The Wind Dynamics of Super-Eddington Sources in FRADO

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F22%3A00129254" target="_blank" >RIV/00216224:14310/22:00129254 - isvavai.cz</a>

Výsledek na webu

<a href="https://www.mdpi.com/2673-8716/2/3/15" target="_blank" >https://www.mdpi.com/2673-8716/2/3/15</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3390/dynamics2030015" target="_blank" >10.3390/dynamics2030015</a>

Jazyk výsledku

angličtina

Název v původním jazyce

The Wind Dynamics of Super-Eddington Sources in FRADO

Popis výsledku v původním jazyce

We perform non-hydrodynamical 2.5D simulations to study the dynamics of material above accretion disk based on the disk radiation pressure acting on dust. We assume a super-accreting underlying disk with the accretion rate of 10 times the Eddington rate with central black hole mass ranging from 107 up to 109M⊙. Such high accretion rates are characteristic for extreme sources. We show that for high accretors the radiatively dust-driving mechanism based on the FRADO model always leads to a massive outflow from the disk surface, and the failed wind develops only at larger radii. The outflow rate strongly depends on the black hole mass, and an optically thick energy-driven solution can exceed the accretion rate for masses larger than 108M⊙ but momentum-driven outflow does not exceed the accretion rate even for super-Eddington accretion, therefore not violating the adopted stationarity of the disk. However, even in this case the outflow from the disk implies a strong mechanical feedback.

Název v anglickém jazyce

The Wind Dynamics of Super-Eddington Sources in FRADO

Popis výsledku anglicky

We perform non-hydrodynamical 2.5D simulations to study the dynamics of material above accretion disk based on the disk radiation pressure acting on dust. We assume a super-accreting underlying disk with the accretion rate of 10 times the Eddington rate with central black hole mass ranging from 107 up to 109M⊙. Such high accretion rates are characteristic for extreme sources. We show that for high accretors the radiatively dust-driving mechanism based on the FRADO model always leads to a massive outflow from the disk surface, and the failed wind develops only at larger radii. The outflow rate strongly depends on the black hole mass, and an optically thick energy-driven solution can exceed the accretion rate for masses larger than 108M⊙ but momentum-driven outflow does not exceed the accretion rate even for super-Eddington accretion, therefore not violating the adopted stationarity of the disk. However, even in this case the outflow from the disk implies a strong mechanical feedback.

Druh

J_SC - Článek v periodiku v databázi SCOPUS

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GX21-13491X" target="_blank" >GX21-13491X: Zkoumání žhavého vesmíru a porozumění kosmické zpětné vazbě</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2022

Kód důvěrnosti údajů

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

Název periodika

Dynamics

ISSN

2673-8716

e-ISSN

2673-8716

Svazek periodika

2

Číslo periodika v rámci svazku

3

Stát vydavatele periodika

CH - Švýcarská konfederace

Počet stran výsledku

11

Strana od-do

295-305

Kód UT WoS článku

—

EID výsledku v databázi Scopus

2-s2.0-85144974684