Red giant–jet collisions in galactic nuclei I: 3D hydrodynamical model of a few stellar orbits
| Autoři | |
|---|---|
| Rok publikování | 2025 |
| Druh | Článek v odborném periodiku |
| Časopis / Zdroj | Monthly Notices of the Royal Astronomical Society |
| Fakulta / Pracoviště MU | |
| Citace | |
| www | https://doi.org/10.1093/mnras/staf810 |
| Doi | http://dx.doi.org/10.1093/mnras/staf810 |
| Klíčová slova | shock waves; stars: late-type; Galaxy: centre; galaxies: jets |
| Přiložené soubory | |
| Popis | 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. |
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