Red giant–jet collisions in galactic nuclei I: 3D hydrodynamical model of a few stellar orbits

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F25%3A00144346" target="_blank" >RIV/00216224:14310/25:00144346 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1093/mnras/staf810" target="_blank" >https://doi.org/10.1093/mnras/staf810</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/staf810" target="_blank" >10.1093/mnras/staf810</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Red giant–jet collisions in galactic nuclei I: 3D hydrodynamical model of a few stellar orbits

Popis výsledku v původním jazyce

Several models have been proposed to explain missing red giants (RGs) near the Galactic centre. Recently, a scenario has been suggested that predicts, among other processes, a long-term ablation of the surface layers of RGs during their repetitive passages through the Galactic jet. In this study, we perform detailed 3D numerical modelling of this phenomenon. We calculate the ablation rate of the surface layers of an RG orbiting the supermassive black hole (SMBH) as it passes through the nuclear jet. In particular, we model the jet-star interaction for approximately 10 passages for the closer orbital distance of 10(-3) pc and 2 passages for 10(-2) pc. We find that the mass loss due to ablation by the jet behaves with time as Delta M-star proportional to root t and the total ablated mass during a single active Galactic nucleus (AGN) phase (10(5) yr) is similar to 10(-4) M-circle dot. We arrive at similar rates of the stellar ablation for the relatively smaller jet luminosity 10(42) erg s(-1) as in the previous analytical calculations. For larger jet luminosities of 10(44) and 10(48) erg s(-1), the ablation rates inferred from similar to 10 interactions as well as extrapolated power-law fits are significantly lower than analytical values. Overall, the mass ablation rate per interaction and the extrapolated cumulative mass loss during the jet activity are comparable to the stellar-wind mass loss. For the smallest orbital distance of 10(-3) pc, we also track the thermal behaviour of the stellar surface layer, whose temperature appears to grow rapidly during the first 10 passages from similar to 3600 K (spectral type M) to similar to 8500 K (spectral type A). RG-jet interactions can thus lead to observable changes in the nuclear stellar population during the jet existence.

Název v anglickém jazyce

Red giant–jet collisions in galactic nuclei I: 3D hydrodynamical model of a few stellar orbits

Popis výsledku anglicky

Several models have been proposed to explain missing red giants (RGs) near the Galactic centre. Recently, a scenario has been suggested that predicts, among other processes, a long-term ablation of the surface layers of RGs during their repetitive passages through the Galactic jet. In this study, we perform detailed 3D numerical modelling of this phenomenon. We calculate the ablation rate of the surface layers of an RG orbiting the supermassive black hole (SMBH) as it passes through the nuclear jet. In particular, we model the jet-star interaction for approximately 10 passages for the closer orbital distance of 10(-3) pc and 2 passages for 10(-2) pc. We find that the mass loss due to ablation by the jet behaves with time as Delta M-star proportional to root t and the total ablated mass during a single active Galactic nucleus (AGN) phase (10(5) yr) is similar to 10(-4) M-circle dot. We arrive at similar rates of the stellar ablation for the relatively smaller jet luminosity 10(42) erg s(-1) as in the previous analytical calculations. For larger jet luminosities of 10(44) and 10(48) erg s(-1), the ablation rates inferred from similar to 10 interactions as well as extrapolated power-law fits are significantly lower than analytical values. Overall, the mass ablation rate per interaction and the extrapolated cumulative mass loss during the jet activity are comparable to the stellar-wind mass loss. For the smallest orbital distance of 10(-3) pc, we also track the thermal behaviour of the stellar surface layer, whose temperature appears to grow rapidly during the first 10 passages from similar to 3600 K (spectral type M) to similar to 8500 K (spectral type A). RG-jet interactions can thus lead to observable changes in the nuclear stellar population during the jet existence.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

Výsledek vznikl pri realizaci vícero projektů. Více informací v záložce Projekty.

Návaznosti

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

Rok uplatnění

2025

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

0035-8711

e-ISSN

1365-2966

Svazek periodika

540

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

22

Strana od-do

1586-1607

Kód UT WoS článku

001499900400001

EID výsledku v databázi Scopus

2-s2.0-105006985607