), grain growth increments the dust mass at a rate similar to 4.8 x 10(-5) M-circle dot yr(-1) during the first 2.5 Myr of the superbubble's evolution, while the net contribution of pair-instability and core-collapse supernovae to the superbubble's dust budget is similar to 1200 M circle dot (M-SC/5.6 x 10(5) M-circle dot), where M-SC is the stellar mass of the starburst. Therefore, dust grain growth and dust injection by supernovae lead to the creation of, without invoking a top-heavy initial mass function, massive amounts of dust within low-metallicity star-forming molecular clouds, in accordance with the large dust mass present in galaxies soon after the onset of cosmic reionization.

Název v anglickém jazyce

Dust Grain Growth and Dusty Supernovae in Low-metallicity Molecular Clouds

Popis výsledku anglicky

We present 3D hydrodynamical models of the evolution of superbubbles powered by stellar winds and supernovae from young coeval massive star clusters within low-metallicity (Z = 0.02 Z(circle dot)), clumpy molecular clouds. We explore the initial stages of the superbubble evolution, including the occurrence of pair-instability and core-collapse supernovae. Our aim is to study the occurrence of dust grain growth within orbiting dusty clumps, and in the superbubble's swept-up supershell. We also aim to address the survival of dust grains produced by sequential supernovae. The model accounts for the star cluster gravitational potential and self-gravity of the parent cloud. It also considers radiative cooling (including that induced by dust) and a state-of-the-art population synthesis model for the coeval cluster. As shown before, a superbubble embedded into a clumpy medium becomes highly distorted, expanding mostly due to the hot gas streaming through low-density channels Our results indicate that in the case of massive (similar to 10 M-circle dot) molecular clouds, hosting a super star cluster (similar to 5.6 x 10(5) M-circle dot), grain growth increments the dust mass at a rate similar to 4.8 x 10(-5) M-circle dot yr(-1) during the first 2.5 Myr of the superbubble's evolution, while the net contribution of pair-instability and core-collapse supernovae to the superbubble's dust budget is similar to 1200 M circle dot (M-SC/5.6 x 10(5) M-circle dot), where M-SC is the stellar mass of the starburst. Therefore, dust grain growth and dust injection by supernovae lead to the creation of, without invoking a top-heavy initial mass function, massive amounts of dust within low-metallicity star-forming molecular clouds, in accordance with the large dust mass present in galaxies soon after the onset of cosmic reionization.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA19-15008S" target="_blank" >GA19-15008S: Efektivita tvorby hvězd v hmotných hvězdokupách</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2022

Kód důvěrnosti údajů

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

Název periodika

Astrophysical Journal

ISSN

0004-637X

e-ISSN

1538-4357

Svazek periodika

934

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

8

Strana od-do

51

Kód UT WoS článku

000829563100001

EID výsledku v databázi Scopus

2-s2.0-85135712108